WorldWideScience

Sample records for science instruments observatories

  1. Optical instrumentation for science and formation flying with a starshade observatory

    Science.gov (United States)

    Martin, Stefan; Scharf, Daniel; Cady, Eric; Liebe, Carl; Tang, Hong

    2015-09-01

    In conjunction with a space telescope of modest size, a starshade enables observation of small exoplanets close to the parent star by blocking the direct starlight while the planet light remains unobscured. The starshade is flown some tens of thousands of kilometers ahead of the telescope. Science instruments may include a wide field camera for imaging the target exoplanetary system as well as an integral field spectrometer for characterization of exoplanet atmospheres. We show the preliminary designs of the optical instruments for observatories such as Exo-S, discuss formation flying and control, retargeting maneuvers and other aspects of a starshade mission. The implementation of a starshade-ready WFIRST-AFTA is discussed and we show how a compact, standalone instrument package could be developed as an add-on to future space telescopes, requiring only minor additions to the telescope spacecraft.

  2. EARLY SCIENCE WITH SOFIA, THE STRATOSPHERIC OBSERVATORY FOR INFRARED ASTRONOMY

    Energy Technology Data Exchange (ETDEWEB)

    Young, E. T.; Becklin, E. E.; De Buizer, J. M.; Andersson, B.-G.; Casey, S. C.; Helton, L. A. [SOFIA Science Center, Universities Space Research Association, NASA Ames Research Center, MS 232, Moffett Field, CA 94035 (United States); Marcum, P. M.; Roellig, T. L.; Temi, P. [NASA Ames Research Center, MS 232, Moffett Field, CA 94035 (United States); Herter, T. L. [Astronomy Department, 202 Space Sciences Building, Cornell University, Ithaca, NY 14853-6801 (United States); Guesten, R. [Max-Planck Institut fuer Radioastronomie, Auf dem Huegel 69, Bonn (Germany); Dunham, E. W. [Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff AZ 86001 (United States); Backman, D.; Burgdorf, M. [SOFIA Science Center, NASA Ames Research Center, MS 211-1, Moffett Field, CA 94035 (United States); Caroff, L. J.; Erickson, E. F. [NASA Ames Research Center, Moffett Field, CA 94035 (United States); Davidson, J. A. [School of Physics, The University of Western Australia (M013), 35 Stirling Highway, Crawley WA 6009 (Australia); Gehrz, R. D. [Minnesota Institute for Astrophysics, School of Physics and Astronomy, 116 Church Street, S. E., University of Minnesota, Minneapolis, MN 55455 (United States); Harper, D. A. [Yerkes Observatory, University of Chicago, 373 W. Geneva St., Williams Bay, WI (United States); Harvey, P. M. [Astronomy Department, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712-0259 (United States); and others

    2012-04-20

    The Stratospheric Observatory For Infrared Astronomy (SOFIA) is an airborne observatory consisting of a specially modified Boeing 747SP with a 2.7 m telescope, flying at altitudes as high as 13.7 km (45,000 ft). Designed to observe at wavelengths from 0.3 {mu}m to 1.6 mm, SOFIA operates above 99.8% of the water vapor that obscures much of the infrared and submillimeter. SOFIA has seven science instruments under development, including an occultation photometer, near-, mid-, and far-infrared cameras, infrared spectrometers, and heterodyne receivers. SOFIA, a joint project between NASA and the German Aerospace Center Deutsches Zentrum fuer Luft und-Raumfahrt, began initial science flights in 2010 December, and has conducted 30 science flights in the subsequent year. During this early science period three instruments have flown: the mid-infrared camera FORCAST, the heterodyne spectrometer GREAT, and the occultation photometer HIPO. This Letter provides an overview of the observatory and its early performance.

  3. The Role of Project Science in the Chandra X-Ray Observatory

    Science.gov (United States)

    O'Dell, Stephen L.; Weisskopf, Martin C.

    2006-01-01

    The Chandra X-Ray Observatory, one of NASA's Great Observatories, has an outstanding record of scientific and technical success. This success results from the efforts of a team comprising NASA, its contractors, the Smithsonian Astrophysical Observatory, the instrument groups, and other elements of the scientific community, including thousands of scientists who utilize this powerful facility for astrophysical research. We discuss the role of NASA Project Science in the formulation, development, calibration, and operation of the Chandra X-ray Observatory. In addition to representing the scientific community within the Project, Project Science performed what we term "science systems engineering". This activity encompasses translation of science requirements into technical requirements and assessment of the scientific impact of programmatic and technical trades. We briefly describe several examples of science systems engineering conducted by Chandra Project Science.

  4. Seafloor Observatory Science: a Review

    Directory of Open Access Journals (Sweden)

    L. Beranzoli

    2006-06-01

    Full Text Available The ocean exerts a pervasive influence on Earth’s environment. It is therefore important that we learn how this system operates (NRC, 1998b; 1999. For example, the ocean is an important regulator of climate change (e.g., IPCC, 1995. Understanding the link between natural and anthropogenic climate change and ocean circulation is essential for predicting the magnitude and impact of future changes in Earth’s climate. Understanding the ocean, and the complex physical, biological, chemical, and geological systems operating within it, should be an important goal for the opening decades of the 21st century. Another fundamental reason for increasing our understanding of ocean systems is that the global economy is highly dependent on the ocean (e.g., for tourism, fisheries, hydrocarbons, and mineral resources (Summerhayes, 1996. The establishment of a global network of seafloor observatories will help to provide the means to accomplish this goal. These observatories will have power and communication capabilities and will provide support for spatially distributed sensing systems and mobile platforms. Sensors and instruments will potentially collect data from above the air-sea interface to below the seafloor. Seafloor observatories will also be a powerful complement to satellite measurement systems by providing the ability to collect vertically distributed measurements within the water column for use with the spatial measurements acquired by satellites while also providing the capability to calibrate remotely sensed satellite measurements (NRC, 2000. Ocean observatory science has already had major successes. For example the TAO array has enabled the detection, understanding and prediction of El Niño events (e.g., Fujimoto et al., 2003. This paper is a world-wide review of the new emerging “Seafloor Observatory Science”, and describes both the scientific motivations for seafloor observatories and the technical solutions applied to their architecture. A

  5. Property and instrumental heritage of the Bordeaux Astronomical Observatory; What future?

    Science.gov (United States)

    de La Noë, J.; Charlot, P.; Grousset, F.

    2009-11-01

    In the years 1870, the Government of the Third Republic decided to develop scientific and technical research. Such an effort contributed to supporting and creating universities and other institutes such as astronomical observatories. The dual wish of the Bordeaux council and professors at the Faculté des Sciences de Bordeaux led to the foundation of the astronomical Observatory of Bordeaux. It was set up by Georges Rayet in the years 1880's. The observatory owns a property of 12 hectares with a dozen of buildings, five domes housing an instrument, a Würzburg radiotelescope, a 2.5 meter radiotelescope, and a large collection of about 250 instruments, 4 500 photographic plates, drawings, slides for teaching astronomy, maps of the Carte du Ciel and 200 files of archives. In addition, the library contains about a thousand books for the period 1600-1950. The future of the observatory is not clear at the present time, when the Laboratoire d'Astrophysique will leave to the campus in a few years.

  6. Optical Manufacturing and Testing Requirements Identified by the NASA Science Instruments, Observatories and Sensor Systems Technology Assessment

    Science.gov (United States)

    Stahl, H. Philip; Barney, Rich; Bauman, Jill; Feinberg, Lee; Mcleese, Dan; Singh, Upendra

    2011-01-01

    In August 2010, the NASA Office of Chief Technologist (OCT) commissioned an assessment of 15 different technology areas of importance to the future of NASA. Technology assessment #8 (TA8) was Science Instruments, Observatories and Sensor Systems (SIOSS). SIOSS assess the needs for optical technology ranging from detectors to lasers, x-ray mirrors to microwave antenna, in-situ spectrographs for on-surface planetary sample characterization to large space telescopes. The needs assessment looked across the entirety of NASA and not just the Science Mission Directorate. This paper reviews the optical manufacturing and testing technologies identified by SIOSS which require development in order to enable future NASA high priority missions.

  7. Transformative Science for the Next Decade with the Green Bank Observatory

    Science.gov (United States)

    O'Neil, Karen; Frayer, David; Ghigo, Frank; Lockman, Felix; Lynch, Ryan; Maddalena, Ronald; minter, Anthony; Prestage, Richard

    2018-01-01

    With new instruments and improved performance, the 100m Green Bank Telescope is now demonstrating its full potential. On this 60th anniversary of the groundbreaking for the Green Bank Observatory, we can look forward to the future of the facility for the next 5, 10, and even 20 years. Here we describe the results from a recent workshop, “Transformative Science for the Next Decade with the Green Bank Observatory: Big Questions, Large Programs, and New Instruments,” and describe the scientific plans for our facility.

  8. TELICS—A Telescope Instrument Control System for Small/Medium Sized Astronomical Observatories

    Science.gov (United States)

    Srivastava, Mudit K.; Ramaprakash, A. N.; Burse, Mahesh P.; Chordia, Pravin A.; Chillal, Kalpesh S.; Mestry, Vilas B.; Das, Hillol K.; Kohok, Abhay A.

    2009-10-01

    For any modern astronomical observatory, it is essential to have an efficient interface between the telescope and its back-end instruments. However, for small and medium-sized observatories, this requirement is often limited by tight financial constraints. Therefore a simple yet versatile and low-cost control system is required for such observatories to minimize cost and effort. Here we report the development of a modern, multipurpose instrument control system TELICS (Telescope Instrument Control System) to integrate the controls of various instruments and devices mounted on the telescope. TELICS consists of an embedded hardware unit known as a common control unit (CCU) in combination with Linux-based data acquisition and user interface. The hardware of the CCU is built around the ATmega 128 microcontroller (Atmel Corp.) and is designed with a backplane, master-slave architecture. A Qt-based graphical user interface (GUI) has been developed and the back-end application software is based on C/C++. TELICS provides feedback mechanisms that give the operator good visibility and a quick-look display of the status and modes of instruments as well as data. TELICS has been used for regular science observations since 2008 March on the 2 m, f/10 IUCAA Telescope located at Girawali in Pune, India.

  9. Critical Science Instrument Alignment of the James Webb Space Telescope (JWST) Integrated Science Instrument Module (ISIM)

    Science.gov (United States)

    Rohrbach, Scott O.; Kubalak, David A.; Gracey, Renee M.; Sabatke, Derek S.; Howard, Joseph M.; Telfer, Randal C.; Zielinski, Thomas P.

    2016-01-01

    This paper describes the critical instrument alignment terms associated with the six-degree of freedom alignment of each the Science Instrument (SI) in the James Webb Space Telescope (JWST), including focus, pupil shear, pupil clocking, and boresight. We present the test methods used during cryogenic-vacuum tests to directly measure the performance of each parameter, the requirements levied on each, and the impact of any violations of these requirements at the instrument and Observatory level.

  10. The Science and Design of the AGIS Observatory

    Science.gov (United States)

    Schroedter, Martin

    2010-02-01

    The AGIS observatory is a next-generation array of imaging atmospheric Cherenkov telescopes (IACTs) for gamma-ray astronomy between 100 GeV and 100 TeV. The AGIS observatory is the next logical step in high energy gamma-ray astronomy, offering improved angular resolution and sensitivity compared to FERMI, and overlapping the high energy end of FERMI's sensitivity band. The baseline AGIS observatory will employ an array of 36 Schwarzschild-Couder IACTs in combination with a highly pixelated (0.05^o diameter) camera. The instrument is designed to provide millicrab sensitivity over a wide (8^o diameter) field of view, allowing both deep studies of faint point sources as well as efficient mapping of the Galactic plane and extended sources. I will describe science drivers behind the AGIS observatory and the design and status of the project. )

  11. New developments in instrumentation at the W. M. Keck Observatory

    Science.gov (United States)

    Adkins, Sean M.; Armandroff, Taft E.; Fitzgerald, Michael P.; Johnson, James; Larkin, James E.; Lewis, Hilton A.; Martin, Christopher; Matthews, Keith Y.; Prochaska, J. X.; Wizinowich, Peter

    2014-07-01

    The W. M. Keck Observatory continues to develop new capabilities in support of our science driven strategic plan which emphasizes leadership in key areas of observational astronomy. This leadership is a key component of the scientific productivity of our observing community and depends on our ability to develop new instrumentation, upgrades to existing instrumentation, and upgrades to supporting infrastructure at the observatory. In this paper we describe the as measured performance of projects completed in 2014 and the expected performance of projects currently in the development or construction phases. Projects reaching completion in 2014 include a near-IR tip/tilt sensor for the Keck I adaptive optics system, a new center launch system for the Keck II laser guide star facility, and NIRES, a near-IR Echelle spectrograph for the Keck II telescope. Projects in development include a new seeing limited integral field spectrograph for the visible wavelength range called the Keck Cosmic Web Imager, a deployable tertiary mirror for the Keck I telescope, upgrades to the spectrograph detector and the imager of the OSIRIS instrument, and an upgrade to the telescope control systems on both Keck telescopes.

  12. Enrique Gaviola and the Astronomical Observatory of Cordoba. Its impact in the Argentine science development

    International Nuclear Information System (INIS)

    Bernaola, Omar A.

    2001-01-01

    The history of the Astronomical Observatory of Cordoba (Argentina), opened in 1871, is related. The physicist Enrique Gaviola (1900-1989) has been the director of the Observatory from 1940 to 1945 and again from 1956 to 1957. He was instrumental in the construction of the Observatory's big telescope (inaugurated in 1942, diameter 152 cm). The influence that E. Gaviola exerted upon the development of physics in Argentina, including the nuclear sciences, is also related

  13. New seismic instrumentation packaged for all terrestrial environments (including the quietest observatories!).

    Science.gov (United States)

    Parker, Tim; Devanney, Peter; Bainbridge, Geoff; Townsend, Bruce

    2017-04-01

    The march to make every type of seismometer, weak to strong motion, reliable and economically deployable in any terrestrial environment continues with the availability of three new sensors and seismic systems including ones with over 200dB of dynamic range. Until recently there were probably 100 pier type broadband sensors for every observatory type pier, not the types of deployments geoscientists are needing to advance science and monitoring capability. Deeper boreholes are now the recognized quieter environments for best observatory class instruments and these same instruments can now be deployed in direct burial environments which is unprecedented. The experiences of facilities in large deployments of broadband seismometers in continental scale rolling arrays proves the utility of packaging new sensors in corrosion resistant casings and designing in the robustness needed to work reliably in temporary deployments. Integrating digitizers and other sensors decreases deployment complexity, decreases acquisition and deployment costs, increases reliability and utility. We'll discuss the informed evolution of broadband pier instruments into the modern integrated field tools that enable economic densification of monitoring arrays along with supporting new ways to approach geoscience research in a field environment.

  14. The Architectural and Instrumental Heritage of the Strasbourg University Observatory

    Science.gov (United States)

    Davoigneau, Jean

    When, in 1872, Alsace was handed over to Germany, Empperor Wilhelm I decided to make Strasbourg the showcase of his empire, and in particular to build a prestigious university and an observatory. The construction of the observatory was entrusted to the astronomer August Winnecke (1835-1897), former director of the Pulkovo observatory, and to the Baumeister Hermann Eggert. Begun in 1876, the work was completed in 1880. The astronomical instruments, ordered from German makers, were installed during the winter of 1880-1881, and the observatory was inaugurated on September 22, 1881 at the general assembly of the Astronomische Gesellschaft, the international association of astronomers, whose secretary was Winnecke. Marking the south-eastern extremity of the ‘imperial axis’, the architecture of the university observatory harmonizes perfectly with the new German city built on the former French parade grounds. The astronomical heritage operation conducted at the beginning of the present decade provides a richly docurnented and illustrated inventory of both the architecture and instruments of this institution. This work has also highlighted the unique quality of the collection of instruments, befitting the long and complex history of this institution.

  15. Creation of an instrument maintenance program at W. M. Keck Observatory

    Science.gov (United States)

    Hill, G. M.; Kwok, S. H.; Mader, J. A.; Wirth, G. D.; Dahm, S. E.; Goodrich, R. W.

    2014-08-01

    Until a few years ago, the W. M. Keck Observatory (WMKO) did not have a systematic program of instrument maintenance at a level appropriate for a world-leading observatory. We describe the creation of such a program within the context of WMKO's lean operations model which posed challenges but also guided the design of the system and resulted in some unique and notable capabilities. These capabilities and the flexibility of the system have led to its adoption across the Observatory for virtually all PM's. The success of the Observatory in implementing the program and its impact on instrument reliability are presented. Lessons learned are reviewed and strategic implications discussed.

  16. Using Citizen Science to Close Gaps in Cabled Ocean Observatory Research

    Science.gov (United States)

    Morley, M. G.; Moran, K.; Riddell, D. J.; Hoeberechts, M.; Flagg, R.; Walsh, J.; Dobell, R.; Longo, J.

    2015-12-01

    Ocean Networks Canada operates the world-leading NEPTUNE and VENUS cabled ocean observatories off the west coast of British Columbia, and a community observatory in Cambridge Bay, Nunavut. Continuous power and connectivity permit large volumes of data to be collected and made available to scientists and citizens alike over the Internet through a web-based interface. The Oceans 2.0 data management system contains over one quarter petabyte of data, including more than 20,000 hours of video from fixed seafloor cameras and a further 8,000 hours of video collected by remotely operated vehicles. Cabled observatory instrument deployments enable the collection of high-frequency, long-duration time series of data from a specific location. This enables the study of important questions such as whether effects of climate change—for instance, variations in temperature or sea-level—are seen over the long term. However, cabled observatory monitoring also presents challenges to scientific researchers: the overwhelming volume of data and the fixed spatial location can be barriers to addressing some big questions. Here we describe how Ocean Networks Canada is using Citizen Science to address these limitations and supplement cabled observatory research. Two applications are presented: Digital Fishers is a crowd-sourcing application in which participants watch short deep-sea video clips and make annotations based on scientific research questions. To date, 3,000 participants have contributed 140,000 scientific observations on topics including sablefish abundance, hydrothermal vent geology and deep-sea feeding behaviour. Community Fishers is a program in which ordinary citizens aboard vessels of opportunity collect ocean data including water temperature, salinity, dissolved oxygen and chlorophyll. The program's focus is to directly address the typical quality concerns around data that are collected using a citizen science approach. This is done by providing high quality scientific

  17. The Development of the Classical Observatory: From a Functional Shelter for the Telescope to the Temple of Science

    Directory of Open Access Journals (Sweden)

    Tapio Markkanen

    2013-11-01

    Full Text Available At the end of the 18th century and at the beginning of the 19th century, observatory buildings underwent a change, because astronomical tools of observation had transformed from light portable equipment into permanently mounted accurate instruments. For positional astronomy, observations were mainly carried out in the meridian or in the prime vertical. A new type of telescope, the equatorially mounted refractor was adopted for the observation of objects such as planets, comets and double stars. The new instruments and methods of observation also required new approaches to observatory design. The new research needs began to determine the exterior, structure and functions of the observatory building. At the beginning of the 19th century, new standards of observatory planning were developed for the construction of the new observatories of Tartu, Helsinki and Pulkovo. Over many decades, the adopted design principles guided the construction and architecture of avant-garde observatories around the world. They also provided for the archetype of the observatory as a universal emblem for science well into the 20th century. The article discusses the development stages of these design principles and their global impacts.

  18. Science requirements and the design of cabled ocean observatories

    Directory of Open Access Journals (Sweden)

    H. Mikada

    2006-06-01

    Full Text Available The ocean sciences are beginning a new phase in which scientists will enter the ocean environment and adaptively observe the Earth-Ocean system through remote control of sensors and sensor platforms. This new ocean science paradigm will be implemented using innovative facilities called ocean observatories which provide unprecedented levels of power and communication to access and manipulate real-time sensor networks deployed within many different environments in the ocean basins. Most of the principal design drivers for ocean observatories differ from those for commercial submarine telecommunications systems. First, ocean observatories require data to be input and output at one or more seafloor nodes rather than at a few land terminuses. Second, ocean observatories must distribute a lot of power to the seafloor at variable and fluctuating rates. Third, the seafloor infrastructure for an ocean observatory inherently requires that the wet plant be expandable and reconfigurable. Finally, because the wet communications and power infrastructure is comparatively complex, ocean observatory infrastructure must be designed for low life cycle cost rather than zero maintenance. The origin of these differences may be understood by taking a systems engineering approach to ocean observatory design through examining the requirements derived from science and then going through the process of iterative refinement to yield conceptual and physical designs. This is illustrated using the NEPTUNE regional cabled observatory power and data communications sub-systems.

  19. Designing Observatories for the Hydrologic Sciences

    Science.gov (United States)

    Hooper, R. P.

    2004-05-01

    The need for longer-term, multi-scale, coherent, and multi-disciplinary data to test hypotheses in hydrologic science has been recognized by numerous prestigious review panels over the past decade (e.g. NRC's Basic Research Opportunities in Earth Science). Designing such observatories has proven to be a challenge not only on scientific, but also technological, economic and even sociologic levels. The Consortium of Universities for the Advancement of Hydrologic Science, Inc. (CUAHSI) has undertaken a "paper" prototype design of a hydrologic observatory (HO) for the Neuse River Basin, NC and plans to solicit proposals and award grants to develop implementation plans for approximately 10 basins (which may be defined by topographic or groundwater divides) during the summer of 2004. These observatories are envisioned to be community resources with data available to all scientists, with support facilities to permit their use by both local and remote investigators. This paper presents the broad design concepts which were developed from a national team of scientists for the Neuse River Basin Prototype. There are three fundamental characteristics of a watershed or river basin that are critical for answering the major scientific questions proposed by the NRC to advance hydrologic, biogeochemical and ecological sciences: (1) the store and flux of water, sediment, nutrients and contaminants across interfaces at multiple scales must be identified; (2) the residence time of these constituents, and (3) their flowpaths and response spectra to forcing must be estimated. "Stores" consist of subsurface, land surface and atmospheric volumes partitioned over the watershed. The HO will require "core measurements" which will serve the communities of hydrologic science for long range research questions. The core measurements will also provide context for shorter-term or hypothesis-driven research investigations. The HO will support "mobile measurement facilities" designed to support teams

  20. Advanced Technologies and Instrumentation at the National Science Foundation

    Science.gov (United States)

    Kurczynski, Peter; Neff, James E.

    2018-01-01

    Over its more than thirty-year history, the Advanced Technologies and Instrumentation (ATI) program within the Division of Astronomical Sciences has provided grants to support the development and deployment of detectors and instrumentation for ground-based astronomy. This program has enabled scientific advances in diverse fields from solar physics to exoplanets to cosmology. ATI has provided instrumentation for both small and large observatories from radio through visible wavebands. It has played a role in the early development of major initiatives such as the Large Synoptic Survey Telescope. Technology development for astronomy unfolds over a longer period than the lifetime of a single grant. This review will consider ATI from an historical perspective to assess its impact on astronomy.

  1. The Lowell Observatory Predoctoral Fellowship Program

    Science.gov (United States)

    Prato, Lisa A.; Shkolnik, E.

    2014-01-01

    Lowell Observatory is pleased to solicit applications for our Predoctoral Fellowship Program. Now beginning its seventh year, this program is designed to provide unique research opportunities to graduate students in good standing, currently enrolled at Ph.D. granting institutions. Lowell staff research spans a wide range of topics, from astronomical instrumentation, to icy bodies in our solar system, exoplanet science, stellar populations, star formation, and dwarf galaxies. The Observatory's new 4.3 meter Discovery Channel Telescope has successfully begun science operations and we anticipate the commissioning of several new instruments in 2014, making this a particularly exciting time to do research at Lowell. Student research is expected to lead to a thesis dissertation appropriate for graduation at the doctoral level at the student's home institution. The Observatory provides competitive compensation and full benefits to student scholars. For more information, see http://www2.lowell.edu/rsch/predoc.php and links therein. Applications for Fall 2014 are due by May 1, 2014.

  2. Compton Gamma-Ray Observatory

    Science.gov (United States)

    1991-01-01

    This photograph shows the Compton Gamma-Ray Observatory (GRO) being deployed by the Remote Manipulator System (RMS) arm aboard the Space Shuttle Atlantis during the STS-37 mission in April 1991. The GRO reentered Earth atmosphere and ended its successful mission in June 2000. For nearly 9 years, the GRO Burst and Transient Source Experiment (BATSE), designed and built by the Marshall Space Flight Center (MSFC), kept an unblinking watch on the universe to alert scientists to the invisible, mysterious gamma-ray bursts that had puzzled them for decades. By studying gamma-rays from objects like black holes, pulsars, quasars, neutron stars, and other exotic objects, scientists could discover clues to the birth, evolution, and death of stars, galaxies, and the universe. The gamma-ray instrument was one of four major science instruments aboard the Compton. It consisted of eight detectors, or modules, located at each corner of the rectangular satellite to simultaneously scan the entire universe for bursts of gamma-rays ranging in duration from fractions of a second to minutes. In January 1999, the instrument, via the Internet, cued a computer-controlled telescope at Las Alamos National Laboratory in Los Alamos, New Mexico, within 20 seconds of registering a burst. With this capability, the gamma-ray experiment came to serve as a gamma-ray burst alert for the Hubble Space Telescope, the Chandra X-Ray Observatory, and major gound-based observatories around the world. Thirty-seven universities, observatories, and NASA centers in 19 states, and 11 more institutions in Europe and Russia, participated in the BATSE science program.

  3. Science Potential of a Deep Ocean Antineutrino Observatory

    International Nuclear Information System (INIS)

    Dye, S.T.

    2007-01-01

    This paper presents science potential of a deep ocean antineutrino observatory being developed at Hawaii. The observatory design allows for relocation from one site to another. Positioning the observatory some 60 km distant from a nuclear reactor complex enables precision measurement of neutrino mixing parameters, leading to a determination of neutrino mass hierarchy and θ 13 . At a mid-Pacific location the observatory measures the flux and ratio of uranium and thorium decay neutrinos from earth's mantle and performs a sensitive search for a hypothetical natural fission reactor in earth's core. A subsequent deployment at another mid-ocean location would test lateral heterogeneity of uranium and thorium in earth's mantle

  4. Aryabhatta Research Institute of Observational Sciences: reincarnation of a 50 year old State Observatory of Nainital

    Science.gov (United States)

    Sagar, Ram

    2006-03-01

    The fifty year old State Observatory, well known as U.P. State Observatory till the formation of Uttaranchal in November 2000, was reincarnated on March 22, 2004 as Aryabhatta Research Institute of Observational Sciences with acronym ARIES, an autonomous institute, under the Department of Science & Technology, Government of India. The growth of academic and technical activities and new mandate of the Institute are briefly described. In early 60's, the Institute was one of the 12 centres established by the Smithsonian Astrophysical Observatory, USA, all over the globe but the only centre in India for imaging artificial earth satellites. Commensurating with its observing capabilities, the Institute started a number of front-line research programmes during the last decade, e.g., optical follow up observations of GRB afterglows, radio and space borne astronomical resources, intra-night optical variability in active galactic nuclei as well as gravitational microlensing and milli-magnitude variations in the rapidly oscillating peculiar A type stars. As a part of atmospheric studies, characterisation of aerosol at an altitude of about 2 km is going on since 2002. ARIES has plans for establishing modern observing facilities equipped with latest backend instruments in the area of both astrophysics and atmospheric science. Formation of ARIES, therefore augurs well for the overall development of astrophysics and atmospheric science in India.

  5. Science Potential of a Deep Ocean Antineutrino Observatory

    Energy Technology Data Exchange (ETDEWEB)

    Dye, S.T. [Department of Physics and Astronomy, University of Hawaii, 2505 Correa Road, Honolulu, Hawaii, 96822 (United States); College of Natural Sciences, Hawaii Pacific University, 45-045 Kamehameha Highway, Kaneohe, Hawaii 96744 (United States)

    2007-06-15

    This paper presents science potential of a deep ocean antineutrino observatory being developed at Hawaii. The observatory design allows for relocation from one site to another. Positioning the observatory some 60 km distant from a nuclear reactor complex enables precision measurement of neutrino mixing parameters, leading to a determination of neutrino mass hierarchy and {theta}{sub 13}. At a mid-Pacific location the observatory measures the flux and ratio of uranium and thorium decay neutrinos from earth's mantle and performs a sensitive search for a hypothetical natural fission reactor in earth's core. A subsequent deployment at another mid-ocean location would test lateral heterogeneity of uranium and thorium in earth's mantle.

  6. Citizen Observatories and the New Earth Observation Science

    Directory of Open Access Journals (Sweden)

    Alan Grainger

    2017-02-01

    Full Text Available Earth observation is diversifying, and now includes new types of systems, such as citizen observatories, unmanned aerial vehicles and wireless sensor networks. However, the Copernicus Programme vision of a seamless chain from satellite data to usable information in the hands of decision makers is still largely unrealized, and remote sensing science lacks a conceptual framework to explain why. This paper reviews the literatures on citizen science, citizen observatories and conceptualization of remote sensing systems. It then proposes a Conceptual Framework for Earth Observation which can be used in a new Earth observation science to explain blockages in the chain from collecting data to disseminating information in any Earth observation system, including remote sensing systems. The framework differs from its predecessors by including social variables as well as technological and natural ones. It is used here, with evidence from successful citizen science projects, to compare the factors that are likely to influence the effectiveness of satellite remote sensing systems and citizen observatories. The paper finds that constraints on achieving the seamless “Copernicus Chain” are not solely technical, as assumed in the new Space Strategy for Europe, but include social constraints too. Achieving the Copernicus Chain will depend on the balance between: (a the ‘forward’ momentum generated by the repetitive functioning of each component in the system, as a result of automatic operation or human institutions, and by the efficiency of interfaces between components; and (b the ‘backward’ flow of information on the information needs of end users. Citizen observatories will face challenges in components which for satellite remote sensing systems are: (a automatic or straightforward, e.g., sensor design and launch, data collection, and data products; and (b also challenging, e.g., data processing. Since citizen observatories will rely even more on

  7. New Life for Astronomical Instruments of the Past at the Astronomical Observatory of Taras Shevchenko

    Science.gov (United States)

    Kazantseva, Liliya

    2012-09-01

    Astronomical instruments of the past are certainly valuable artifacts of the history of science and education. Like other collections of scientific equipment, they also demonstrate i) development of scientific and technical ideas, ii) technological features of the historical period, iii) professional features of artists or companies -- manufacturers, and iv) national and local specificity of production. However, astronomical instruments are also devices made for observations of rare phenomena -- solar eclipses, transits of planets of the solar disk, etc. Instruments used to study these rare events were very different for each event, since the science changed quickly between events. The Astronomical Observatory of Kyiv National Taras Shevchenko University has a collection of tools made by leading European and local shops from the early nineteenth century. These include tools for optically observing the first artificial Earth satellites, photography, chronometry, and meteorology. In addition, it has assembled a library of descriptions of astronomical instruments and makers'price-lists. Of particular interest are the large stationary tools that are still active in their pavilions. Almost every instrument has a long interesting history. Museification of astronomical instruments gives them a second life, expanding educational programs and tracing the development of astronomy in general and scientific institution and region in particular. It would be advisable to first create a regional database of these rare astronomical instruments (which is already being done in Ukraine), then a common global database. By combining all the historical information about astronomical instruments with the advantages of the Internet, you can show the full evolution of an astronomical instrument with all its features. Time is relentless, and much is destroyed, badly kept and thrown in the garbage. We need time to protect, capture, and tell about it.

  8. Astronomy and astrophysics communication in the UCM Observatory

    Science.gov (United States)

    Crespo-Chacón, I.; de Castro, E.; Díaz, C.; Gallego, J.; Gálvez, M. C.; Hernán-Obispo, M.; López-Santiago, J.; Montes, D.; Pascual, S.; Verdet, A.; Villar, V.; Zamorano, J.

    We present a summary of the last activities of science communication that have taken place in the Observatorio de la Universidad Complutense de Madrid (UCM Observatory) on the occasion of the Third Science Week of the Comunidad Autónoma de Madrid (3-16 November 2003), including guided tours through the observatory facilities, solar observations, and several talks. Moreover the current telescopes, instruments and tools of the UCM Observatory have allowed us to organize other communicating activities such as the live observation, together with its internet broadcast, of total lunar eclipses and other exceptional astronomical events as the Venus transit that took place in 8 June 2004.

  9. Using the Critical Zone Observatory Network to Put Geology into Environmental Science

    Science.gov (United States)

    Brantley, S. L.

    2017-12-01

    The use of observatories to study the environment in the U.S.A. arguably began in 1910. Since then, many environmental observatories were set up to study impacts of land use change. At that time, observatories did not emphasize geological structure. Around 2004, scientists in the U.S.A. began to emphasize the need to study the Earth's surface as one integrated system that includes the geological underpinnings. In 2007, the Geosciences Directorate within the U.S. National Science Foundation established the Critical Zone Observatory (CZO) program. Today the CZO network has grown to 9 observatories, and 45 countries now host such observatories. A CZO is an observatory that promotes the study of the entire layer of Earth's surface from vegetation canopy to groundwater as one entity. The observatories are somewhat similar to other NSF-funded observatories such as Long Term Ecological Research (LTER) sites but they differ in that they emphasize the history of the landscape and how it mediates today's fluxes. LTERs largely focus on ecological science. The concepts of CZ science and CZOs - developed by the Geosciences Directorate - have been extraordinarily impactful: we now have deeper understanding of how surficial processes respond to tectonic, climatic, and anthropogenic drivers. One reason CZOs succeed is that they host scientists who make measurements in one place that cross timescales from that of the meteorologist to the geologist. The NSF Geosciences Directorate has thus promoted insights showing that many of the unexplained mysteries of "catchment science" or "ecosystem science" can be explained by the underlying geological story of a site. The scientific challenges of this endeavor are dwarfed, however, by cultural challenges. Specifically, while both CZOs and observatories such as LTERs struggle to publish many types of data from different disciplines in a continually changing cyber-world, only CZO scientists find they must repeatedly explain why such

  10. The Earth System Science Pathfinder Orbiting Carbon Observatory (OCO) Mission

    Science.gov (United States)

    Crisp, David

    2003-01-01

    A viewgraph presentation describing the Earth System Science Pathfinder Orbiting Carbon Observatory (OCO) Mission is shown. The contents include: 1) Why CO2?; 2) What Processes Control CO2 Sinks?; 3) OCO Science Team; 4) Space-Based Measurements of CO2; 5) Driving Requirement: Precise, Bias-Free Global Measurements; 6) Making Precise CO2 Measurements from Space; 7) OCO Spatial Sampling Strategy; 8) OCO Observing Modes; 9) Implementation Approach; 10) The OCO Instrument; 11) The OCO Spacecraft; 12) OCO Will Fly in the A-Train; 13) Validation Program Ensures Accuracy and Minimizes Spatially Coherent Biases; 14) Can OCO Provide the Required Precision?; 15) O2 Column Retrievals with Ground-based FTS; 16) X(sub CO2) Retrieval Simulations; 17) Impact of Albedo and Aerosol Uncertainty on X(sub CO2) Retrievals; 18) Carbon Cycle Modeling Studies: Seasonal Cycle; 19) Carbon Cycle Modeling Studies: The North-South Gradient in CO2; 20) Carbon Cycle Modeling Studies: Effect of Diurnal Biases; 21) Project Status and Schedule; and 22) Summary.

  11. 40+ Years of Instrumentation for the La Silla Paranal Observatory

    Science.gov (United States)

    D'Odorico, S.

    2018-03-01

    As ESO Period 100 comes to a close, I look back at the development of ESO's instrumentation programme over more than 40 years. Instrumentation and detector activities were initially started by a small group of designers, engineers, technicians and astronomers while ESO was still at CERN in Geneva in the late 1970s. They have since led to the development of a successful suite of optical and infrared instruments for the La Silla Paranal Observatory, as testified by the continuous growth in the number of proposals for observing time and in the publications based on data from ESO telescopes. The instrumentation programme evolved significantly with the VLT and most instruments were developed by national institutes in close cooperation with ESO. This policy was a cornerstone of the VLT programme from the beginning and a key to its success.

  12. Large-Scale Science Observatories: Building on What We Have Learned from USArray

    Science.gov (United States)

    Woodward, R.; Busby, R.; Detrick, R. S.; Frassetto, A.

    2015-12-01

    With the NSF-sponsored EarthScope USArray observatory, the Earth science community has built the operational capability and experience to tackle scientific challenges at the largest scales, such as a Subduction Zone Observatory. In the first ten years of USArray, geophysical instruments were deployed across roughly 2% of the Earth's surface. The USArray operated a rolling deployment of seismic stations that occupied ~1,700 sites across the USA, made co-located atmospheric observations, occupied hundreds of sites with magnetotelluric sensors, expanded a backbone reference network of seismic stations, and provided instruments to PI-led teams that deployed thousands of additional seismic stations. USArray included a comprehensive outreach component that directly engaged hundreds of students at over 50 colleges and universities to locate station sites and provided Earth science exposure to roughly 1,000 landowners who hosted stations. The project also included a comprehensive data management capability that received, archived and distributed data, metadata, and data products; data were acquired and distributed in real time. The USArray project was completed on time and under budget and developed a number of best practices that can inform other large-scale science initiatives that the Earth science community is contemplating. Key strategies employed by USArray included: using a survey, rather than hypothesis-driven, mode of observation to generate comprehensive, high quality data on a large-scale for exploration and discovery; making data freely and openly available to any investigator from the very onset of the project; and using proven, commercial, off-the-shelf systems to ensure a fast start and avoid delays due to over-reliance on unproven technology or concepts. Scope was set ambitiously, but managed carefully to avoid overextending. Configuration was controlled to ensure efficient operations while providing consistent, uniform observations. Finally, community

  13. The Operation and Architecture of the Keck Observatory Archive

    Science.gov (United States)

    Berriman, G. B.; Gelino, C. R.; Laity, A.; Kong, M.; Swain, M.; Holt, J.; Goodrich, R.; Mader, J.; Tran, H. D.

    2014-05-01

    The Infrared Processing and Analysis Center (IPAC) and the W. M. Keck Observatory (WMKO) are collaborating to build an archive for the twin 10-m Keck Telescopes, located near the summit of Mauna Kea. The Keck Observatory Archive (KOA) takes advantage of IPAC's long experience with managing and archiving large and complex data sets from active missions and serving them to the community; and of the Observatory's knowledge of the operation of its sophisticated instrumentation and the organization of the data products. By the end of 2013, KOA will contain data from all eight active observatory instruments, with an anticipated volume of 28 TB. The data include raw science and observations, quick look products, weather information, and, for some instruments, reduced and calibrated products. The goal of including data from all instruments is the cumulation of a rapid expansion of the archive's holdings, and already data from four new instruments have been added since October 2012. One more active instrument, the integral field spectrograph OSIRIS, is scheduled for ingestion in December 2013. After preparation for ingestion into the archive, the data are transmitted electronically from WMKO to IPAC for curation in the physical archive. This process includes validation of the science and content of the data and verification that data were not corrupted in transmission. The archived data include both newly-acquired observations and all previously acquired observations. The older data extends back to the date of instrument commissioning; for some instruments, such as HIRES, these data can extend as far back as 1994. KOA will continue to ingest all newly obtained observations, at an anticipated volume of 4 TB per year, and plans to ingest data from two decommissioned instruments. Access to these data is governed by a data use policy that guarantees Principal Investigators (PI) exclusive access to their data for at least 18 months, and allows for extensions as granted by

  14. James Gregory, the University observatory and the early acquisition of scientific instruments at the University of St Andrews

    Science.gov (United States)

    Rawson, Helen C.

    2015-01-01

    James Gregory, inventor of the reflecting telescope and Fellow of the Royal Society, was the first Regius Professor of Mathematics of the University of St Andrews, 1668–74. He attempted to establish in St Andrews what would, if completed, have been the first purpose-built observatory in the British Isles. He travelled to London in 1673 to purchase instruments for equipping the observatory and improving the teaching and study of natural philosophy and mathematics in the university, seeking the advice of John Flamsteed, later the first Astronomer Royal. This paper considers the observatory initiative and the early acquisition of instruments at the University of St Andrews, with reference to Gregory's correspondence, inventories made ca. 1699–ca. 1718 and extant instruments themselves, some of which predate Gregory's time. It examines the structure and fate of the university observatory, the legacy of Gregory's teaching and endeavours, and the meridian line laid down in 1748 in the University Library.

  15. The OCO-3 Mission: Science Objectives and Instrument Performance

    Science.gov (United States)

    Eldering, A.; Basilio, R. R.; Bennett, M. W.

    2017-12-01

    The Orbiting Carbon Observatory 3 (OCO-3) will continue global CO2 and solar-induced chlorophyll fluorescence (SIF) using the flight spare instrument from OCO-2. The instrument is currently being tested, and will be packaged for installation on the International Space Station (ISS) (launch readiness in early 2018.) This talk will focus on the science objectives, updated simulations of the science data products, and the outcome of recent instrument performance tests. The low-inclination ISS orbit lets OCO-3 sample the tropics and sub-tropics across the full range of daylight hours with dense observations at northern and southern mid-latitudes (+/- 52º). The combination of these dense CO2 and SIF measurements provides continuity of data for global flux estimates as well as a unique opportunity to address key deficiencies in our understanding of the global carbon cycle. The instrument utilizes an agile, 2-axis pointing mechanism (PMA), providing the capability to look towards the bright reflection from the ocean and validation targets. The PMA also allows for a snapshot mapping mode to collect dense datasets over 100km by 100km areas. Measurements over urban centers could aid in making estimates of fossil fuel CO2 emissions. Similarly, the snapshot mapping mode can be used to sample regions of interest for the terrestrial carbon cycle. In addition, there is potential to utilize data from ISS instruments ECOSTRESS (ECOsystem Spaceborne Thermal Radiometer Experiment on Space Station) and GEDI (Global Ecosystem Dynamics Investigation), which measure other key variables of the control of carbon uptake by plants, to complement OCO-3 data in science analysis. In 2017, the OCO-2 instrument was transformed into the ISS-ready OCO-3 payload. The transformed instrument was thoroughly tested and characterized. Key characteristics, such as instrument ILS, spectral resolution, and radiometric performance will be described. Analysis of direct sun measurements taken during testing

  16. Making Kew Observatory: the Royal Society, the British Association and the politics of early Victorian science.

    Science.gov (United States)

    Macdonald, Lee T

    2015-09-01

    Built in 1769 as a private observatory for King George III, Kew Observatory was taken over in 1842 by the British Association for the Advancement of Science (BAAS). It was then quickly transformed into what some claimed to be a 'physical observatory' of the sort proposed by John Herschel - an observatory that gathered data in a wide range of physical sciences, including geomagnetism and meteorology, rather than just astronomy. Yet this article argues that the institution which emerged in the 1840s was different in many ways from that envisaged by Herschel. It uses a chronological framework to show how, at every stage, the geophysicist and Royal Artillery officer Edward Sabine manipulated the project towards his own agenda: an independent observatory through which he could control the geomagnetic and meteorological research, including the ongoing 'Magnetic Crusade'. The political machinations surrounding Kew Observatory, within the Royal Society and the BAAS, may help to illuminate the complex politics of science in early Victorian Britain, particularly the role of 'scientific servicemen' such as Sabine. Both the diversity of activities at Kew and the complexity of the observatory's origins make its study important in the context of the growing field of the 'observatory sciences'.

  17. NASA X-Ray Observatory Completes Tests Under Harsh Simulated Space Conditions

    Science.gov (United States)

    1998-07-01

    NASA's most powerful X-ray observatory has successfully completed a month-long series of tests in the extreme heat, cold, and airless conditions it will encounter in space during its five-year mission to shed new light on some of the darkest mysteries of the universe. The Advanced X-ray Astrophysics Facility was put through the rigorous testing as it was alternately heated and cooled in a special vacuum chamber at TRW Space and Electronics Group in Redondo Beach, Calif., NASA's prime contractor for the observatory. "Successful completion of thermal vacuum testing marks a significant step in readying the observatory for launch aboard the Space Shuttle in January," said Fred Wojtalik, manager of the Observatory Projects Office at NASA's Marshall Space Flight Center in Huntsville, Ala. "The observatory is a complex, highly sophisticated, precision instrument," explained Wojtalik. "We are pleased with the outcome of the testing, and are very proud of the tremendous team of NASA and contractor technicians, engineers and scientists that came together and worked hard to meet this challenging task." Testing began in May after the observatory was raised into the 60-foot thermal vacuum chamber at TRW. Testing was completed on June 20. During the tests the Advanced X-ray Astrophysics Facility was exposed to 232 degree heat and 195 degree below zero Fahrenheit cold. During four temperature cycles, all elements of the observatory - the spacecraft, telescope, and science instruments - were checked out. Computer commands directing the observatory to perform certain functions were sent from test consoles at TRW to all Advanced X-ray Astrophysics Facility components. A team of contractor and NASA engineers and scientists monitored and evaluated the results. Commands were also sent from, and test data monitored at, the Advanced X-ray Astrophysics Facility Operations Control Center in Cambridge, Mass., as part of the test series. The observatory will be managed and controlled from

  18. SOFIA science instruments: commissioning, upgrades and future opportunities

    Science.gov (United States)

    Smith, Erin C.; Miles, John W.; Helton, L. Andrew; Sankrit, Ravi; Andersson, B. G.; Becklin, Eric E.; De Buizer, James M.; Dowell, C. D.; Dunham, Edward W.; Güsten, Rolf; Harper, Doyal A.; Herter, Terry L.; Keller, Luke D.; Klein, Randolf; Krabbe, Alfred; Logsdon, Sarah; Marcum, Pamela M.; McLean, Ian S.; Reach, William T.; Richter, Matthew J.; Roellig, Thomas L.; Sandell, Göran; Savage, Maureen L.; Temi, Pasquale; Vacca, William D.; Vaillancourt, John E.; Van Cleve, Jeffrey E.; Young, Erick T.

    2014-07-01

    The Stratospheric Observatory for Infrared Astronomy (SOFIA) is the world's largest airborne observatory, featuring a 2.5 meter effective aperture telescope housed in the aft section of a Boeing 747SP aircraft. SOFIA's current instrument suite includes: FORCAST (Faint Object InfraRed CAmera for the SOFIA Telescope), a 5-40 μm dual band imager/grism spectrometer developed at Cornell University; HIPO (High-speed Imaging Photometer for Occultations), a 0.3-1.1μm imager built by Lowell Observatory; GREAT (German Receiver for Astronomy at Terahertz Frequencies), a multichannel heterodyne spectrometer from 60-240 μm, developed by a consortium led by the Max Planck Institute for Radio Astronomy; FLITECAM (First Light Infrared Test Experiment CAMera), a 1-5 μm wide-field imager/grism spectrometer developed at UCLA; FIFI-LS (Far-Infrared Field-Imaging Line Spectrometer), a 42-200 μm IFU grating spectrograph completed by University Stuttgart; and EXES (Echelon-Cross-Echelle Spectrograph), a 5-28 μm highresolution spectrometer designed at the University of Texas and being completed by UC Davis and NASA Ames Research Center. HAWC+ (High-resolution Airborne Wideband Camera) is a 50-240 μm imager that was originally developed at the University of Chicago as a first-generation instrument (HAWC), and is being upgraded at JPL to add polarimetry and new detectors developed at Goddard Space Flight Center (GSFC). SOFIA will continually update its instrument suite with new instrumentation, technology demonstration experiments and upgrades to the existing instrument suite. This paper details the current instrument capabilities and status, as well as the plans for future instrumentation.

  19. VESPA: A community-driven Virtual Observatory in Planetary Science

    Czech Academy of Sciences Publication Activity Database

    Erard, S.; Cecconi, B.; Le Sidaner, P.; Rossi, A. P.; Capria, M.T.; Schmitt, B.; Génot, V.; André, N.; Vandaele, A. C.; Scherf, M.; Hueso, R.; Määttänen, A.; Thuillot, W.; Carry, B.; Achilleos, N.; Marmo, C.; Santolík, Ondřej; Benson, K.; Fernique, P.; Beigbeder, L.; Millour, E.; Rousseau, B.; Andrieu, F.; Chauvin, C.; Minin, M.; Ivanoski, S.; Longobardo, A.; Bollard, P.; Albert, D.; Gangloff, M.; Jourdane, N.; Bouchemit, M.; Glorian, J. M.; Trompet, L.; Al-Ubaidi, T.; Juaristi, J.; Desmars, J.; Guio, P.; Delaa, O.; Lagain, A.; Souček, Jan; Píša, David

    2018-01-01

    Roč. 150, SI (2018), s. 65-85 ISSN 0032-0633 EU Projects: European Commission(XE) 654208 - EPN2020-RI Institutional support: RVO:68378289 Keywords : Virtual Observatory * Solar System * GIS Subject RIV: BN - Astronomy, Celestial Mechanics, Astrophysics OBOR OECD: Astronomy (including astrophysics,space science) Impact factor: 1.892, year: 2016 https://www.sciencedirect.com/science/article/pii/S0032063316304937#gs1

  20. 150th Anniversary of the Astronomical Observatory Library of Sciences

    Science.gov (United States)

    Solntseva, T.

    The scientific library of the Astronomical observatory of Kyiv Taras Shevchenko University is one of the oldest ones of such a type in Ukraine. Our Astronomical Observatory and its scientific library will celebrate 150th anniversary of their foundation. 900 volumes of duplicates of Olbers' private library underlay our library. These ones were acquired by Russian Academy of Sciences for Poulkovo observatory in 1841 but according to Struve's order were transmitted to Kyiv Saint Volodymyr University. These books are of great value. There are works edited during Copernicus', Kepler's, Galilei's, Newton's, Descartes' lifetime. Our library contains more than 100000 units of storage - monographs, periodical astronomical editions from the first (Astronomische Nachrichten, Astronomical journal, Monthly Notices etc.), editions of the majority of the astronomical observatories and institutions of the world, unique astronomical atlases and maps

  1. Science Initiatives of the US Virtual Astronomical Observatory

    Science.gov (United States)

    Hanisch, R. J.

    2012-09-01

    The United States Virtual Astronomical Observatory program is the operational facility successor to the National Virtual Observatory development project. The primary goal of the US VAO is to build on the standards, protocols, and associated infrastructure developed by NVO and the International Virtual Observatory Alliance partners and to bring to fruition a suite of applications and web-based tools that greatly enhance the research productivity of professional astronomers. To this end, and guided by the advice of our Science Council (Fabbiano et al. 2011), we have focused on five science initiatives in the first two years of VAO operations: 1) scalable cross-comparisons between astronomical source catalogs, 2) dynamic spectral energy distribution construction, visualization, and model fitting, 3) integration and periodogram analysis of time series data from the Harvard Time Series Center and NASA Star and Exoplanet Database, 4) integration of VO data discovery and access tools into the IRAF data analysis environment, and 5) a web-based portal to VO data discovery, access, and display tools. We are also developing tools for data linking and semantic discovery, and have a plan for providing data mining and advanced statistical analysis resources for VAO users. Initial versions of these applications and web-based services are being released over the course of the summer and fall of 2011, with further updates and enhancements planned for throughout 2012 and beyond.

  2. Science Initiatives of the US Virtual Astronomical Observatory

    Directory of Open Access Journals (Sweden)

    Hanisch Robert J.

    2012-09-01

    Full Text Available The United States Virtual Astronomical Observatory program is the operational facility successor to the National Virtual Observatory development project. The primary goal of the US VAO is to build on the standards, protocols, and associated infrastructure developed by NVO and the International Virtual Observatory Alliance partners and to bring to fruition a suite of applications and web-based tools that greatly enhance the research productivity of professional astronomers. To this end, and guided by the advice of our Science Council (advisory committee, we are focusing on five science initiatives in the first two years of VAO operations: (1 scalable cross-comparisons between astronomical source catalogs, (2 dynamic spectral energy distribution construction, visualization, and model fitting, (3 integration and periodogram analysis of time series data from the Harvard Time Series Center and NASA Star and Exoplanet Database, (4 integration of VO data discovery and access tools into the IR AF data analysis environment, and (5 a web-based portal to VO data discovery, access, and display tools. We are also developing tools for data linking and semantic discovery, and have a plan for providing data mining and advanced statistical analysis resources for VAO users. Initial versions of these applications and web-based services are being released over the course of the summer and fall of 2011, with further updates and enhancements planned for throughout 2012 and beyond.

  3. On-Orbit Performance of the Helioseismic and Magnetic Imager Instrument onboard the Solar Dynamics Observatory

    Science.gov (United States)

    Hoeksema, J. T.; Baldner, C. S.; Bush, R. I.; Schou, J.; Scherrer, P. H.

    2018-03-01

    The Helioseismic and Magnetic Imager (HMI) instrument is a major component of NASA's Solar Dynamics Observatory (SDO) spacecraft. Since commencement of full regular science operations on 1 May 2010, HMI has operated with remarkable continuity, e.g. during the more than five years of the SDO prime mission that ended 30 September 2015, HMI collected 98.4% of all possible 45-second velocity maps; minimizing gaps in these full-disk Dopplergrams is crucial for helioseismology. HMI velocity, intensity, and magnetic-field measurements are used in numerous investigations, so understanding the quality of the data is important. This article describes the calibration measurements used to track the performance of the HMI instrument, and it details trends in important instrument parameters during the prime mission. Regular calibration sequences provide information used to improve and update the calibration of HMI data. The set-point temperature of the instrument front window and optical bench is adjusted regularly to maintain instrument focus, and changes in the temperature-control scheme have been made to improve stability in the observable quantities. The exposure time has been changed to compensate for a 20% decrease in instrument throughput. Measurements of the performance of the shutter and tuning mechanisms show that they are aging as expected and continue to perform according to specification. Parameters of the tunable optical-filter elements are regularly adjusted to account for drifts in the central wavelength. Frequent measurements of changing CCD-camera characteristics, such as gain and flat field, are used to calibrate the observations. Infrequent expected events such as eclipses, transits, and spacecraft off-points interrupt regular instrument operations and provide the opportunity to perform additional calibration. Onboard instrument anomalies are rare and seem to occur quite uniformly in time. The instrument continues to perform very well.

  4. Design and Ground Calibration of the Helioseismic and Magnetic Imager (HMI) Instrument on the Solar Dynamics Observatory (SDO)

    Science.gov (United States)

    Schou, J.; Scherrer, P. H.; Bush, R. I.; Wachter, R.; Couvidat, S.; Rabello-Soares, M. C.; Bogart, R. S.; Hoeksema, J. T.; Liu, Y.; Duvall, T. L., Jr.; hide

    2012-01-01

    The Helioseismic and Magnetic Imager (HMI) investigation will study the solar interior using helioseismic techniques as well as the magnetic field near the solar surface. The HMI instrument is part of the Solar Dynamics Observatory (SDO) that was launched on 11 February 2010. The instrument is designed to measure the Doppler shift, intensity, and vector magnetic field at the solar photosphere using the 6173 Fe I absorption line. The instrument consists of a front-window filter, a telescope, a set of wave plates for polarimetry, an image-stabilization system, a blocking filter, a five-stage Lyot filter with one tunable element, two wide-field tunable Michelson interferometers, a pair of 4096(exo 2) pixel cameras with independent shutters, and associated electronics. Each camera takes a full-disk image roughly every 3.75 seconds giving an overall cadence of 45 seconds for the Doppler, intensity, and line-of-sight magnetic-field measurements and a slower cadence for the full vector magnetic field. This article describes the design of the HMI instrument and provides an overview of the pre-launch calibration efforts. Overviews of the investigation, details of the calibrations, data handling, and the science analysis are provided in accompanying articles.

  5. Social Media Programs at the National Optical Astronomy Observatory

    Science.gov (United States)

    Sparks, Robert T.; Walker, Constance Elaine; Pompea, Stephen M.

    2015-08-01

    Observatories and other science research organizations want to share their research and activities with the public. The last several years, social media has become and increasingly important venue for communicating information about observatory activities, research and education and public outreach.The National Optical Astronomy Observatory (NOAO) uses a wide variety of social media to communicate with different audiences. NOAO is active on social media platforms including Facebook, Twitter, Google+ and Pinterest. Our social media accounts include those for the National Optical Astronomy Observatory, Cerro Tololo Inter-American Observatory, Kitt Peak National Observatory and our dark skies conservation program Globe at Night.Our social media programs have a variety of audiences. NOAO uses social media to announce and promote NOAO sponsored meetings, observatory news and proposal deadlines to the professional astronomical community. Social media accounts are used to disseminate NOAO press releases, images from the observatory and other science using data from NOAO telescopes.Social media is important in our Education and Public Outreach programs (EPO). Globe at Night has very active facebook and twitter accounts encouraging people to become involved in preserving dark skies. Social media plays a role in recruiting teachers for professional development workshops such as Project Astro.NOAO produces monthly podcasts for the 365 Days of Astronomy podcast featuring interviews with NOAO astronomers. Each podcast highlights the science of an NOAO astronomer, an NOAO operated telescope or instrument, or an NOAO program. A separate series of podcasts is produced for NOAO’s Dark Skies Education programs. All the podcasts are archived at 365daysofastronomy.org.

  6. The National Virtual Observatory Science Definintion Team: Report and Status

    Science.gov (United States)

    Djorgovski, S. G.; NVO SDT Team

    2002-05-01

    Astronomy has become an enormously data-rich science, with numerous multi-Terabyte sky surveys and archives over the full range of wavelengths, and Petabyte-scale data sets already on the horizon. The amount of the available information is growing exponentially, largely driven by the progress in detector and information technology, and the quality and complexity of the data are unprecedented. This great quantitative advance will result in qualitative changes in the way astronomy is done. The Virtual Observatory concept is the astronomy community's organized response to the challenges posed by efficient handling and scientific exploration of new, massive data sets. The NAS Decadal Survey, Astronomy and Astrophysics in the New Millennium, recommends as the first priority in the ``small'' projects category creation of the National Virtual Observatory (NVO). In response to this, the NSF and NASA formed in June 2001 the NVO Science Definition Team (SDT), with a mandate to: (1) Define and formulate a joint NASA/NSF initiative to pursue the NVO goals; (2) Solicit input from the U.S. astronomy community, and incorporate it in the NVO definition documents and recommendations for further actions; and (3) Serve as liaison to broader space science, computer science, and statistics communities for the NVO initiative, and as liaison with the similar efforts in Europe, looking forward towards a truly Global Virtual Observatory. The Team has delivered its report to the agencies and made it publicly available on its website (http://nvosdt.org), where many other relevant links can be found. We will summarize the report, its conclusions, and recommendations.

  7. The MicroObservatory Net

    Science.gov (United States)

    Brecher, K.; Sadler, P.

    1994-12-01

    A group of scientists, engineers and educators based at the Harvard-Smithsonian Center for Astrophysics (CfA) has developed a prototype of a small, inexpensive and fully integrated automated astronomical telescope and image processing system. The project team is now building five second generation instruments. The MicroObservatory has been designed to be used for classroom instruction by teachers as well as for original scientific research projects by students. Probably in no other area of frontier science is it possible for a broad spectrum of students (not just the gifted) to have access to state-of-the-art technologies that would allow for original research. The MicroObservatory combines the imaging power of a cooled CCD, with a self contained and weatherized reflecting optical telescope and mount. A microcomputer points the telescope and processes the captured images. The MicroObservatory has also been designed to be used as a valuable new capture and display device for real time astronomical imaging in planetariums and science museums. When the new instruments are completed in the next few months, they will be tried with high school students and teachers, as well as with museum groups. We are now planning to make the MicroObservatories available to students, teachers and other individual users over the Internet. We plan to allow the telescope to be controlled in real time or in batch mode, from a Macintosh or PC compatible computer. In the real-time mode, we hope to give individual access to all of the telescope control functions without the need for an "on-site" operator. Users would sign up for a specific period of time. In the batch mode, users would submit jobs for the telescope. After the MicroObservatory completed a specific job, the images would be e-mailed back to the user. At present, we are interested in gaining answers to the following questions: (1) What are the best approaches to scheduling real-time observations? (2) What criteria should be used

  8. The Cherenkov Telescope Array Observatory: top level use cases

    Science.gov (United States)

    Bulgarelli, A.; Kosack, K.; Hinton, J.; Tosti, G.; Schwanke, U.; Schwarz, J.; Colomé, P.; Conforti, V.; Khelifi, B.; Goullon, J.; Ong, R.; Markoff, S.; Contreras, J. L.; Lucarelli, F.; Antonelli, L. A.; Bigongiari, C.; Boisson, C.; Bosnjak, Z.; Brau-Nogué, S.; Carosi, A.; Chen, A.; Cotter, G.; Covino, S.; Daniel, M.; De Cesare, G.; de Ona Wilhelmi, E.; Della Volpe, M.; Di Pierro, F.; Fioretti, V.; Füßling, M.; Garczarczyk, M.; Gaug, M.; Glicenstein, J. F.; Goldoni, P.; Götz, D.; Grandi, P.; Heller, M.; Hermann, G.; Inoue, S.; Knödlseder, J.; Lenain, J.-P.; Lindfors, E.; Lombardi, S.; Luque-Escamilla, P.; Maier, G.; Marisaldi, M.; Mundell, C.; Neyroud, N.; Noda, K.; O'Brien, P.; Petrucci, P. O.; Martí Ribas, J.; Ribó, M.; Rodriguez, J.; Romano, P.; Schmid, J.; Serre, N.; Sol, H.; Schussler, F.; Stamerra, A.; Stolarczyk, T.; Vandenbrouck, J.; Vercellone, S.; Vergani, S.; Zech, A.; Zoli, A.

    2016-08-01

    Today the scientific community is facing an increasing complexity of the scientific projects, from both a technological and a management point of view. The reason for this is in the advance of science itself, where new experiments with unprecedented levels of accuracy, precision and coverage (time and spatial) are realised. Astronomy is one of the fields of the physical sciences where a strong interaction between the scientists, the instrument and software developers is necessary to achieve the goals of any Big Science Project. The Cherenkov Telescope Array (CTA) will be the largest ground-based very high-energy gamma-ray observatory of the next decades. To achieve the full potential of the CTA Observatory, the system must be put into place to enable users to operate the telescopes productively. The software will cover all stages of the CTA system, from the preparation of the observing proposals to the final data reduction, and must also fit into the overall system. Scientists, engineers, operators and others will use the system to operate the Observatory, hence they should be involved in the design process from the beginning. We have organised a workgroup and a workflow for the definition of the CTA Top Level Use Cases in the context of the Requirement Management activities of the CTA Observatory. Scientists, instrument and software developers are collaborating and sharing information to provide a common and general understanding of the Observatory from a functional point of view. Scientists that will use the CTA Observatory will provide mainly Science Driven Use Cases, whereas software engineers will subsequently provide more detailed Use Cases, comments and feedbacks. The main purposes are to define observing modes and strategies, and to provide a framework for the flow down of the Use Cases and requirements to check missing requirements and the already developed Use-Case models at CTA sub-system level. Use Cases will also provide the basis for the definition of

  9. OCO-2 (Orbiting Carbon Observatory-2) mission operations planning and initial operations experiences

    Science.gov (United States)

    Basilio, Ralph R.; Pollock, H. Randy; Hunyadi-Lay, Sarah L.

    2014-10-01

    OCO-2 (Orbiting Carbon Observatory-2) is the first NASA (National Aeronautics and Space Administration) mission dedicated to studying atmospheric carbon dioxide, specifically to identify sources (emitters) and sinks (absorbers) on a regional (1000 km x 1000 km) scale. The mission is designed to meet a science imperative by providing critical and urgent measurements needed to improve understanding of the carbon cycle and global climate change processes. The single instrument consisting of three grating spectrometers was built at the Jet Propulsion Laboratory, but is based on the design co-developed with Hamilton Sundstrand Corporation for the original OCO mission. The instrument underwent an extensive ground test program. This was generally made possible through the use of a thermal vacuum chamber with a window/port that allowed optical ground support equipment to stimulate the instrument. The instrument was later delivered to Orbital Sciences Corporation for integration and test with the LEOStar-2 spacecraft. During the overall ground test campaign, proper function and performance in simulated launch, ascent, and space environments were verified. The observatory was launched into space on 02 July 2014. Initial indications are that the instrument is meeting functional and performance specifications, and there is every expectation that the spatially-order, geo-located, calibrated spectra of reflected sunlight and the science retrievals will meet the Level 1 science requirements.

  10. Diverse Portfolio of Scientific Instrumentation Initiatives of the Deep Carbon Observatory

    Science.gov (United States)

    Schiffries, Craig; Hazen, Robert; Hemley, Russell; Mangum, Andrea

    2016-04-01

    Advances in scientific instrumentation are important drivers of scientific discovery. The Deep Carbon Observatory (DCO) supports a diverse portfolio of scientific instrumentation initiatives worldwide as part of its ten-year quest to achieve a transformational understanding of the quantities, movements, origins, and forms of Earth's deep carbon. Substantial progress has been made in the development of a wide range of instruments, including: • Quantum cascade laser-infrared absorption spectrometer for clumped methane isotope thermometry (Shuhei Ono) • Large-radius high-mass-resolution multiple-collector isotope ratio mass spectrometer for analysis of rare isotopologues of methane and other gases (Edward Young, Douglas Rumble) • Volcanic field deployment of the laser isotope ratio-meter (Damien Weidmann) • Novel large-volume diamond anvil cell for neutron scattering (Malcolm Guthrie, Reinhard Boehler) • Novel synchrotron x-ray probes for deep carbon (Wendy Mao) • Ultrafast laser instrument for in situ measurements of elastic, electronic, and transport properties of carbon-bearing fluids and crystalline materials (Alexander Goncharov) • Combined instrument for molecular imaging in geochemistry (Andrew Steele) • Pressurized Underwater Sample Handler (Isabelle Daniel, Karyn Rogers) These and other DCO instrumentation projects are highly leveraged investments involving a large number of sponsors, partners, and collaborators.

  11. Systems approach to the design of the CCD sensors and camera electronics for the AIA and HMI instruments on solar dynamics observatory

    Science.gov (United States)

    Waltham, N.; Beardsley, S.; Clapp, M.; Lang, J.; Jerram, P.; Pool, P.; Auker, G.; Morris, D.; Duncan, D.

    2017-11-01

    Solar Dynamics Observatory (SDO) is imaging the Sun in many wavelengths near simultaneously and with a resolution ten times higher than the average high-definition television. In this paper we describe our innovative systems approach to the design of the CCD cameras for two of SDO's remote sensing instruments, the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI). Both instruments share use of a custom-designed 16 million pixel science-grade CCD and common camera readout electronics. A prime requirement was for the CCD to operate with significantly lower drive voltages than before, motivated by our wish to simplify the design of the camera readout electronics. Here, the challenge lies in the design of circuitry to drive the CCD's highly capacitive electrodes and to digitize its analogue video output signal with low noise and to high precision. The challenge is greatly exacerbated when forced to work with only fully space-qualified, radiation-tolerant components. We describe our systems approach to the design of the AIA and HMI CCD and camera electronics, and the engineering solutions that enabled us to comply with both mission and instrument science requirements.

  12. Combined Raman/Infrared Reflectance Instrument for In Situ Mineral Analysis, Phase I

    Data.gov (United States)

    National Aeronautics and Space Administration — NASA's Science Instruments, Observatories, and Sensor Systems Roadmap calls for instruments capable of in situ mineralogical analysis in support of planetary...

  13. Invited Review Article: The Chandra X-ray Observatory

    Science.gov (United States)

    Schwartz, Daniel A.

    2014-06-01

    The Chandra X-ray Observatory is an orbiting x-ray telescope facility. It is one of the National Aeronautics and Space Administration's four "Great Observatories" that collectively have carried out astronomical observations covering the infrared through gamma-ray portion of the electromagnetic spectrum. Chandra is used by astronomers world-wide to acquire imaging and spectroscopic data over a nominal 0.1-10 keV (124-1.24 Å) range. We describe the three major parts of the observatory: the telescope, the spacecraft systems, and the science instruments. This article will emphasize features of the design and development driven by some of the experimental considerations unique to x-ray astronomy. We will update the on-orbit performance and present examples of the scientific highlights.

  14. UNESCO Global Ethics Observatory: database on ethics related legislation and guidelines.

    NARCIS (Netherlands)

    Ang, T.W.; Have, H.A.M.J. ten; Solbakk, J.H.; Nys, H.

    2008-01-01

    The Database on Ethics Related Legislation and Guidelines was launched in March 2007 as the fourth database of the UNESCO Global Ethics Observatory system of databases in ethics of science and technology. The database offers a collection of legal instruments searchable by region, country, bioethical

  15. Observatories of Sawai Jai Singh II

    Science.gov (United States)

    Johnson-Roehr, Susan N.

    Sawai Jai Singh II, Maharaja of Amber and Jaipur, constructed five observatories in the second quarter of the eighteenth century in the north Indian cities of Shahjahanabad (Delhi), Jaipur, Ujjain, Mathura, and Varanasi. Believing the accuracy of his naked-eye observations would improve with larger, more stable instruments, Jai Singh reengineered common brass instruments using stone construction methods. His applied ingenuity led to the invention of several outsize masonry instruments, the majority of which were used to determine the coordinates of celestial objects with reference to the local horizon. During Jai Singh's lifetime, the observatories were used to make observations in order to update existing ephemerides such as the Zīj-i Ulugh Begī. Jai Singh established communications with European astronomers through a number of Jesuits living and working in India. In addition to dispatching ambassadorial parties to Portugal, he invited French and Bavarian Jesuits to visit and make use of the observatories in Shahjahanabad and Jaipur. The observatories were abandoned after Jai Singh's death in 1743 CE. The Mathura observatory was disassembled completely before 1857. The instruments at the remaining observatories were restored extensively during the nineteenth and twentieth centuries.

  16. Rigorous noise test and calibration check of strong-motion instrumentation at the Conrad Observatory in Austria.

    Science.gov (United States)

    Steiner, R.; Costa, G.; Lenhardt, W.; Horn, N.; Suhadolc, P.

    2012-04-01

    In the framework of the European InterregIV Italy/Austria project: "HAREIA - Historical and Recent Earthquakes in Italy and Austria" the Central Institute for Meteorology and Geodynamics (ZAMG) and Mathematic and Geosciences Department of University of Trieste (DMG) are upgrading the transfrontier seismic network of South-Eastern Alps with new 12 accelerometric stations to enhance the strong motion instrument density near the Austria/Italy border. Various public institutions of the provinces Alto Adige (Bolzano Province), Veneto (ARPAV) and Friuli Venezia Giulia (Regional Civil Defense) in Italy and in the Austrian province of Tyrol are involved in the project. The site selection was carried out to improve the present local network geometry thus meeting the needs of public Institutions in the involved regions. In Tyrol and Alto Adige some strategic buildings (hospitals and public buildings) have been selected, whereas in Veneto and Friuli Venezia Giulia the sites are in the free field, mainly located near villages. The instruments will be installed in an innovative box, designed by ZAMG, that provides electric and water isolation. The common choice regarding the instrument selection has been the new Kinemetrics Basalt ® accelerograph to guarantee homogeneity with the already installed instrumentation and compatibility with the software already in use at the different seismic institutions in the area. Prior to deployment the equipment was tested at the Conrad Observatory and a common set-up has been devised. The Conrad Observatory, seismically particularly quiet, permits to analyze both the sensor and the acquisition system noise. The instruments were connected to the network and the data sent in real-time to the ZAMG data center in Vienna and the DMG data center in Trieste. The data have been collected in the database and analyzed using signal processing modules PQLX and Matlab. The data analysis of the recordings at the ultra-quiet Conrad Observatory pointed out

  17. Atmospheric Science Research at the Whiteface Mountain Adirondack High Peaks Observatory

    Science.gov (United States)

    Schwab, J. J.; Brandt, R. E.; Casson, P.; Demerjian, K. L.; Crandall, B. A.

    2014-12-01

    The Atmospheric Sciences Research Center established an atmospheric observatory at Whiteface Mountain in the Adirondacks in 1961. The current mountain top observatory building was built by the University at Albany in 1969-70 and the New York State Department of Environmental Conservation (DEC) began ozone measurements at this summit location in 1973. Those measurements continue to this day and constitute a valuable long term data record for tropospheric ozone in the northeastern U.S. The elevation of the summit is 1483 m above sea level, and is roughly 90 m above the tree line in this location. With a mean cloud base height of less than 1100 m at the summit, it is a prime location for cloud research. The research station headquarters, laboratories, offices, and a second measurement site are located at the Marble Mountain Lodge, perched on a shoulder northeast of the massif at an elevation of 604 m above sea level. Parameters measured at the site include meteorological variables, trace gases, precipitation chemistry, aerosol mass and components, and more. Precipitation and cloud chemistry has a long history at the lodge and summit locations, respectively, and continues to this day. Some data from the 40-year record will be shown in the presentation. In the late 1980's the summit site was outfitted with instrumentation to measure oxides of nitrogen and other ozone precursors. Measurements of many of these same parameters were added at the lodge site and continue to this day. In this poster we will give an overview of the Whiteface Mountain Observatory and its two measurement locations. We will highlight the parameters currently being measured at our sites, and indicate those measured by ASRC, as well as those measured by other organizations. We will also recap some of the historical activities and measurement programs that have taken place at the site, as alluded to above. Also included will be examples of the rich archive of trends data for gas phase species

  18. VESPA: developing the planetary science Virtual Observatory in H2020

    Science.gov (United States)

    Erard, Stéphane; Cecconi, Baptiste; Le Sidaner, Pierre; Capria, Teresa; Rossi, Angelo Pio

    2016-04-01

    The Europlanet H2020 programme will develop a research infrastructure in Horizon 2020. The programme includes a follow-on to the FP7 activity aimed at developing the Planetary Science Virtual Observatory (VO). This activity is called VESPA, which stands for Virtual European Solar and Planetary Access. Building on the IDIS activity of Europlanet FP7, VESPA will distribute more data, will improve the connected tools and infrastructure, and will help developing a community of both users and data providers. One goal of the Europlanet FP7 programme was to set the basis for a European Virtual Observatory in Planetary Science. A prototype has been set up during FP7, most of the activity being dedicated to the definition of standards to handle data in this field. The aim was to facilitate searches in big archives as well as sparse databases, to make on-line data access and visualization possible, and to allow small data providers to make their data available in an interoperable environment with minimum effort. This system makes intensive use of studies and developments led in Astronomy (IVOA), Solar Science (HELIO), plasma physics (SPASE), and space archive services (IPDA). It remains consistent with extensions of IVOA standards.

  19. Observatories, think tanks, and community models in the hydrologic and environmental sciences: How does it affect me?

    Science.gov (United States)

    Torgersen, Thomas

    2006-06-01

    Multiple issues in hydrologic and environmental sciences are now squarely in the public focus and require both government and scientific study. Two facts also emerge: (1) The new approach being touted publicly for advancing the hydrologic and environmental sciences is the establishment of community-operated "big science" (observatories, think tanks, community models, and data repositories). (2) There have been important changes in the business of science over the last 20 years that make it important for the hydrologic and environmental sciences to demonstrate the "value" of public investment in hydrological and environmental science. Given that community-operated big science (observatories, think tanks, community models, and data repositories) could become operational, I argue that such big science should not mean a reduction in the importance of single-investigator science. Rather, specific linkages between the large-scale, team-built, community-operated big science and the single investigator should provide context data, observatory data, and systems models for a continuing stream of hypotheses by discipline-based, specialized research and a strong rationale for continued, single-PI ("discovery-based") research. I also argue that big science can be managed to provide a better means of demonstrating the value of public investment in the hydrologic and environmental sciences. Decisions regarding policy will still be political, but big science could provide an integration of the best scientific understanding as a guide for the best policy.

  20. Science Objectives and Design of the European Seas Observatory NETwork (ESONET)

    Science.gov (United States)

    Ruhl, H.; Géli, L.; Karstensen, J.; Colaço, A.; Lampitt, R.; Greinert, J.; Phannkuche, O.; Auffret, Y.

    2009-04-01

    The needs for a network of ocean observing systems cross many applied and research areas of earth and marine science. Many of the science areas that can be examined using such systems have direct impacts on societal health and well being and our understanding of ocean function in a shifting climate. The European Seas Observatory NETwork (ESONET) Network of Excellence has been evaluating ocean observatory design requirements, data management needs, standardization and interoperability concerns, social implications, outreach and education, as well as financial and legal aspects of developing such a system. ESONET has great potential to address a growing set of Earth science questions that require a broad and integrated network of ocean and seafloor observations. ESONET activities are also importantly integrating researchers in the European Community, as well as internationally. There is now wide recognition that research addressing science questions of international priority, such as understanding the potential impacts of climate change or geohazards like earthquakes and tsunamis should be conducted in a framework that can address questions across adequate temporal and spatial scales. We will present the relevant science priorities in the four interconnected fields of geoscience, physical oceanography, biogeochemistry, and marine ecology, and some of the practical ways in which these questions can be addressed using ESONET. Several key questions persist that will require comprehensive interdisciplinary approaches including: How can monitoring of factors such as seismic activity, fluid pore chemistry and pressure, improve seismic, slope failure, and tsunami warning? To what extent do seabed processes influence ocean physics, biogeochemistry, and marine ecosystems? How are physical and biogeochemical processes that occur at differing scales related? What aspects of physical oceanography and biogeochemical cycling will be most sensitive to climate change? What will the

  1. The Science of String Instruments

    CERN Document Server

    Rossing, Thomas D

    2010-01-01

    Many performing musicians, as well as instrument builders, are coming to realize the importance of understanding the science of musical instruments. This book explains how string instruments produce sound. It presents basic ideas in simple language, and it also translates some more sophisticated ideas in non-technical language. It should be of interest to performers, researchers, and instrument makers alike.

  2. Seismic instrumentation plan for the Hawaiian Volcano Observatory

    Science.gov (United States)

    Thelen, Weston A.

    2014-01-01

    The seismic network operated by the U.S. Geological Survey’s Hawaiian Volcano Observatory (HVO) is the main source of authoritative data for reporting earthquakes in the State of Hawaii, including those that occur on the State’s six active volcanoes (Kīlauea, Mauna Loa, Hualālai, Mauna Kea, Haleakalā, Lō‘ihi). Of these volcanoes, Kīlauea and Mauna Loa are considered “very high threat” in a report on the rationale for a National Volcanic Early Warning System (NVEWS) (Ewert and others, 2005). This seismic instrumentation plan assesses the current state of HVO’s seismic network with respect to the State’s active volcanoes and calculates the number of stations that are needed to upgrade the current network to provide a seismic early warning capability for forecasting volcanic activity. Further, the report provides proposed priorities for upgrading the seismic network and a cost assessment for both the installation costs and maintenance costs of the improved network that are required to fully realize the potential of the early warning system.

  3. Improvements to science operations at Kitt Peak National Observatory

    Science.gov (United States)

    Bohannan, Bruce

    1998-07-01

    In recent years Kitt Peak National Observatory has undertaken a number of innovative projects to optimize science operations with the suite of telescopes we operate on Kitt Peak, Arizona. Changing scientific requirements and expectations of our users, evolving technology and declining budgets have motivated the changes. The operations improvements have included telescope performance enhancements--with the focus on the Mayall 4-m--modes of observing and scheduling, telescope control and observing systems, planning and communication, and data archiving.

  4. The BINA collaboration: science at the Royal Observatory of Belgium

    Science.gov (United States)

    De Cat, Peter; Cuypers, Jan; Blomme, Ronny; Frémat, Yves; Groenewegen, Martin; Lampens, Patricia; Lobel, Alex; Pauwels, Thierry; Van de Steene, Griet; van Hoof, Peter

    2018-04-01

    The Belgo-Indian Network for Astronomy and Astrophysics (BINA) is a collaboration between Indian and Belgian astronomical institutes with the main aim to optimize the scientific output of the Indo-Belgian telescopes, being the 4.0-m International Liquid Mirror Telescope and the 3.6-m Devasthal Optical Telescope. These new facilities are both located at the Devasthal Observatory near Nainital, India. In this contribution, we introduce projects that are of scientific interest for colleagues of the department "Astronomy and Astrophysics" of the Royal Observatory of Belgium (ROB). It serves as an invitation for Indian astronomers to participate. We highlight how these projects could benefit from observations with the Indo-Belgian telescopes by using instruments from the first-generation (currently offered) and/or the next-generation (development or design phase). We show that, from an ROB point-of-view, the BINA would be the most successful if the 3.6-m DOT would be equipped with an efficient optical high-resolution spectrograph.

  5. A case study about the Colombian Observatory of Science and Technology: between context relevant and internationally comparable indicators

    Energy Technology Data Exchange (ETDEWEB)

    Salazar, M.; Crespi, G.

    2016-07-01

    In very few countries around the world there are observatories for the design and production of science, technology and innovation (STI) indicators; mainly government organizations in charge of STI funding or national statistical agencies are the ones in charge of these activities. The purpose of this study is to assess the evolution and the results of the Colombian Observatory of Science and Technology (OCyT by its name in Spanish). The main objective is to explore if the Colombian model for the production of STI has been successful, if it is sustainable and what key institutional factors should be taken into consideration previously to replicate this experience in other contexts. The OCyT was created because there was a clear need, mainly within Colciencias’ policy makers and managers, to have regular and reliable indicators supporting the design and evaluation of STI policies Even if Colciencias has this responsibility, it chose to create an independent institution and innovated regarding the organizational arrangement not a subsidiary agency. As a not for profit organization and a public private partnership certainly the sustainability of the Observatory relies on the one hand, on the support provided by its associates (mainly Colciencias) and, on the other hand, on project funding. The issue at stake is if the OCyT should remain mainly as an indicator producer (its main goal and what it is paid for) or evolves into a research organization (knowledge producer), a consultant (service provider), or a combination of all. How to maintain a balance between national needs and international standards? Indicators should help policy makers to design, monitor and evaluate policies, programs and instruments, and in that sense indicators should be customized to their necessities. In addition, indicators are also used to make international comparisons, therefore the need to adopt international standards and guidelines. (Author)

  6. Improvements in geomagnetic observatory data quality

    DEFF Research Database (Denmark)

    Reda, Jan; Fouassier, Danielle; Isac, Anca

    2011-01-01

    between observatories and the establishment of observatory networks has harmonized standards and practices across the world; improving the quality of the data product available to the user. Nonetheless, operating a highquality geomagnetic observatory is non-trivial. This article gives a record...... of the current state of observatory instrumentation and methods, citing some of the general problems in the complex operation of geomagnetic observatories. It further gives an overview of recent improvements of observatory data quality based on presentation during 11th IAGA Assembly at Sopron and INTERMAGNET...

  7. The Lowell Observatory Predoctoral Scholar Program

    Science.gov (United States)

    Prato, Lisa; Nofi, Larissa

    2018-01-01

    Lowell Observatory is pleased to solicit applications for our Predoctoral Scholar Fellowship Program. Now beginning its tenth year, this program is designed to provide unique research opportunities to graduate students in good standing, currently enrolled at Ph.D. granting institutions. Lowell staff research spans a wide range of topics, from astronomical instrumentation, to icy bodies in our solar system, exoplanet science, stellar populations, star formation, and dwarf galaxies. Strong collaborations, the new Ph.D. program at Northern Arizona University, and cooperative links across the greater Flagstaff astronomical community create a powerful multi-institutional locus in northern Arizona. Lowell Observatory's new 4.3 meter Discovery Channel Telescope is operating at full science capacity and boasts some of the most cutting-edge and exciting capabilities available in optical/infrared astronomy. Student research is expected to lead to a thesis dissertation appropriate for graduation at the doctoral level at the student's home institution. For more information, see http://www2.lowell.edu/rsch/predoc.php and links therein. Applications for Fall 2018 are due by May 1, 2018; alternate application dates will be considered on an individual basis.

  8. The Ocean Observatories Initiative: Data, Data and More Data

    Science.gov (United States)

    Crowley, M. F.; Vardaro, M.; Belabbassi, L.; Smith, M. J.; Garzio, L. M.; Knuth, F.; Glenn, S. M.; Schofield, O.; Lichtenwalner, C. S.; Kerfoot, J.

    2016-02-01

    The Ocean Observatories Initiative (OOI), a project funded by the National Science Foundation (NSF) and managed by the Consortium for Ocean Leadership, is a networked infrastructure of science-driven sensor systems that measure the physical, chemical, geological, and biological variables in the ocean and seafloor on coastal, regional, and global scales. OOI long term research arrays have been installed off the Washington coast (Cabled), Massachusetts and Oregon coasts (Coastal) and off Alaska, Greenland, Chile and Argentina (Global). Woods Hole Oceanographic Institution and Oregon State University are responsible for the coastal and global moorings and their autonomous vehicles. The University of Washington is responsible for cabled seafloor systems and moorings. Rutgers University operates the Cyberinfrastructure (CI) portion of the OOI, which acquires, processes and distributes data to the scientists, researchers, educators and the public. It also provides observatory mission command and control, data assessment and distribution, and long-term data management. This talk will present an overview of the OOI infrastructure and its three primary websites which include: 1) An OOI overview website offering technical information on the infrastructure ranging from instruments to science goals, news, deployment updates, and information on the proposal process, 2) The Education and Public Engagement website where students can view and analyze exactly the same data that scientists have access to at exactly the same time, but with simple visualization tools and compartmentalized lessons that lead them through complex science questions, and 3) The primary data access website and machine to machine interface where anyone can plot or download data from the over 700 instruments within the OOI Network.

  9. Increased Science Instrumentation Funding Strengthens Mars Program

    Science.gov (United States)

    Graham, Lee D.; Graff, T. G.

    2012-01-01

    As the strategic knowledge gaps mature for the exploration of Mars, Mars sample return (MSR), and Phobos/Deimos missions, one approach that becomes more probable involves smaller science instrumentation and integrated science suites. Recent technological advances provide the foundation for a significant evolution of instrumentation; however, the funding support is currently too small to fully utilize these advances. We propose that an increase in funding for instrumentation development occur in the near-term so that these foundational technologies can be applied. These instruments would directly address the significant knowledge gaps for humans to Mars orbit, humans to the Martian surface, and humans to Phobos/ Deimos. They would also address the topics covered by the Decadal Survey and the Mars scientific goals, objectives, investigations and priorities as stated by the MEPAG. We argue that an increase of science instrumentation funding would be of great benefit to the Mars program as well as the potential for human exploration of the Mars system. If the total non-Earth-related planetary science instrumentation budget were increased 100% it would not add an appreciable amount to the overall NASA budget and would provide the real potential for future breakthroughs. If such an approach were implemented in the near-term, NASA would benefit greatly in terms of science knowledge of the Mars, Phobos/Deimos system, exploration risk mitigation, technology development, and public interest.

  10. Astrbiology Science and Technology for Instrument Development (ASTID)

    Data.gov (United States)

    National Aeronautics and Space Administration — The Astrobiology Science and Technology for Instrument Development (ASTID) develops instrumentation capabilities to help meet Astrobiology science requirements on...

  11. Design, Observing and Data Systems, and Final Installation of the NEPTUNE Canada Regional Cabled Ocean Observatory

    Science.gov (United States)

    Barnes, C. R.; Best, M. M.; Johnson, F. R.; Phibbs, P.; Pirenne, B.

    2009-05-01

    NEPTUNE Canada (NC; www.neptunecanada.ca) will complete most of the installation of the world's first regional cabled ocean observatory in late 2009 off Canada's west coast. It will comprise five main observatory nodes (100-2700m water depths) linked by an 800km backbone cable delivering 10kVDC power and 10Gbps communications bandwidth to hundreds of sensors, with a 25-year design life. Infrastructure (100M) and initial operational funding (20M) is secured. University of Victoria (UVic) leads a consortium of 12 Canadian universities, hosts the coastal VENUS cabled observatory, with Ocean Networks Canada (ONC) providing management oversight. Observatory architecture has a trunk and branch topology. Installed in late 2007, the backbone cable loops from/to UVic's Port Alberni shore station. The wet plant's design, manufacture and installation was contracted to Alcatel-Lucent. Each node provides six interface ports for connection of science instrument arrays or extensions. Each port provides dual optical Ethernet links and up to 9kW of electrical power at 400VDC. Junction boxes, designed and built by OceanWorks support up to 10 instruments each and can be daisy- chained. They accommodate both serial and 10/100 Ethernet instruments, and provide a variety of voltages (400V, 48V, 24V, 15V). Backbone equipment has all been qualified and installed; shore station re-equipping is complete; junction boxes are manufactured. A major marine program will deploy nodes and instruments in July-September 2009; instruments to one node will probably be deferred until 2010. Observatory instruments will be deployed in subsurface (boreholes), on seabed, and buoyed through the water column. Over 130 instruments (over 40 different types) will host several hundred sensors; mobile assets include a tethered crawler and a 400m vertical profiler. Experiments will address: earthquake dynamics and tsunami hazards; fluid fluxes in both ocean crust and sediments, including gas hydrates; ocean

  12. A next generation Ultra-Fast Flash Observatory (UFFO-100) for IR/optical observations of the rise phase of gamma-ray bursts

    DEFF Research Database (Denmark)

    Grossan, B.; Park, I.H.; Ahmad, S.

    2012-01-01

    generation of rapid-response space observatory instruments. We list science topics motivating ourinstruments, those that require rapid optical-IR GRB response, including: A survey of GRB rise shapes/times,measurements of optical bulk Lorentz factors, investigation of magnetic dominated (vs. non-magnetic) jet...... for a next generation space observatory as a secondinstrument on a low-earth orbit spacecraft, with a 120 kg instrument mass budget. Restricted to relatively modest mass,power, and launch resources, we find that a coded mask X-ray camera with 1024 cm2 of detector area could rapidlylocate about 64...

  13. A Computer-Based Instrument That Identifies Common Science Misconceptions

    Science.gov (United States)

    Larrabee, Timothy G.; Stein, Mary; Barman, Charles

    2006-01-01

    This article describes the rationale for and development of a computer-based instrument that helps identify commonly held science misconceptions. The instrument, known as the Science Beliefs Test, is a 47-item instrument that targets topics in chemistry, physics, biology, earth science, and astronomy. The use of an online data collection system…

  14. Bright THz Instrument and Nonlinear THz Science

    Science.gov (United States)

    2017-10-30

    Report: Bright THz Instrument and Nonlinear THz Science The views, opinions and/or findings contained in this report are those of the author(s) and...Number: W911NF-16-1-0436 Organization: University of Rochester Title: Bright THz Instrument and Nonlinear THz Science Report Term: 0-Other Email: xi...exploring new cutting-edge research and broader applications, following the significant development of THz science and technology in the late 80’s, is the

  15. Advances in instrumentation at the W. M. Keck Observatory

    Science.gov (United States)

    Adkins, Sean M.; Armandroff, Taft E.; Johnson, James; Lewis, Hilton A.; Martin, Christopher; McLean, Ian S.; Wizinowich, Peter

    2012-09-01

    In this paper we describe both recently completed instrumentation projects and our current development efforts in terms of their role in the strategic plan, the key science areas they address, and their performance as measured or predicted. Projects reaching completion in 2012 include MOSFIRE, a near IR multi-object spectrograph, a laser guide star adaptive optics facility on the Keck I telescope, and an upgrade to the guide camera for the HIRES instrument on Keck I. Projects in development include a new seeing limited integral field spectrograph for the visible wavelength range called the Keck Cosmic Web Imager (KCWI), an upgrade to the telescope control systems on both Keck telescopes, a near-IR tip/tilt sensor for the Keck I adaptive optics system, and a new grating for the OSIRIS integral field spectrograph.

  16. Deep Carbon Observatory investigates Carbon from Crust to Core: An Academic Record of the History of Deep Carbon Science

    Science.gov (United States)

    Mitton, S. A.

    2017-12-01

    Carbon plays an unparalleled role in our lives: as the element of life, as the basis of most of society's energy, as the backbone of most new materials, and as the central focus in efforts to understand Earth's variable and uncertain climate. Yet in spite of carbon's importance, scientists remain largely ignorant of the physical, chemical, and biological behavior of many of Earth's carbon-bearing systems. The Deep Carbon Observatory (DCO) is a global research program to transform our understanding of carbon in Earth. At its heart, DCO is a community of scientists, from biologists to physicists, geoscientists to chemists, and many others whose work crosses these disciplinary lines, forging a new, integrative field of deep carbon science. As a historian of science, I specialise in the history of planetary science and astronomy since 1900. This is directed toward understanding of the history of the steps on the road to discovering the internal dynamics of our planet. Within a framework that describes the historical background to the new field of Earth System Science, I present the first history of deep carbon science. This project will identifies the key discoveries of deep carbon science. It will assess the impact of new knowledge on geochemistry, geodynamics, and geobiology. The project will lead to publication, in book form in 2019, of an illuminating narrative that will highlight the engaging human stories of many remarkable scientists and natural philosophers from whom we have learned about the complexity of Earth's internal world. On this journey of discovery we will encounter not just the pioneering researchers of deep carbon science, but also their institutions, their instrumental inventiveness, and their passion for exploration. The book is organised thematically around the four communities of the Deep Carbon Observatory: Deep Life, Extreme Physics and Chemistry, Reservoirs and Fluxes, and Deep Energy. The presentation has a gallery and list of Deep Carbon

  17. The Astrophysical Multimessenger Observatory Network (AMON)

    Science.gov (United States)

    Smith. M. W. E.; Fox, D. B.; Cowen, D. F.; Meszaros, P.; Tesic, G.; Fixelle, J.; Bartos, I.; Sommers, P.; Ashtekar, Abhay; Babu, G. Jogesh; hide

    2013-01-01

    We summarize the science opportunity, design elements, current and projected partner observatories, and anticipated science returns of the Astrophysical Multimessenger Observatory Network (AMON). AMON will link multiple current and future high-energy, multimessenger, and follow-up observatories together into a single network, enabling near real-time coincidence searches for multimessenger astrophysical transients and their electromagnetic counterparts. Candidate and high-confidence multimessenger transient events will be identified, characterized, and distributed as AMON alerts within the network and to interested external observers, leading to follow-up observations across the electromagnetic spectrum. In this way, AMON aims to evoke the discovery of multimessenger transients from within observatory subthreshold data streams and facilitate the exploitation of these transients for purposes of astronomy and fundamental physics. As a central hub of global multimessenger science, AMON will also enable cross-collaboration analyses of archival datasets in search of rare or exotic astrophysical phenomena.

  18. Instrumentation between science, state and industry

    CERN Document Server

    Shinn, Terry

    2001-01-01

    these. In this book, we appropriate their conception of research-technology, and ex­ tend it to many other phenomena which are less stable and less localized in time and space than the Zeeman/Cotton situation. In the following pages, we use the concept for instances where research activities are orientated primarily toward technologies which facilitate both the production of scientific knowledge and the production of other goods. In particular, we use the tenn for instances where instruments and meth­ ods· traverse numerous geographic and institutional boundaries; that is, fields dis­ tinctly different and distant from the instruments' and methods' initial focus. We suggest that instruments such as the ultra-centrifuge, and the trajectories of the men who devise such artefacts, diverge in an interesting way from other fonns of artefacts and careers in science, metrology and engineering with which students of science and technology are more familiar. The instrument systems developed by re­ search-technolo...

  19. Pro-Amateur Observatories as a Significant Resource for Professional Astronomers - Taurus Hill Observatory

    Science.gov (United States)

    Haukka, H.; Hentunen, V.-P.; Nissinen, M.; Salmi, T.; Aartolahti, H.; Juutilainen, J.; Vilokki, H.

    2013-09-01

    Taurus Hill Observatory (THO), observatory code A95, is an amateur observatory located in Varkaus, Finland. The observatory is maintained by the local astronomical association of Warkauden Kassiopeia [8]. THO research team has observed and measured various stellar objects and phenomena. Observatory has mainly focuse d on asteroid [1] and exoplanet light curve measurements, observing the gamma rays burst, supernova discoveries and monitoring [2]. We also do long term monitoring projects [3]. THO research team has presented its research work on previous EPSC meetings ([4], [5],[6], [7]) and got very supportive reactions from the European planetary science community. The results and publications that pro-amateur based observatories, like THO, have contributed, clearly demonstrates that pro-amateurs area significant resource for the professional astronomers now and even more in the future.

  20. The Carl Sagan solar and stellar observatories as remote observatories

    Science.gov (United States)

    Saucedo-Morales, J.; Loera-Gonzalez, P.

    In this work we summarize recent efforts made by the University of Sonora, with the goal of expanding the capability for remote operation of the Carl Sagan Solar and Stellar Observatories, as well as the first steps that have been taken in order to achieve autonomous robotic operation in the near future. The solar observatory was established in 2007 on the university campus by our late colleague A. Sánchez-Ibarra. It consists of four solar telescopes mounted on a single equatorial mount. On the other hand, the stellar observatory, which saw the first light on 16 February 2010, is located 21 km away from Hermosillo, Sonora at the site of the School of Agriculture of the University of Sonora. Both observatories can now be remotely controlled, and to some extent are able to operate autonomously. In this paper we discuss how this has been accomplished in terms of the use of software as well as the instruments under control. We also briefly discuss the main scientific and educational objectives, the future plans to improve the control software and to construct an autonomous observatory on a mountain site, as well as the opportunities for collaborations.

  1. Design and Implementation of Data Reduction Pipelines for the Keck Observatory Archive

    Science.gov (United States)

    Gelino, C. R.; Berriman, G. B.; Kong, M.; Laity, A. C.; Swain, M. A.; Campbell, R.; Goodrich, R. W.; Holt, J.; Lyke, J.; Mader, J. A.; Tran, H. D.; Barlow, T.

    2015-09-01

    The Keck Observatory Archive (KOA), a collaboration between the NASA Exoplanet Science Institute and the W. M. Keck Observatory, serves science and calibration data for all active and inactive instruments from the twin Keck Telescopes located near the summit of Mauna Kea, Hawaii. In addition to the raw data, we produce and provide quick look reduced data for four instruments (HIRES, LWS, NIRC2, and OSIRIS) so that KOA users can more easily assess the scientific content and the quality of the data, which can often be difficult with raw data. The reduced products derive from both publicly available data reduction packages (when available) and KOA-created reduction scripts. The automation of publicly available data reduction packages has the benefit of providing a good quality product without the additional time and expense of creating a new reduction package, and is easily applied to bulk processing needs. The downside is that the pipeline is not always able to create an ideal product, particularly for spectra, because the processing options for one type of target (eg., point sources) may not be appropriate for other types of targets (eg., extended galaxies and nebulae). In this poster we present the design and implementation for the current pipelines used at KOA and discuss our strategies for handling data for which the nature of the targets and the observers' scientific goals and data taking procedures are unknown. We also discuss our plans for implementing automated pipelines for the remaining six instruments.

  2. Advanced Instrumentation for Ultrafast Science at the LCLS

    Energy Technology Data Exchange (ETDEWEB)

    Berrah, Nora [Univ. of Connecticut, Storrs, CT (United States)

    2015-10-13

    This grant supported a Single Investigator and Small Group Research (SISGR) application to enable multi-user research in Ultrafast Science using the Linac Coherent Light Source (LCLS), the world’s first hard x-ray free electron laser (FEL) which lased for the first time at 1.5 Å on April 20, 2009. The goal of our proposal was to enable a New Era of Science by requesting funds to purchase and build Advanced Instrumentation for Ultrafast Science (AIUS), to utilize the intense, short x-ray pulses produced by the LCLS. The proposed instrumentation will allow peer review selected users to probe the ultrasmall and capture the ultrafast. These tools will expand on the investment already made in the construction of the light source and its instrumentation in both the LCLS and LUSI projects. The AIUS will provide researchers in the AMO, Chemical, Biological and Condensed Matter communities with greater flexibility in defining their scientific agenda at the LCLS. The proposed instrumentation will complement and significantly augment the present AMO instrument (funded through the LCLS project) through detectors and capabilities not included in the initial suite of instrumentation at the facility. We have built all of the instrumentations and they have been utilized by scientists. Please see report attached.

  3. Remote Instrumentation for eScience and Related Aspects

    CERN Document Server

    Lawenda, Marcin; Meyer, Norbert; Pugliese, Roberto; Węglarz, Jan; Zappatore, Sandro

    2012-01-01

    Making scientific instruments a manageable resource over distributed computing infrastructures such as the grid has been a key focal point of e-science research in recent years. It is now known by the generic term ‘remote instrumentation’, and is the subject of this useful volume that covers a range of perspectives on the topic reflected by the contributions to the 2010 workshop on remote instrumentation held in Poznań, Poland. E-science itself is a complex set of disciplines requiring computationally intensive distributed operations, high-speed networking, and collaborative working tools. As such, it is most often (and correctly) associated with grid- and cloud-computing infrastructures and middleware. The contributions to this publication consider broader aspects of the theme of remote instrumentation applied to e-science, as well as exploring related technologies that enable the implementation of truly distributed and coordinated laboratories. Among the topics discussed are remote instrumentation and ...

  4. Investigating Near Space Interaction Regions: Developing a Remote Observatory

    Science.gov (United States)

    Gallant, M.; Mierkiewicz, E. J.; Oliversen, R. J.; Jaehnig, K.; Percival, J.; Harlander, J.; Englert, C. R.; Kallio, R.; Roesler, F. L.; Nossal, S. M.; Gardner, D.; Rosborough, S.

    2016-12-01

    The Investigating Near Space Interaction Regions (INSpIRe) effort will (1) establish an adaptable research station capable of contributing to terrestrial and planetary aeronomy; (2) integrate two state-of-the-art second generation Fabry-Perot (FP) and Spatial Heteorodyne Spectrometers (SHS) into a remotely operable configuration; (3) deploy this instrumentation to a clear-air site, establishing a stable, well-calibrated observatory; (4) embark on a series of observations designed to contribute to three major areas of geocoronal research: geocoronal physics, structure/coupling, and variability. This poster describes the development of the INSpIRe remote observatory. Based at Embry-Riddle Aeronautical University (ERAU), initiative INSpIRe provides a platform to encourage the next generation of researchers to apply knowledge gained in the classroom to real-world science and engineering. Students at ERAU contribute to the INSpIRe effort's hardware and software needs. Mechanical/optical systems are in design to bring light to any of four instruments. Control software is in development to allow remote users to control everything from dome and optical system operations to calibration and data collection. In April 2016, we also installed and tested our first science instrument in the INSpIRe trailer, the Redline DASH Demonstration Instrument (REDDI). REDDI uses Doppler Asymmetric Spatial Heterodyne (DASH) spectroscopy, and its deployment as part of INSpIRe is a collaborative research effort between the Naval Research Lab, St Cloud State University, and ERAU. Similar to a stepped Michelson device, REDDI measures oxygen (630.0 nm) winds from the thermosphere. REDDI is currently mounted in a temporary location under INSpIRe's main siderostat until its entrance optical system can be modified. First light tests produced good signal-to-noise fringes in ten minute integrations, indicating that we will soon be able to measure thermospheric winds from our Daytona Beach testing site

  5. SIRTA, a ground-based atmospheric observatory for cloud and aerosol research

    Directory of Open Access Journals (Sweden)

    M. Haeffelin

    2005-02-01

    Full Text Available Ground-based remote sensing observatories have a crucial role to play in providing data to improve our understanding of atmospheric processes, to test the performance of atmospheric models, and to develop new methods for future space-borne observations. Institut Pierre Simon Laplace, a French research institute in environmental sciences, created the Site Instrumental de Recherche par Télédétection Atmosphérique (SIRTA, an atmospheric observatory with these goals in mind. Today SIRTA, located 20km south of Paris, operates a suite a state-of-the-art active and passive remote sensing instruments dedicated to routine monitoring of cloud and aerosol properties, and key atmospheric parameters. Detailed description of the state of the atmospheric column is progressively archived and made accessible to the scientific community. This paper describes the SIRTA infrastructure and database, and provides an overview of the scientific research associated with the observatory. Researchers using SIRTA data conduct research on atmospheric processes involving complex interactions between clouds, aerosols and radiative and dynamic processes in the atmospheric column. Atmospheric modellers working with SIRTA observations develop new methods to test their models and innovative analyses to improve parametric representations of sub-grid processes that must be accounted for in the model. SIRTA provides the means to develop data interpretation tools for future active remote sensing missions in space (e.g. CloudSat and CALIPSO. SIRTA observation and research activities take place in networks of atmospheric observatories that allow scientists to access consistent data sets from diverse regions on the globe.

  6. Using and Developing Measurement Instruments in Science Education: A Rasch Modeling Approach. Science & Engineering Education Sources

    Science.gov (United States)

    Liu, Xiufeng

    2010-01-01

    This book meets a demand in the science education community for a comprehensive and introductory measurement book in science education. It describes measurement instruments reported in refereed science education research journals, and introduces the Rasch modeling approach to developing measurement instruments in common science assessment domains,…

  7. Developing the Planetary Science Virtual Observatory

    Science.gov (United States)

    Erard, Stéphane; Cecconi, Baptiste; Le Sidaner, Pierre; Henry, Florence; Chauvin, Cyril; Berthier, Jérôme; André, Nicolas; Génot, Vincent; Schmitt, Bernard; Capria, Teresa; Chanteur, Gérard

    2015-08-01

    In the frame of the Europlanet-RI program, a prototype Virtual Observatory dedicated to Planetary Science has been set up. Most of the activity was dedicated to the definition of standards to handle data in this field. The aim was to facilitate searches in big archives as well as sparse databases, to make on-line data access and visualization possible, and to allow small data providers to make their data available in an interoperable environment with minimum effort. This system makes intensive use of studies and developments led in Astronomy (IVOA), Solar Science (HELIO), and space archive services (IPDA).The current architecture connects existing data services with IVOA or IPDA protocols whenever relevant. However, a more general standard has been devised to handle the specific complexity of Planetary Science, e.g. in terms of measurement types and coordinate frames. This protocol, named EPN-TAP, is based on TAP and includes precise requirements to describe the contents of a data service (Erard et al Astron & Comp 2014). A light framework (DaCHS/GAVO) and a procedure have been identified to install small data services, and several hands-on sessions have been organized already. The data services are declared in standard IVOA registries. Support to new data services in Europe will be provided during the proposed Europlanet H2020 program, with a focus on planetary mission support (Rosetta, Cassini…).A specific client (VESPA) has been developed at VO-Paris (http://vespa.obspm.fr). It is able to use all the mandatory parameters in EPN-TAP, plus extra parameters from individual services. A resolver for target names is also available. Selected data can be sent to VO visualization tools such as TOPCAT or Aladin though the SAMP protocol.Future steps will include the development of a connection between the VO world and GIS tools, and integration of heliophysics, planetary plasma and reference spectroscopic data.The EuroPlaNet-RI project was funded by the European

  8. The Rare Book Collection of Capodimonte Astronomical Observatory Will be on the Web: Ancient Science Available to Everyone

    Science.gov (United States)

    Cirella, E. O.; Caprio, G.

    2015-04-01

    This paper describes a project for the preservation, promotion, and creation of a website for the rare book collection of Capodimonte Astronomical Observatory. The project, promoted by INAF—Capodimonte Astronomical Observatory, was supported by the Campania Region through European funds. The final component of the project was the publication of a bibliographical catalog, Le Cinquecentine dell'Osservatorio Astronomico di Capodimonte, which was addressed to specialized users, including historians of science and bibliophiles.

  9. The Russian-Ukrainian Observatories Network for the European Astronomical Observatory Route Project

    Science.gov (United States)

    Andrievsky, S. M.; Bondar, N. I.; Karetnikov, V. G.; Kazantseva, L. V.; Nefedyev, Y. A.; Pinigin, G. I.; Pozhalova, Zh. A.; Rostopchina-Shakhovskay, A. N.; Stepanov, A. V.; Tolbin, S. V.

    2011-09-01

    In 2004,the Center of UNESCO World Heritage has announced a new initiative "Astronomy & World Heritage" directed for search and preserving of objects,referred to astronomy,its history in a global value,historical and cultural properties. There were defined a strategy of thematic programme "Initiative" and general criteria for selecting of ancient astronomical objects and observatories. In particular, properties that are situated or have significance in relation to celestial objects or astronomical events; representations of sky and/or celestial bodies and astronomical events; observatories and instruments; properties closely connected with the history of astronomy. In 2005-2006,in accordance with the program "Initiative", information about outstanding properties connected with astronomy have been collected.In Ukraine such work was organized by astronomical expert group in Nikolaev Astronomical Observatory. In 2007, Nikolaev observatory was included to the Tentative List of UNESCO under # 5116. Later, in 2008, the network of four astronomical observatories of Ukraine in Kiev,Crimea, Nikolaev and Odessa,considering their high authenticities and integrities,was included to the Tentative List of UNESCO under # 5267 "Astronomical Observatories of Ukraine". In 2008-2009, a new project "Thematic Study" was opened as a successor of "Initiative". It includes all fields of astronomical heritage from earlier prehistory to the Space astronomy (14 themes in total). We present the Ukraine-Russian Observatories network for the "European astronomical observatory Route project". From Russia two observatories are presented: Kazan Observatory and Pulkovo Observatory in the theme "Astronomy from the Renaissance to the mid-twentieth century".The description of astronomical observatories of Ukraine is given in accordance with the project "Thematic study"; the theme "Astronomy from the Renaissance to the mid-twentieth century" - astronomical observatories in Kiev,Nikolaev and Odessa; the

  10. Griffith Observatory: Hollywood's Celestial Theater

    Science.gov (United States)

    Margolis, Emily A.; Dr. Stuart W. Leslie

    2018-01-01

    The Griffith Observatory, perched atop the Hollywood Hills, is perhaps the most recognizable observatory in the world. Since opening in 1935, this Los Angeles icon has brought millions of visitors closer to the heavens. Through an analysis of planning documentation, internal newsletters, media coverage, programming and exhibition design, I demonstrate how the Observatory’s Southern California location shaped its form and function. The astronomical community at nearby Mt. Wilson Observatory and Caltech informed the selection of instrumentation and programming, especially for presentations with the Observatory’s Zeiss Planetarium, the second installed in the United States. Meanwhile the Observatory staff called upon some of Hollywood’s best artists, model makers, and scriptwriters to translate the latest astronomical discoveries into spectacular audiovisual experiences, which were enhanced with Space Age technological displays on loan from Southern California’s aerospace companies. The influences of these three communities- professional astronomy, entertainment, and aerospace- persist today and continue to make Griffith Observatory one of the premiere sites of public astronomy in the country.

  11. Education in Science Centers: Evaluating School Visits to an Astronomical Observatory in Brazil

    Directory of Open Access Journals (Sweden)

    Pedro Donizete Colombo Junior

    2009-03-01

    Full Text Available The present article analyzes the activity “Guided Visit of School Groups” carried out at Astronomical Observatory of the Center for Scientific and Cultural Diffusion (CDCC of University of Sao Paulo (USP with K4 and K5 pupils. The objectives of this research were to identify influences of such activity on learning of astronomical concepts and on pupils’ motivation. The results demonstrate that pupils have difficulties to understand Solar System concepts and the distances involved, on the other hand, the activity motivates the pupils to return with their parents and friends to the Observatory. At last, the success of visits to science centers aiming at the learning of basic concepts and motivation comprises at least three moments: the one that precedes the visit, the visit itself and the return to the classroom.

  12. High-Energy Astrophysics with the High Altitude Water Cherenkov (HAWC) Observatory

    Science.gov (United States)

    Pretz, John; HAWC Collaboration

    2013-04-01

    The High Altitude Water Cherenkov (HAWC) observatory, under construction at Sierra Negra in the state of Puebla, Mexico, consists of a 22500 square meter area of water Cherenkov detectors: water tanks instrumented with light-sensitive photomultiplier tubes. The experiment is used to detect energetic secondary particles reaching the ground when a 50 GeV to 100 TeV cosmic ray or gamma ray interacts in the atmosphere above the experiment. By timing the arrival of particles on the ground, the direction of the original primary particle may be resolved with an error of between 1.0 (50 GeV) and 0.1 (10 TeV) degrees. Gamma-ray primaries may be distinguished from cosmic ray background by identifying the penetrating particles characteristic of a hadronic particle shower. The instrument is 10% complete and is performing as expected, with 30% of the channels anticipated by the summer of 2013. HAWC will complement existing Imaging Atmospheric Cherenkov Telescopes and space-based gamma-ray telescopes with its extreme high-energy sensitivity and its large field-of-view. The observatory will be used to study particle acceleration in Pulsar Wind Nebulae, Supernova Remnants, Active Galactic Nuclei and Gamma-ray Bursts. Additionally, the instrument can be used to probe dark matter annihilation in halo and sub-halos of the galaxy. We will present the sensitivity of the HAWC instrument in the context of the main science objectives. We will also present the status of the deployment including first data from the instrument and prospects for the future.

  13. Design and validation of a standards-based science teacher efficacy instrument

    Science.gov (United States)

    Kerr, Patricia Reda

    National standards for K--12 science education address all aspects of science education, with their main emphasis on curriculum---both science subject matter and the process involved in doing science. Standards for science teacher education programs have been developing along a parallel plane, as is self-efficacy research involving classroom teachers. Generally, studies about efficacy have been dichotomous---basing the theoretical underpinnings on the work of either Rotter's Locus of Control theory or on Bandura's explanations of efficacy beliefs and outcome expectancy. This study brings all three threads together---K--12 science standards, teacher education standards, and efficacy beliefs---in an instrument designed to measure science teacher efficacy with items based on identified critical attributes of standards-based science teaching and learning. Based on Bandura's explanation of efficacy being task-specific and having outcome expectancy, a developmental, systematic progression from standards-based strategies and activities to tasks to critical attributes was used to craft items for a standards-based science teacher efficacy instrument. Demographic questions related to school characteristics, teacher characteristics, preservice background, science teaching experience, and post-certification professional development were included in the instrument. The instrument was completed by 102 middle level science teachers, with complete data for 87 teachers. A principal components analysis of the science teachers' responses to the instrument resulted in two components: Standards-Based Science Teacher Efficacy: Beliefs About Teaching (BAT, reliability = .92) and Standards-Based Science Teacher Efficacy: Beliefs About Student Achievement (BASA, reliability = .82). Variables that were characteristic of professional development activities, science content preparation, and school environment were identified as members of the sets of variables predicting the BAT and BASA

  14. Proceedings of the XIIIth IAGA Workshop on Geomagnetic Observatory Instruments, Data Acquisition, and Processing

    Science.gov (United States)

    Love, Jeffrey J.

    2009-01-01

    The thirteenth biennial International Association of Geomagnetism and Aeronomy (IAGA) Workshop on Geomagnetic Observatory Instruments, Data Acquisition and Processing was held in the United States for the first time on June 9-18, 2008. Hosted by the U.S. Geological Survey's (USGS) Geomagnetism Program, the workshop's measurement session was held at the Boulder Observatory and the scientific session was held on the campus of the Colorado School of Mines in Golden, Colorado. More than 100 participants came from 36 countries and 6 continents. Preparation for the workshop began when the USGS Geomagnetism Program agreed, at the close of the twelfth workshop in Belsk Poland in 2006, to host the next workshop. Working under the leadership of Alan Berarducci, who served as the chairman of the local organizing committee, and Tim White, who served as co-chairman, preparations began in 2007. The Boulder Observatory was extensively renovated and additional observation piers were installed. Meeting space on the Colorado School of Mines campus was arranged, and considerable planning was devoted to managing the many large and small issues that accompany an international meeting. Without the devoted efforts of both Alan and Tim, other Geomagnetism Program staff, and our partners at the Colorado School of Mines, the workshop simply would not have occurred. We express our thanks to Jill McCarthy, the USGS Central Region Geologic Hazards Team Chief Scientist; Carol A. Finn, the Group Leader of the USGS Geomagnetism Program; the USGS International Office; and Melody Francisco of the Office of Special Programs and Continuing Education of the Colorado School of Mines. We also thank the student employees that the Geomagnetism Program has had over the years and leading up to the time of the workshop. For preparation of the proceedings, thanks go to Eddie and Tim. And, finally, we thank our sponsors, the USGS, IAGA, and the Colorado School of Mines.

  15. Development of an instrument to measure student attitudes toward science fairs

    Science.gov (United States)

    Huddleston, Claudia A.

    Science fairs are woven into the very fabric of science instruction in the United States and in other countries. Even though thousands of students participate in science fairs every year, no instrument to measure student attitudes toward partaking in this hands-on learning experience has been fully developed and available for school administrators and teachers to assess the perceived value that current students attribute to participation in science fairs. Therefore, the purpose of this study was to continue the development and refinement of an instrument that measured student attitudes towards science fairs based on an unpublished instrument created by Michael (2005). The instrument developed and tested using 110 students at two different middle schools in southwest Virginia. The instrument consisted of 45 questions. After applying a principal component factor analysis, the instrument was reduced to two domains, enjoyment and value. The internal consistency of the instrument was calculated using Cronbach's alpha and showed good internal consistency of .89 between the two domains. Further analysis was conducted using a Pearson product-moment test and showed a significant positive correlation between enjoyment and value (r = .78). Demographic information was explored concerning the domains using a series of statistical tests, and results revealed no significant differences among race and science fair category. However, a significant difference was found among gender and students who won awards and those who did not. The conclusion was that further development and refinement of the instrument should be conducted.

  16. High Resolution, Non-Dispersive X-Ray Calorimeter Spectrometers on EBITs and Orbiting Observatories

    Science.gov (United States)

    Porter, Frederick S.

    2010-01-01

    X-ray spectroscopy is the primary tool for performing atomic physics with Electron beam ion trap (EBITs). X-ray instruments have generally fallen into two general categories, 1) dispersive instruments with very high spectral resolving powers but limited spectral range, limited count rates, and require an entrance slit, generally, for EBITs, defined by the electron beam itself, and 2) non-dispersive solid-state detectors with much lower spectral resolving powers but that have a broad dynamic range, high count rate ability and do not require a slit. Both of these approaches have compromises that limit the type and efficiency of measurements that can be performed. In 1984 NASA initiated a program to produce a non-dispersive instrument with high spectral resolving power for x-ray astrophysics based on the cryogenic x-ray calorimeter. This program produced the XRS non-dispersive spectrometers on the Astro-E, Astro-E2 (Suzaku) orbiting observatories, the SXS instrument on the Astro-H observatory, and the planned XMS instrument on the International X-ray Observatory. Complimenting these spaceflight programs, a permanent high-resolution x-ray calorimeter spectrometer, the XRS/EBIT, was installed on the LLNL EBIT in 2000. This unique instrument was upgraded to a spectral resolving power of 1000 at 6 keV in 2003 and replaced by a nearly autonomous production-class spectrometer, the EBIT Calorimeter Spectrometer (ECS), in 2007. The ECS spectrometer has a simultaneous bandpass from 0.07 to over 100 keV with a spectral resolving power of 1300 at 6 keV with unit quantum efficiency, and 1900 at 60 keV with a quantum efficiency of 30%. X-ray calorimeters are event based, single photon spectrometers with event time tagging to better than 10 us. We are currently developing a follow-on instrument based on a newer generation of x-ray calorimeters with a spectral resolving power of 3000 at 6 keV, and improved timing and measurement cadence. The unique capabilities of the x

  17. In Brief: Deep-sea observatory

    Science.gov (United States)

    Showstack, Randy

    2008-11-01

    The first deep-sea ocean observatory offshore of the continental United States has begun operating in the waters off central California. The remotely operated Monterey Accelerated Research System (MARS) will allow scientists to monitor the deep sea continuously. Among the first devices to be hooked up to the observatory are instruments to monitor earthquakes, videotape deep-sea animals, and study the effects of acidification on seafloor animals. ``Some day we may look back at the first packets of data streaming in from the MARS observatory as the equivalent of those first words spoken by Alexander Graham Bell: `Watson, come here, I need you!','' commented Marcia McNutt, president and CEO of the Monterey Bay Aquarium Research Institute, which coordinated construction of the observatory. For more information, see http://www.mbari.org/news/news_releases/2008/mars-live/mars-live.html.

  18. Status of the JWST Integrated Science Instrument Module

    Science.gov (United States)

    Greenhouse, Matthew A.; Dunn, Jamie; Kimble, Randy A.; Lambros, Scott; Lundquist, Ray; Rauscher, Bernard J.; Van Campen, Julie

    2015-01-01

    The James Webb Space Telescope (JWST) Integrated Science Instrument Module (ISIM) is the science instrument payload of the JWST. It is one of three system elements that comprise the JWST space vehicle. It consists of four science sensors, a fine guidance sensor, and nine other subsystems that support them. At 1.4 metric tons, it comprises approximately 20% of the JWST mass. The ISIM is currently at 100% integration and has completed 2 of 3 planned element-level space simulation tests. The ISIM is on schedule to be delivered for integration with the Optical Telescope Element during 2015. In this poster, we present an overview of the ISIM and its status.

  19. "A bare outpost of learned European culture on the edge of the jungles of Java": Johan Maurits Mohr (1716-1775) and the emergence of instrumental and institutional science in Dutch colonial Indonesia.

    Science.gov (United States)

    Zuidervaart, Huib J; Van Gent, Rob H

    2004-03-01

    The transits of Venus in 1761 and 1769 appear to mark the starting point of instrumental science in the Dutch East Indies (now Indonesia). This essay examines the conditions that triggered and constituted instrumental and institutional science on Indonesian soil in the late eighteenth century. In 1765 the Reverend J. M. Mohr, whose wife had received a large inheritance, undertook to build a fully equipped private observatory in Batavia (now Jakarta). There he made several major astronomical and meteorological observations. Mohr's initiative inspired other Europeans living on Java around 1770 to start a scientific movement. Because of the lack of governmental and other support, it was not until 1778 that this offspring of the Dutch-Indonesian Enlightenment became a reality. The Bataviaasch Genootschap van Kunsten en Wetenschappen tried from the beginning to put into effect the program Mohr had outlined. The members even bought his instruments from his widow, intending to continue his measurements. For a number of reasons, however, this instrumental program was more than the society could support. Around 1790 instrumental science in the former Dutch East Indies came to a standstill, not to be resumed for several decades.

  20. Virtual Fieldwork and Critical Zone Observatories as Vehicles for Teaching "Three Dimensional" (NGSS) Science

    Science.gov (United States)

    Duggan-Haas, D.; Ross, R. M.; Derry, L. A.; White, T.

    2014-12-01

    The Next Generation Science Standards (NGSS) offers a vision for K-12 science education that has important differences from common and long-standing classroom practice in many ways. NGSS's three dimensions (Scientific and Engineering Practices, Crosscutting Concepts, and Disciplinary Core Ideas), coupled with the recognition that it takes years to develop deep understandings of big ideas, do not mesh well with common K-12 (or K-16) teaching practices. NGSS also infuses systems and complexity into the K-12 curriculum. The Critical Zone lies between the bottom of the groundwater and the tops of the trees -- the layer of the Earth system where most life resides. Critical Zone Observatories (CZOs) are NSF-funded observatories in markedly varied ecosystems throughout the US, where interdisciplinary teams study the interplay of geological, biological, physical, and chemical sciences. The work being done in CZOs is three-dimensional science that is both deepening the scientific community's understandings of Earth systems and providing a cutting edge and highly relevant model for K-12 science education. Virtual Fieldwork Experiences (VFEs) are multi-media representations of actual field sites that are intended to mimic fieldwork by allowing for open-ended inquiry. The Paleontological Research Institution has developed tools and strategies to build VFEs of any site that use consistent formats, yet allow for inquiry to take multiple directions. Working together with CZO scientists, PRI staff are developing VFEs and accompanying curriculum materials for each CZO site. Ready-to-use VFEs act as models that teachers and students can use to create VFEs local to their schools. VFEs, like CZOs, facilitate use of interdisciplinary science to better understand the environment. A local VFE can be built up over time with contributions from students and teachers in middle school sciences, high school biology, Earth science, and environmental science -- classes where most curriculum

  1. The Pushchino Radio Astronomy Observatory of the P N Lebedev Physical Institute Astro Space Center: yesterday, today, and tomorrow

    International Nuclear Information System (INIS)

    Dagkesamanskii, Rustam D

    2009-01-01

    The development of Russian (formerly Soviet) radio astronomy is indissolubly linked with the P N Lebedev Physical Institute (LPI), Russian Academy of Sciences. From the late 1940s, the institute conducted most of its radio astronomy research in the Crimea, at stations or on field trips; in the late 1950s, the center of gravity of research moved to the southern Moscow region, where one of the largest radio astronomy observatories in the country and in the world was developed within less than twenty years. The observatory unique instrumentation system is briefly reviewed in a historical perspective. Key research areas and some major achievements are outlined, and the prospects of the observatory as (currently) part of the LPI Astro Space Center are examined. (conferences and symposia)

  2. The Pushchino Radio Astronomy Observatory of the P N Lebedev Physical Institute Astro Space Center: yesterday, today, and tomorrow

    Energy Technology Data Exchange (ETDEWEB)

    Dagkesamanskii, Rustam D [Pushchino Radio Astronomy Observatory, Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Pushchino, Moscow region (Russian Federation)

    2009-11-30

    The development of Russian (formerly Soviet) radio astronomy is indissolubly linked with the P N Lebedev Physical Institute (LPI), Russian Academy of Sciences. From the late 1940s, the institute conducted most of its radio astronomy research in the Crimea, at stations or on field trips; in the late 1950s, the center of gravity of research moved to the southern Moscow region, where one of the largest radio astronomy observatories in the country and in the world was developed within less than twenty years. The observatory unique instrumentation system is briefly reviewed in a historical perspective. Key research areas and some major achievements are outlined, and the prospects of the observatory as (currently) part of the LPI Astro Space Center are examined. (conferences and symposia)

  3. The Keck Cosmic Web Imager (KCWI): A Powerful New Integral Field Spectrograph for the Keck Observatory

    Science.gov (United States)

    Morrissey, Patrick; KCWI Team

    2013-01-01

    The Keck Cosmic Web Imager (KCWI) is a new facility instrument being developed for the W. M. Keck Observatory and funded for construction by the Telescope System Instrumentation Program (TSIP) of the National Science Foundation (NSF). KCWI is a bench-mounted spectrograph for the Keck II right Nasmyth focal station, providing integral field spectroscopy over a seeing-limited field up to 20"x33" in extent. Selectable Volume Phase Holographic (VPH) gratings provide high efficiency and spectral resolution in the range of 1000 to 20000. The dual-beam design of KCWI passed a Preliminary Design Review in summer 2011. The detailed design of the KCWI blue channel (350 to 700 nm) is now nearly complete, with the red channel (530 to 1050 nm) planned for a phased implementation contingent upon additional funding. KCWI builds on the experience of the Caltech team in implementing the Cosmic Web Imager (CWI), in operation since 2009 at Palomar Observatory. KCWI adds considerable flexibility to the CWI design, and will take full advantage of the excellent seeing and dark sky above Mauna Kea with a selectable nod-and-shuffle observing mode. The KCWI team is lead by Caltech (project management, design and implementation) in partnership with the University of California at Santa Cruz (camera optical and mechanical design) and the W. M. Keck Observatory (program oversight and observatory interfaces).

  4. Operating a wide-area remote observing system for the W. M. Keck Observatory

    Science.gov (United States)

    Wirth, Gregory D.; Kibrick, Robert I.; Goodrich, Robert W.; Lyke, James E.

    2008-07-01

    For over a decade, the W. M. Keck Observatory's two 10-meter telescopes have been operated remotely from its Waimea headquarters. Over the last 6 years, WMKO remote observing has expanded to allow teams at dedicated sites in California to observe either in collaboration with colleagues in Waimea or entirely from the U.S. mainland. Once an experimental effort, the Observatory's mainland observing capability is now fully operational, supported on all science instruments (except the interferometer) and regularly used by astronomers at eight mainland sites. Establishing a convenient and secure observing capability from those sites required careful planning to ensure that they are properly equipped and configured. It also entailed a significant investment in hardware and software, including both custom scripts to simplify launching the instrument interface at remote sites and automated routers employing ISDN backup lines to ensure continuation of observing during Internet outages. Observers often wait until shortly before their runs to request use of the mainland facilities. Scheduling these requests and ensuring proper system operation prior to observing requires close coordination between personnel at WMKO and the mainland sites. An established protocol for approving requests and carrying out pre-run checkout has proven useful in ensuring success. The Observatory anticipates enhancing and expanding its remote observing system. Future plans include deploying dedicated summit computers for running VNC server software, implementing a web-based tracking system for mainland-based observing requests, expanding the system to additional mainland sites, and converting to full-time VNC operation for all instruments.

  5. INSTRUMENTALISM IN SCIENCE: COMMENTS AND CRITICISMS

    African Journals Online (AJOL)

    Admin

    that guide the scientist in making his decisions or a perceived system of procedural rules. ... to science, information and theories than an ... instrumentalists try to provide the foundation of ..... instrumentalism, which are practical rather than.

  6. Recycled material-based science instruments to support science education in rural area at Central Sulawesi District of Indonesia

    Science.gov (United States)

    Ali, M.; Supriyatman; Saehana, S.

    2018-03-01

    It has been successfully designing low cost of science experiment from recycled materials. The science instruments were produced to explain expansion concept and hydrostatic pressure inside the liquid. Science instruments were calibrated and then validated. It was also implemented in science learning.

  7. New Developments At The Science Archives Of The NASA Exoplanet Science Institute

    Science.gov (United States)

    Berriman, G. Bruce

    2018-06-01

    The NASA Exoplanet Science Institute (NExScI) at Caltech/IPAC is the science center for NASA's Exoplanet Exploration Program and as such, NExScI operates three scientific archives: the NASA Exoplanet Archive (NEA) and Exoplanet Follow-up Observation Program Website (ExoFOP), and the Keck Observatory Archive (KOA).The NASA Exoplanet Archive supports research and mission planning by the exoplanet community by operating a service that provides confirmed and candidate planets, numerous project and contributed data sets and integrated analysis tools. The ExoFOP provides an environment for exoplanet observers to share and exchange data, observing notes, and information regarding the Kepler, K2, and TESS candidates. KOA serves all raw science and calibration observations acquired by all active and decommissioned instruments at the W. M. Keck Observatory, as well as reduced data sets contributed by Keck observers.In the coming years, the NExScI archives will support a series of major endeavours allowing flexible, interactive analysis of the data available at the archives. These endeavours exploit a common infrastructure based upon modern interfaces such as JuypterLab and Python. The first service will enable reduction and analysis of precision radial velocity data from the HIRES Keck instrument. The Exoplanet Archive is developing a JuypterLab environment based on the HIRES PRV interactive environment. Additionally, KOA is supporting an Observatory initiative to develop modern, Python based pipelines, and as part of this work, it has delivered a NIRSPEC reduction pipeline. The ensemble of pipelines will be accessible through the same environments.

  8. The Advanced X-ray Spectroscopy and Imaging Observatory (AXSIO)

    Science.gov (United States)

    White, Nicholas E.; Bookbinder, Jay; Petre, Robert; Smith, Randall; Ptak, Andrew; Tananbaum, Harvey; Garcia, Michael

    2012-01-01

    Following recommendations from the 2010 "New Worlds, New Horizons" (NWNH) report, the Advanced X-ray Spectroscopy and Imaging Observatory (AXSIO) concept streamlines the International X-ray Observatory (IXO) mission to concentrate on the science objectives that are enabled by high-resolution spectroscopic capabilities. AXSIO will trace orbits close to the event horizon of black holes, measure black hole spin for tens of supermassive black holes (SMBH), use spectroscopy to characterize outflows and the environment of AGN during their peak activity, observe 5MBH out to redshift z=6, map bulk motions and turbulence in galaxy clusters, find the missing baryons in the cosmic web using background quasars, and observe the process of cosmic feedback where black holes and supernovae inject energy on galactic and intergalactic scales. These measurements are enabled by a 0.9 sq m collecting area at 1.25 keV, a micro calorimeter array providing high-resolution spectroscopic imaging and a deployable high efficiency grating spectrometer. AXSIO delivers a 30-fold increase in effective area for high resolution spectroscopy. The key simplifications are guided by recommendations in the NWNH panel report include a reduction in focal length from 20m to 10m, eliminating the extendable optical bench, and a reduction in the instrument complement from six to two, avoiding a movable instrument platform. A focus on spectroscopic science allows the spatial resolution requirement to be relaxed to 10 arc sec (with a 5 arc sec goal). These simplifications decrease the total mission cost to under the $2B cost to NASA recommended by NWNH. AXSIO will be available to the entire astronomical community with observing allocations based on peer-review.

  9. Measuring primary teachers' attitudes toward teaching science: development of the dimensions of attitude toward science (DAS) instrument

    NARCIS (Netherlands)

    van Aalderen-Smeets, Sandra; Walma van der Molen, Julie Henriëtte

    2013-01-01

    In this article, we present a valid and reliable instrument which measures the attitude of in-service and pre-service primary teachers toward teaching science, called the Dimensions of Attitude Toward Science (DAS) Instrument. Attention to the attitudes of primary teachers toward teaching science is

  10. The GLAST LAT Instrument Science Operations Center

    International Nuclear Information System (INIS)

    Cameron, Robert A.; SLAC

    2007-01-01

    The Gamma-ray Large Area Space Telescope (GLAST) is scheduled for launch in late 2007. Operations support and science data processing for the Large Area Telescope (LAT) instrument on GLAST will be provided by the LAT Instrument Science Operations Center (ISOC) at the Stanford Linear Accelerator Center (SLAC). The ISOC supports GLAST mission operations in conjunction with other GLAST mission ground system elements and supports the research activities of the LAT scientific collaboration. The ISOC will be responsible for monitoring the health and safety of the LAT, preparing command loads for the LAT, maintaining embedded flight software which controls the LAT detector and data acquisition flight hardware, maintaining the operating configuration of the LAT and its calibration, and applying event reconstruction processing to down-linked LAT data to recover information about detected gamma-ray photons. The SLAC computer farm will be used to process LAT event data and generate science products, to be made available to the LAT collaboration through the ISOC and to the broader scientific community through the GLAST Science Support Center at NASA/GSFC. ISOC science operations will optimize the performance of the LAT and oversee automated science processing of LAT data to detect and monitor transient gamma-ray sources

  11. The Atsa Suborbital Observatory: An Observatory for a Commercial Suborbital Spacecraft

    Science.gov (United States)

    Vilas, F.; Sollitt, L. S.

    2012-12-01

    The advantages of astronomical observations made above Earth's atmosphere have long been understood: free access to spectral regions inaccessible from Earth (e.g., UV) or affected by the atmosphere's content (e.g., IR). Most robotic, space-based telescopes maintain large angular separation between the Sun and an observational target in order to avoid accidental damage to instruments from the Sun. For most astronomical targets, this possibility is easily avoided by waiting until objects are visible away from the Sun. For the Solar System objects inside Earth's orbit, this is never the case. Suborbital astronomical observations have over 50 years' history using NASA's sounding rockets and experimental space planes. Commercial suborbital spacecraft are largely expected to go to ~100 km altitude above Earth, providing a limited amount of time for astronomical observations. The unique scientific advantage to these observations is the ability to point close to the Sun: if a suborbital spacecraft accidentally turns too close to the Sun and fries an instrument, it is easy to land the spacecraft and repair the hardware for the next flight. Objects uniquely observed during the short observing window include inner-Earth asteroids, Mercury, Venus, and Sun-grazing comets. Both open-FOV and target-specific observations are possible. Despite many space probes to the inner Solar System, scientific questions remain. These include inner-Earth asteroid size and bulk density informing Solar System evolution studies and efforts to develop methods of mitigation against imminent impactors to Earth; chemistry and dynamics of Venus' atmosphere addressing physical phenomena such as greenhouse effect, atmospheric super-rotation and global resurfacing on Venus. With the Atsa Suborbital Observatory, we combine the strengths of both ground-based observatories and space-based observing to create a facility where a telescope is maintained and used interchangeably with both in-house facility

  12. The Footprint Database and Web Services of the Herschel Space Observatory

    Science.gov (United States)

    Dobos, László; Varga-Verebélyi, Erika; Verdugo, Eva; Teyssier, David; Exter, Katrina; Valtchanov, Ivan; Budavári, Tamás; Kiss, Csaba

    2016-10-01

    Data from the Herschel Space Observatory is freely available to the public but no uniformly processed catalogue of the observations has been published so far. To date, the Herschel Science Archive does not contain the exact sky coverage (footprint) of individual observations and supports search for measurements based on bounding circles only. Drawing on previous experience in implementing footprint databases, we built the Herschel Footprint Database and Web Services for the Herschel Space Observatory to provide efficient search capabilities for typical astronomical queries. The database was designed with the following main goals in mind: (a) provide a unified data model for meta-data of all instruments and observational modes, (b) quickly find observations covering a selected object and its neighbourhood, (c) quickly find every observation in a larger area of the sky, (d) allow for finding solar system objects crossing observation fields. As a first step, we developed a unified data model of observations of all three Herschel instruments for all pointing and instrument modes. Then, using telescope pointing information and observational meta-data, we compiled a database of footprints. As opposed to methods using pixellation of the sphere, we represent sky coverage in an exact geometric form allowing for precise area calculations. For easier handling of Herschel observation footprints with rather complex shapes, two algorithms were implemented to reduce the outline. Furthermore, a new visualisation tool to plot footprints with various spherical projections was developed. Indexing of the footprints using Hierarchical Triangular Mesh makes it possible to quickly find observations based on sky coverage, time and meta-data. The database is accessible via a web site http://herschel.vo.elte.hu and also as a set of REST web service functions, which makes it readily usable from programming environments such as Python or IDL. The web service allows downloading footprint data

  13. Astronomical publications of Melbourne Observatory

    Science.gov (United States)

    Andropoulos, Jenny Ioanna

    2014-05-01

    During the second half of the 19th century and the first half of the 20th century, four well-equipped government observatories were maintained in Australia - in Melbourne, Sydney, Adelaide and Perth. These institutions conducted astronomical observations, often in the course of providing a local time service, and they also collected and collated meteorological data. As well, some of these observatories were involved at times in geodetic surveying, geomagnetic recording, gravity measurements, seismology, tide recording and physical standards, so the term "observatory" was being used in a rather broad sense! Despite the international renown that once applied to Williamstown and Melbourne Observatories, relatively little has been written by modern-day scholars about astronomical activities at these observatories. This research is intended to rectify this situation to some extent by gathering, cataloguing and analysing the published astronomical output of the two Observatories to see what contributions they made to science and society. It also compares their contributions with those of Sydney, Adelaide and Perth Observatories. Overall, Williamstown and Melbourne Observatories produced a prodigious amount of material on astronomy in scientific and technical journals, in reports and in newspapers. The other observatories more or less did likewise, so no observatory of those studied markedly outperformed the others in the long term, especially when account is taken of their relative resourcing in staff and equipment.

  14. The PLATO Dome A site-testing observatory: Power generation and control systems

    Science.gov (United States)

    Lawrence, J. S.; Ashley, M. C. B.; Hengst, S.; Luong-van, D. M.; Storey, J. W. V.; Yang, H.; Zhou, X.; Zhu, Z.

    2009-06-01

    The atmospheric conditions above Dome A, a currently unmanned location at the highest point on the Antarctic plateau, are uniquely suited to astronomy. For certain types of astronomy Dome A is likely to be the best location on the planet, and this has motivated the development of the Plateau Observatory (PLATO). PLATO was deployed to Dome A in early 2008. It houses a suite of purpose-built site-testing instruments designed to quantify the benefits of Dome A site for astronomy, and science instruments designed to take advantage of the observing conditions. The PLATO power generation and control system is designed to provide continuous power and heat, and a high-reliability command and communications platform for these instruments. PLATO has run and collected data throughout the winter 2008 season completely unattended. Here we present a detailed description of the power generation, power control, thermal management, instrument interface, and communications systems for PLATO, and an overview of the system performance for 2008.

  15. Measuring Primary Teachers' Attitudes toward Teaching Science: Development of the Dimensions of Attitude toward Science (DAS) Instrument

    Science.gov (United States)

    van Aalderen-Smeets, Sandra; Walma van der Molen, Juliette

    2013-01-01

    In this article, we present a valid and reliable instrument which measures the attitude of in-service and pre-service primary teachers toward teaching science, called the Dimensions of Attitude Toward Science (DAS) Instrument. Attention to the attitudes of primary teachers toward teaching science is of fundamental importance to the…

  16. A case study in adaptable and reusable infrastructure at the Keck Observatory Archive: VO interfaces, moving targets, and more

    Science.gov (United States)

    Berriman, G. Bruce; Cohen, Richard W.; Colson, Andrew; Gelino, Christopher R.; Good, John C.; Kong, Mihseh; Laity, Anastasia C.; Mader, Jeffrey A.; Swain, Melanie A.; Tran, Hien D.; Wang, Shin-Ywan

    2016-08-01

    The Keck Observatory Archive (KOA) (https://koa.ipac.caltech.edu) curates all observations acquired at the W. M. Keck Observatory (WMKO) since it began operations in 1994, including data from eight active instruments and two decommissioned instruments. The archive is a collaboration between WMKO and the NASA Exoplanet Science Institute (NExScI). Since its inception in 2004, the science information system used at KOA has adopted an architectural approach that emphasizes software re-use and adaptability. This paper describes how KOA is currently leveraging and extending open source software components to develop new services and to support delivery of a complete set of instrument metadata, which will enable more sophisticated and extensive queries than currently possible. In August 2015, KOA deployed a program interface to discover public data from all instruments equipped with an imaging mode. The interface complies with version 2 of the Simple Imaging Access Protocol (SIAP), under development by the International Virtual Observatory Alliance (IVOA), which defines a standard mechanism for discovering images through spatial queries. The heart of the KOA service is an R-tree-based, database-indexing mechanism prototyped by the Virtual Astronomical Observatory (VAO) and further developed by the Montage Image Mosaic project, designed to provide fast access to large imaging data sets as a first step in creating wide-area image mosaics (such as mosaics of subsets of the 4.7 million images of the SDSS DR9 release). The KOA service uses the results of the spatial R-tree search to create an SQLite data database for further relational filtering. The service uses a JSON configuration file to describe the association between instrument parameters and the service query parameters, and to make it applicable beyond the Keck instruments. The images generated at the Keck telescope usually do not encode the image footprints as WCS fields in the FITS file headers. Because SIAP

  17. Las Cumbres Observatory 1-Meter Global Science Telescope Network

    Science.gov (United States)

    Pickles, Andrew; Dubberley, M.; Haldeman, B.; Haynes, R.; Posner, V.; Rosing, W.; staff, LCOGT

    2009-05-01

    We present the optical, mechanical and electronic design of the LCOGT 1-m telescope. These telescopes are planned to go in pairs to each of 6 sites worldwide, complementing 0.4m telescopes and 2-m telescopes at two existing sites. This science network is designed to provide continuously available photometric monitoring and spectroscopy of variable sources. The 1-m optical design is an f/8 quasi-RC system, with a doublet corrector and field flattener to provide good image quality out to 0.8 degrees. The field of view of the Fairchild 4K science CCD is 27 arcmin, with 0.39 arcsec pixels. The mechanical design includes a stiff C-ring equatorial mount and friction drive rollers, mounted on a triangular base that can be adjusted for latitude. Another friction drive is coupled at the Declination axis to the M1 mirror cell, that forms the main Optical Tube Assembly (OTA) structural element. The OTA design includes a stiff carbon fiber truss assembly, with offset vanes to an M2 drive that provides remote focus, tilt and collimation. The tube assembly weighs about 600 Kg, including Hextek mirrors, 4K science CCD, filter wheel, autoguiders and medium resolution spectrograph pick-off fiber. The telescopes will be housed in domes at existing observatory sites. They are designed to operate remotely and reliably under centralized control for automatic, optimized scheduling of observations with available hardware.

  18. Deep Space Climate Observatory (DSCOVR)

    Data.gov (United States)

    National Oceanic and Atmospheric Administration, Department of Commerce — The Deep Space Climate ObserVatoRy (DSCOVR) satellite is a NOAA operated asset at the first Lagrange (L1) point. The primary space weather instrument is the PlasMag...

  19. Norwegian Ocean Observatory Network (NOON)

    Science.gov (United States)

    Ferré, Bénédicte; Mienert, Jürgen; Winther, Svein; Hageberg, Anne; Rune Godoe, Olav; Partners, Noon

    2010-05-01

    The Norwegian Ocean Observatory Network (NOON) is led by the University of Tromsø and collaborates with the Universities of Oslo and Bergen, UniResearch, Institute of Marine Research, Christian Michelsen Research and SINTEF. It is supported by the Research Council of Norway and oil and gas (O&G) industries like Statoil to develop science, technology and new educational programs. Main topics relate to ocean climate and environment as well as marine resources offshore Norway from the northern North Atlantic to the Arctic Ocean. NOON's vision is to bring Norway to the international forefront in using cable based ocean observatory technology for marine science and management, by establishing an infrastructure that enables real-time and long term monitoring of processes and interactions between hydrosphere, geosphere and biosphere. This activity is in concert with the EU funded European Strategy Forum on Research Infrastructures (ESFRI) roadmap and European Multidisciplinary Seafloor Observation (EMSO) project to attract international leading research developments. NOON envisions developing towards a European Research Infrastructure Consortium (ERIC). Beside, the research community in Norway already possesses a considerable marine infrastructure that can expand towards an international focus for real-time multidisciplinary observations in times of rapid climate change. PIC The presently established cable-based fjord observatory, followed by the establishment of a cable-based ocean observatory network towards the Arctic from an O&G installation, will provide invaluable knowledge and experience necessary to make a successful larger cable-based observatory network at the Norwegian and Arctic margin (figure 1). Access to large quantities of real-time observation from the deep sea, including high definition video, could be used to provide the public and future recruits to science a fascinating insight into an almost unexplored part of the Earth beyond the Arctic Circle

  20. New Platforms for Suborbital Astronomical Observations and In Situ Atmospheric Measurements: Spacecraft, Instruments, and Facilities

    Science.gov (United States)

    Rodway, K.; DeForest, C. E.; Diller, J.; Vilas, F.; Sollitt, L. S.; Reyes, M. F.; Filo, A. S.; Anderson, E.

    2014-12-01

    Suborbital astronomical observations have over 50 years' history using NASA's sounding rockets and experimental space planes. The new commercial space industry is developing suborbital reusable launch vehicles (sRLV's) to provide low-cost, flexible, and frequent access to space at ~100 km altitude. In the case of XCOR Aerospace's Lynx spacecraft, the vehicle design and capabilities work well for hosting specially designed experiments that can be flown with a human-tended researcher or alone with the pilot on a customized mission. Some of the first-generation instruments and facilities that will conduct solar observations on dedicated Lynx science missions include the SwRI Solar Instrument Pointing Platform (SSIPP) and Atsa Suborbital Observatory, as well as KickSat sprites, which are picosatellites for in situ atmospheric and solar phenomena measurements. The SSIPP is a demonstration two-stage pointed solar observatory that operates inside the Lynx cockpit. The coarse pointing stage includes the pilot in the feedback loop, and the fine stage stabilizes the solar image to achieve arcsecond class pointing. SSIPP is a stepping-stone to future external instruments that can operate with larger apertures and shorter wavelengths in the solar atmosphere. The Planetary Science Institute's Atsa Suborbital Observatory combines the strengths of ground-based observatories and space-based observing to create a facility where a telescope is maintained and used interchangeably with either in-house facility instruments or user-provided instruments. The Atsa prototype is a proof of concept, hand-guided camera that mounts on the interior of the Lynx cockpit to test target acquisition and tracking for human-operated suborbital astronomy. KickSat sprites are mass-producible, one inch printed circuit boards (PCBs) populated by programmable off the shelf microprocessors and radios for real time data transmission. The sprite PCBs can integrate chip-based radiometers, magnetometers

  1. Morro Azul Observatory: A New Center for Teaching and Popularization of Astronomy.

    Science.gov (United States)

    Bretones, Paulo Sergio; Cardoso de Oliveira, Vladimir

    2002-08-01

    In 1999, the Instituto Superior de Ciências Aplicadas (ISCA Faculdades de Limeira) started a project to build an observatory and initiate several astronomy related activities in the city of Limeira and region (São Paulo state) with the aim of teaching and popularizing astronomy. After contracting teachers, a technician and an intern, the Morro Azul Observatory was inaugurated in March 2000 as a part of the geosciences department of ISCA Faculdades. This poster describes the development phases of the Observatory, the activities initiated by the Observatory, and assesses the impact of the project. Several issues will be discussed such as the criteria for choosing the site, buildings, instruments, group visits, and particularly the goals that were reached. The Observatory, as described here, serves as a model for other centers with the same purpose in the country. The achievements of this project include the creation of two astronomical disciplines for the geography course and liaisons with other courses such as tourism, pedagogy, social communication and engineering. New activities were initiated, educational materials created, and the Observatory is now part of the regions teaching network and is in contact with other Brazilian and foreign centers. This poster presents the results from report analyses, visitor records, the local media, goal strategy assessment, and the current state of the project. It concludes with an evaluation of the social commitment of the Observatory, its initiatives for the constant renewal and growth of the project, its policy of maintaining the activities and interchange with other national and international astronomy centers, and the future perspectives in terms of its contribution for the research in science education.

  2. Update on The Ultra-Fast Flash Observatory (UFFO) Pathfinder

    DEFF Research Database (Denmark)

    Grossan, B.; Brandt, Søren; Budtz-Jørgensen, Carl

    2011-01-01

    The Ultra-Fast Flash Observatory (UFFO) uses an X/gamma and an optical/UV instrument to observe gamma-ray bursts (GRB) starting milliseconds after burst trigger and location. The X/gamma instrument, a standard coded-mask camera, locates the GRB and triggers the system. The optical/UV instrument, ...

  3. SPASE and the Heliophysics Virtual Observatories

    Directory of Open Access Journals (Sweden)

    J R Thieman

    2010-02-01

    Full Text Available The Space Physics Archive Search and Extract (SPASE project has developed an information model for interoperable access and retrieval of data within the Heliophysics (also known as space and solar physics science community. The diversity of science data archives within this community has led to the establishment of many virtual observatories to coordinate the data pathways within Heliophysics subdisciplines, such as magnetospheres, waves, radiation belts, etc. The SPASE information model provides a semantic layer and common language for data descriptions so that searches might be made across the whole of the heliophysics data environment, especially through the virtual observatories.

  4. The Marseille Observatory 1860-1920: missed opportunities and elebrated achievements

    Science.gov (United States)

    Caplan, James

    2001-10-01

    After summarizing the early history of the Marseille Observatory (founded by the Jesuits and operational in 1702), I describe the circumstances leading to the takeover by Le Verrier in the 1860s. The observatory was rebuilt on the Plateau Longchamp and new instruments were installed, most notably the 80-cm Foucault glass-mirror telescope. The work of the new observatory is then presented, and the instruments described, starting with the Le Verrier period and continuing through the long directorship of Stephan, and then Bourget. The overall success of the observatory in its Longchamp site was due in part to the assiduous pursuit of routine observations and to the discovery of comets and asteroids, combined with the `exploratory' observations of `nebulae' by Stephan. In addition, the first stellar interferometry observations, and the first applications of the Fabry-Perot interferometer to nebular observations, were important achievements. On the other hand, the failure in the beginning of the twentieth century to adapt the telescopes to photography condemned the observatory to a long period of missed opportunities, from which it did not recover for several decades.

  5. From Soup to Nuts: How Terra has enabled the growth of NASA Earth science communication

    Science.gov (United States)

    Ward, K.; Carlowicz, M. J.; Allen, J.; Voiland, A.; Przyborski, P.

    2014-12-01

    The birth of NASA's Earth Observatory website in 1999 closely mirrored the launch of Terra and over the years its growth has paralleled that of the Earth Observing System (EOS) program. With the launch of Terra, NASA gained an extraordinary platform that not only promised new science capabilities but gave us the data and imagery for telling the stories behind the science. The Earth Observatory Group was founded to communicate these stories to the public. We will present how we have used the capabilities of all the Terra instruments over the past 15 years to expand the public's knowledge of NASA Earth science. The ever-increasing quantity and quality of Terra data, combined with technological improvements to data availability and services has allowed the Earth Observatory and, as a result, the greater science-aware media, to greatly expand the visibility of NASA data and imagery. We will offer thoughts on best practices in using these multi-faceted instruments for public communication and we will share how we have worked with Terra science teams and affiliated systems to see the potential stories in their data and the value of providing the data in a timely fashion. Terra has allowed us to tell the stories of our Earth today like never before.

  6. Reengineering observatory operations for the time domain

    Science.gov (United States)

    Seaman, Robert L.; Vestrand, W. T.; Hessman, Frederic V.

    2014-07-01

    Observatories are complex scientific and technical institutions serving diverse users and purposes. Their telescopes, instruments, software, and human resources engage in interwoven workflows over a broad range of timescales. These workflows have been tuned to be responsive to concepts of observatory operations that were applicable when various assets were commissioned, years or decades in the past. The astronomical community is entering an era of rapid change increasingly characterized by large time domain surveys, robotic telescopes and automated infrastructures, and - most significantly - of operating modes and scientific consortia that span our individual facilities, joining them into complex network entities. Observatories must adapt and numerous initiatives are in progress that focus on redesigning individual components out of the astronomical toolkit. New instrumentation is both more capable and more complex than ever, and even simple instruments may have powerful observation scripting capabilities. Remote and queue observing modes are now widespread. Data archives are becoming ubiquitous. Virtual observatory standards and protocols and astroinformatics data-mining techniques layered on these are areas of active development. Indeed, new large-aperture ground-based telescopes may be as expensive as space missions and have similarly formal project management processes and large data management requirements. This piecewise approach is not enough. Whatever challenges of funding or politics facing the national and international astronomical communities it will be more efficient - scientifically as well as in the usual figures of merit of cost, schedule, performance, and risks - to explicitly address the systems engineering of the astronomical community as a whole.

  7. Future development of the PLATO Observatory for Antarctic science

    Science.gov (United States)

    Ashley, Michael C. B.; Bonner, Colin S.; Everett, Jon R.; Lawrence, Jon S.; Luong-Van, Daniel; McDaid, Scott; McLaren, Campbell; Storey, John W. V.

    2010-07-01

    PLATO is a self-contained robotic observatory built into two 10-foot shipping containers. It has been successfully deployed at Dome A on the Antarctic plateau since January 2008, and has accumulated over 730 days of uptime at the time of writing. PLATO provides 0.5{1kW of continuous electrical power for a year from diesel engines running on Jet-A1, supplemented during the summertime with solar panels. One of the 10-foot shipping containers houses the power system and fuel, the other provides a warm environment for instruments. Two Iridium satellite modems allow 45 MB/day of data to be transferred across the internet. Future enhancements to PLATO, currently in development, include a more modular design, using lithium iron-phosphate batteries, higher power output, and a light-weight low-power version for eld deployment from a Twin Otter aircraft. Technologies used in PLATO include a CAN (Controller Area Network) bus, high-reliability PC/104 com- puters, ultracapacitors for starting the engines, and fault-tolerant redundant design.

  8. The TMT International Observatory: A quick overview of future opportunities for planetary science exploration

    Science.gov (United States)

    Dumas, Christophe; Dawson, Sandra; Otarola, Angel; Skidmore, Warren; Squires, Gordon; Travouillon, Tony; Greathouse, Thomas K.; Li, Jian-Yang; Lu, Junjun; Marchis, Frank; Meech, Karen J.; Wong, Michael H.

    2015-11-01

    The construction of the Thirty-Meter-Telescope International Observatory (TIO) is scheduled to take about eight years, with first-light currently planned for the horizon 2023/24, and start of science operations soon after. Its innovative design, the unequalled astronomical quality of its location, and the scientific capabilities that will be offered by its suite of instruments, all contribute to position TIO as a major ground-based facility of the next decade.In this talk, we will review the expected observing performances of the facility, which will combine adaptive-optics corrected wavefronts with powerful imaging and spectroscopic capabilities. TMT will enable ground-based exploration of our solar system - and planetary systems at large - at a dramatically enhanced sensitivity and spatial resolution across the visible and near-/thermal- infrared regimes. This sharpened vision, spanning the study of planetary atmospheres, ring systems, (cryo-)volcanic activity, small body populations (asteroids, comets, trans-Neptunian objects), and exoplanets, will shed new lights on the processes involved in the formation and evolution of our solar system, including the search for life outside the Earth, and will expand our understanding of the physical and chemical properties of extra-solar planets, complementing TIO's direct studies of planetary systems around other stars.TIO operations will meet a wide range of observing needs. Observing support associated with "classical" and "queue" modes will be offered (including some flavors of remote observing). The TIO schedule will integrate observing programs so as to optimize scientific outputs and take into account the stringent observing time constraints often encountered for observations of our solar system such as, for instance, the scheduling of target-of-oportunity observations, the implementation of short observing runs, or the support of long-term "key-science" programmes.Complementary information about TIO, and the

  9. Transformative ocean science through the VENUS and NEPTUNE Canada ocean observing systems

    International Nuclear Information System (INIS)

    Martin Taylor, S.

    2009-01-01

    The health of the world's oceans and their impact on global environmental and climate change make the development of cabled observing systems vital and timely as a data source and archive of unparalleled importance for new discoveries. The VENUS and NEPTUNE Canada observatories are on the forefront of a new generation of ocean science and technology. Funding of over $100M, principally from the Governments of Canada and BC, for these two observatories supports integrated ocean systems science at a regional scale enabled by new developments in powered sub-sea cable technology and in cyber-infrastructure that streams continuous real-time data to Internet-based web platforms. VENUS is a coastal observatory supporting two instrumented arrays in the Saanich Inlet, near Victoria, and in the Strait of Georgia, off Vancouver. NEPTUNE Canada is an 800 km system on the Juan de Fuca Plate off the west coast of British Columbia, which will have five instrumented nodes in operation over the next 18 months. This paper describes the development and management of these two observatories, the principal research themes, and the applications of the research to public policy, economic development, and public education and outreach. Both observatories depend on partnerships with universities, government agencies, private sector companies, and NGOs. International collaboration is central to the development of the research programs, including partnerships with initiatives in the EU, US, Japan, Taiwan and China.

  10. Astrometry and early astrophysics at Kuffner Observatory in the late 19th century

    Science.gov (United States)

    Habison, Peter

    The astronomer and mathematician Norbert Herz encouraged Moriz von Kuffner, owner of the beer brewery in Ottakring, to finance a private scientific observatory in the western parts of Vienna. In the years 1884-87 the Kuffner Observatory was built at the Gallitzinberg in Wien-Ottakring. It was an example of enlighted patronage and noted at the time for its rapid acquisition of new instruments and by increasing international recognition. It contained the largest heliometer in the world and the largest meridian circle in the Austrian-Hungarian Empire. Of the many scientists who worked here we mention Leo de Ball, Gustav Eberhard, Johannes Hartmann and we should not forget Karl Schwarzschild. Here in Vienna he published papers on celestial mechanics, measuring techniques, optics and his fundamental papers concerning photographic photometry, in particular the quantitative determination of the departure of the reciprocity law. The telescope and the associated camera with which he carried out his measurements are still in existence at the observatory. The observatory houses important astronomical instruments from the 19th century. All telescopes were made by Repsold und Söhne in Hamburg, and Steinheil in Munich. These two German companies were best renowned for quality and precision in high standard astronomical instruments. The Great Refractor (270/3500 mm) is still the third largest refractor in Austria. It was installed at the observatory in 1886 and was used together with the Schwarzschild Refractor for early astrophysical work including photography. It is this double refractor, where Schwarzschild carried out his measurements on photographic photometry. The Meridian Circle (132/1500 mm) was the largest meridian passage instrument of the Austro-Hungarian Empire. Today it is the largest meridian circle in Austria and still one of the largest in Europe. The telescope is equipped with one of the first impersonal micrometers of that time. First observations were carried

  11. The Juno Gravity Science Instrument

    Science.gov (United States)

    Asmar, Sami W.; Bolton, Scott J.; Buccino, Dustin R.; Cornish, Timothy P.; Folkner, William M.; Formaro, Roberto; Iess, Luciano; Jongeling, Andre P.; Lewis, Dorothy K.; Mittskus, Anthony P.; Mukai, Ryan; Simone, Lorenzo

    2017-11-01

    The Juno mission's primary science objectives include the investigation of Jupiter interior structure via the determination of its gravitational field. Juno will provide more accurate determination of Jupiter's gravity harmonics that will provide new constraints on interior structure models. Juno will also measure the gravitational response from tides raised on Jupiter by Galilean satellites. This is accomplished by utilizing Gravity Science instrumentation to support measurements of the Doppler shift of the Juno radio signal by NASA's Deep Space Network at two radio frequencies. The Doppler data measure the changes in the spacecraft velocity in the direction to Earth caused by the Jupiter gravity field. Doppler measurements at X-band (˜ 8 GHz) are supported by the spacecraft telecommunications subsystem for command and telemetry and are used for spacecraft navigation as well as Gravity Science. The spacecraft also includes a Ka-band (˜ 32 GHz) translator and amplifier specifically for the Gravity Science investigation contributed by the Italian Space Agency. The use of two radio frequencies allows for improved accuracy by removal of noise due to charged particles along the radio signal path.

  12. Initial Performance of the Attitude Control and Aspect Determination Subsystems on the Chandra Observatory

    Science.gov (United States)

    Cameron, R.; Aldcroft, T.; Podgorski, W. A.; Freeman, M. D.

    2000-01-01

    The aspect determination system of the Chandra X-ray Observatory plays a key role in realizing the full potential of Chandra's X-ray optics and detectors. We review the performance of the spacecraft hardware components and sub-systems, which provide information for both real time control of the attitude and attitude stability of the Chandra Observatory and also for more accurate post-facto attitude reconstruction. These flight components are comprised of the aspect camera (star tracker) and inertial reference units (gyros), plus the fiducial lights and fiducial transfer optics which provide an alignment null reference system for the science instruments and X-ray optics, together with associated thermal and structural components. Key performance measures will be presented for aspect camera focal plane data, gyro performance both during stable pointing and during maneuvers, alignment stability and mechanism repeatability.

  13. The Farid and Moussa Raphael Observatory

    International Nuclear Information System (INIS)

    Hajjar, R

    2017-01-01

    The Farid and Moussa Raphael Observatory (FMRO) at Notre Dame University Louaize (NDU) is a teaching, research, and outreach facility located at the main campus of the university. It located very close to the Lebanese coast, in an urbanized area. It features a 60-cm Planewave CDK telescope, and instruments that allow for photometric and spetroscopic studies. The observatory currently has one thinned, back-illuminated CCD camera, used as the main imager along with Johnson-Cousin and Sloan photometric filters. It also features two spectrographs, one of which is a fiber fed echelle spectrograph. These are used with a dedicated CCD. The observatory has served for student projects, and summer schools for advanced undergraduate and graduate students. It is also made available for use by the regional and international community. The control system is currently being configured for remote observations. A number of long-term research projects are also being launched at the observatory. (paper)

  14. University Observatory, Ludwig-Maximilians-Universität

    Science.gov (United States)

    Murdin, P.

    2000-11-01

    The University Observatory of Ludwig-Maximilians-Universität was founded in 1816. Astronomers who worked or graduated at the Munich Observatory include: Fraunhofer, Soldner, Lamont, Seeliger and Karl Schwarzschild. At present four professors and ten staff astronomers work here. Funding comes from the Bavarian Government, the German Science Foundation, and other German and European research progra...

  15. The World Space Observatory Ultraviolet (WSO-UV), as a bridge to future UV astronomy

    Science.gov (United States)

    Shustov, B.; Gómez de Castro, A. I.; Sachkov, M.; Vallejo, J. C.; Marcos-Arenal, P.; Kanev, E.; Savanov, I.; Shugarov, A.; Sichevskii, S.

    2018-04-01

    Ultraviolet (UV) astronomy is a vital branch of space astronomy. Many dozens of short-term UV-experiments in space, as well as long-term observatories, have brought a very important knowledge on the physics and chemistry of the Universe during the last decades. Unfortunately, no large UV-observatories are planned to be launched by most of space agencies in the coming 10-15 years. Conversely, the large UVOIR observatories of the future will appear not earlier than in 2030s. This paper briefly describes the projects that have been proposed by various groups. We conclude that the World Space Observatory-Ultraviolet (WSO-UV) will be the only 2-m class UV telescope with capabilities similar to those of the HST for the next decade. The WSO-UV has been described in detail in previous publications, and this paper updates the main characteristics of its instruments and the current state of the whole project. It also addresses the major science topics that have been included in the core program of the WSO-UV, making this core program very relevant to the current state of the UV-astronomy. Finally, we also present here the ground segment architecture that will implement this program.

  16. High-Resolution Spectroscopy at the Wyoming Infrared Observatory: Setting TESS Science on FHiRE

    Science.gov (United States)

    Jang-Condell, Hannah; Pierce, Michael J.; Pilachowski, C. A.; Kobulnicky, Henry; McLane, Jacob N.

    2018-01-01

    The Fiber High Resolution Echelle (FHiRE) spectrograph is a new instrument designed for the 2.3-m Wyoming InfraRed Observatory (WIRO). With the construction of a vacuum chamber for FHiRE to stabilize the spectrograph and a temperature-stabilized Thorium-Argon lamp for precise velocity calibration, we will be able to achieve 1 m/s RV precision, making it an ideal instrument for finding exoplanets. Details of the design of FHiRE are presented in a companion poster (Pierce et al.). The construction of this instrument is well-timed with the planned 2018 launch of NASA's Transiting Exoplanet Survey Satellite (TESS) mission. TESS will require a great deal of follow-up spectroscopy to characterize potential exoplanet host stars as well as radial velocity measurements to confirm new exoplanets. WIRO is ideally suited to acquire the long-term, high-cadence observations that will be required to make progress in this frontier area of astrophysics. We will coordinate our efforts with the TESS Follow-up Observing Program (TFOP), specifically as part of the Recon Spectroscopy and Precise Radial Velocity Work sub-groups.This work is supported by a grant from NASA EPSCOR.

  17. PANIC: A General-purpose Panoramic Near-infrared Camera for the Calar Alto Observatory

    Science.gov (United States)

    Cárdenas Vázquez, M.-C.; Dorner, B.; Huber, A.; Sánchez-Blanco, E.; Alter, M.; Rodríguez Gómez, J. F.; Bizenberger, P.; Naranjo, V.; Ibáñez Mengual, J.-M.; Panduro, J.; García Segura, A. J.; Mall, U.; Fernández, M.; Laun, W.; Ferro Rodríguez, I. M.; Helmling, J.; Terrón, V.; Meisenheimer, K.; Fried, J. W.; Mathar, R. J.; Baumeister, H.; Rohloff, R.-R.; Storz, C.; Verdes-Montenegro, L.; Bouy, H.; Ubierna, M.; Fopp, P.; Funke, B.

    2018-02-01

    PANIC7 is the new PAnoramic Near-Infrared Camera for Calar Alto and is a project jointly developed by the MPIA in Heidelberg, Germany, and the IAA in Granada, Spain, for the German-Spanish Astronomical Center at Calar Alto Observatory (CAHA; Almería, Spain). This new instrument works with the 2.2 m and 3.5 m CAHA telescopes covering a field of view of 30 × 30 arcmin and 15 × 15 arcmin, respectively, with a sampling of 4096 × 4096 pixels. It is designed for the spectral bands from Z to K S , and can also be equipped with narrowband filters. The instrument was delivered to the observatory in 2014 October and was commissioned at both telescopes between 2014 November and 2015 June. Science verification at the 2.2 m telescope was carried out during the second semester of 2015 and the instrument is now at full operation. We describe the design, assembly, integration, and verification process, the final laboratory tests and the PANIC instrument performance. We also present first-light data obtained during the commissioning and preliminary results of the scientific verification. The final optical model and the theoretical performance of the camera were updated according to the as-built data. The laboratory tests were made with a star simulator. Finally, the commissioning phase was done at both telescopes to validate the camera real performance on sky. The final laboratory test confirmed the expected camera performances, complying with the scientific requirements. The commissioning phase on sky has been accomplished.

  18. Purging sensitive science instruments with nitrogen in the STS environment

    Science.gov (United States)

    Lumsden, J. M.; Noel, M. B.

    1983-01-01

    Potential contamination of extremely sensitive science instruments during prelaunch, launch, and earth orbit operations are a major concern to the Galileo and International Solar Polar Mission (ISPM) Programs. The Galileo Program is developing a system to purify Shuttle supplied nitrogen gas for in-flight purging of seven imaging and non-imaging science instruments. Monolayers of contamination deposited on critical surfaces can degrade some instrument sensitivities as much as fifty percent. The purging system provides a reliable supply of filtered and fried nitrogen gas during these critical phases of the mission when the contamination potential is highest. The Galileo and ISPM Programs are including the system as Airborne Support Equipment (ASE).

  19. Extra Solar Planetary Imaging Coronagraph and Science Requirements for the James Webb Telescope Observatory

    Science.gov (United States)

    Clampin, Mark

    2004-01-01

    1) Extra solar planetary imaging coronagraph. Direct detection and characterization of Jovian planets, and other gas giants, in orbit around nearby stars is a necessary precursor to Terrestrial Planet Finder 0 in order to estimate the probability of Terrestrial planets in our stellar neighborhood. Ground based indirect methods are biased towards large close in Jovian planets in solar systems unlikely io harbor Earthlike planets. Thus to estimate the relative abundances of terrestrial planets and to determine optimal observing strategies for TPF a pathfinder mission would be desired. The Extra-Solar Planetary Imaging Coronagraph (EPIC) is such a pathfinder mission. Upto 83 stellar systems are accessible with a 1.5 meter unobscured telescope and coronagraph combination located at the Earth-Sun L2 point. Incorporating radiometric and angular resolution considerations show that Jovians could be directly detected (5 sigma) in the 0.5 - 1.0 micron band outside of an inner working distance of 5/D with integration times of -10 - 100 hours per observation. The primary considerations for a planet imager are optical wavefront quality due to manufacturing, alignment, structural and thermal considerations. pointing stability and control, and manufacturability of coronagraphic masks and stops to increase the planetary-to- stellar contrast and mitigate against straylight. Previously proposed coronagraphic concepts are driven to extreme tolerances. however. we have developed and studied a mission, telescope and coronagraphic detection concept, which is achievable in the time frame of a Discovery class NASA mission. 2) Science requirements for the James Webb Space Telescope observatory. The James Webb Space Observatory (JWST) is an infrared observatory, which will be launched in 201 1 to an orbit at L2. JWST is a segmented, 18 mirror segment telescope with a diameter of 6.5 meters, and a clear aperture of 25 mA2. The telescope is designed to conduct imaging and spectroscopic

  20. An Information Retrieval and Recommendation System for Astronomical Observatories

    Science.gov (United States)

    Mukund, Nikhil; Thakur, Saurabh; Abraham, Sheelu; Aniyan, A. K.; Mitra, Sanjit; Sajeeth Philip, Ninan; Vaghmare, Kaustubh; Acharjya, D. P.

    2018-03-01

    We present a machine-learning-based information retrieval system for astronomical observatories that tries to address user-defined queries related to an instrument. In the modern instrumentation scenario where heterogeneous systems and talents are simultaneously at work, the ability to supply people with the right information helps speed up the tasks for detector operation, maintenance, and upgradation. The proposed method analyzes existing documented efforts at the site to intelligently group related information to a query and to present it online to the user. The user in response can probe the suggested content and explore previously developed solutions or probable ways to address the present situation optimally. We demonstrate natural language-processing-backed knowledge rediscovery by making use of the open source logbook data from the Laser Interferometric Gravitational Observatory (LIGO). We implement and test a web application that incorporates the above idea for LIGO Livingston, LIGO Hanford, and Virgo observatories.

  1. NASA SMD Airborne Science Capabilities for Development and Testing of New Instruments

    Science.gov (United States)

    Fladeland, Matthew

    2015-01-01

    The SMD NASA Airborne Science Program operates and maintains a fleet of highly modified aircraft to support instrument development, satellite instrument calibration, data product validation and earth science process studies. This poster will provide an overview of aircraft available to NASA researchers including performance specifications and modifications for instrument support, processes for requesting aircraft time and developing cost estimates for proposals, and policies and procedures required to ensure safety of flight.

  2. Instrument Remote Control via the Astronomical Instrument Markup Language

    Science.gov (United States)

    Sall, Ken; Ames, Troy; Warsaw, Craig; Koons, Lisa; Shafer, Richard

    1998-01-01

    The Instrument Remote Control (IRC) project ongoing at NASA's Goddard Space Flight Center's (GSFC) Information Systems Center (ISC) supports NASA's mission by defining an adaptive intranet-based framework that provides robust interactive and distributed control and monitoring of remote instruments. An astronomical IRC architecture that combines the platform-independent processing capabilities of Java with the power of Extensible Markup Language (XML) to express hierarchical data in an equally platform-independent, as well as human readable manner, has been developed. This architecture is implemented using a variety of XML support tools and Application Programming Interfaces (API) written in Java. IRC will enable trusted astronomers from around the world to easily access infrared instruments (e.g., telescopes, cameras, and spectrometers) located in remote, inhospitable environments, such as the South Pole, a high Chilean mountaintop, or an airborne observatory aboard a Boeing 747. Using IRC's frameworks, an astronomer or other scientist can easily define the type of onboard instrument, control the instrument remotely, and return monitoring data all through the intranet. The Astronomical Instrument Markup Language (AIML) is the first implementation of the more general Instrument Markup Language (IML). The key aspects of our approach to instrument description and control applies to many domains, from medical instruments to machine assembly lines. The concepts behind AIML apply equally well to the description and control of instruments in general. IRC enables us to apply our techniques to several instruments, preferably from different observatories.

  3. Advance on solar instrumentation in China

    Science.gov (United States)

    Yan, Yihua

    2015-08-01

    The solar observing facilities in China are introduced with the emphasis on the development in recent years and future plans for both ground and space-based solar instrumentations. The recent solar instruments are as follows: A new generation Chinese Spectral Radioreliograph (CSRH) has been constructed at Mingantu Observing Station in Zhengxiangbaiqi, inner Mongolia of China since 2013 and is in test observations now. CSRH has two arrays with 40 × 4.5 m and 60 × 2 m parabolic antennas covering 0.4-2 GHz and 2-15 GHz frequency range. CSRH is renamed as MUSER (Mingantu Ultrawide Spectral Radiheliograph) after its accomplishment. A new 1 m vacuum solar telescope (NVST) has been installed in 2010 at Fuxian lake, 60 km away from Kunming, Yunana. At present it is the best seeing place in China. A new telescope called ONSET (Optical and NIR Solar Eruption Tracer) has been established at the same site as NVST in 2011. ONSET has been put into operation since 2013. For future ground-based plans, Chinese Giant Solar Telescope (CGST) with spatial resolution equivalent to 8m and effective area of 5m full-aperture telescope has been proposed and was formally listed into the National Plans of Major Science & Technology Infrastructures in China. The pre-study and site survey for CGST have been pursued. A 1-meter mid-infrared telescope for precise measurement of the solar magnetic field has been funded by NSFC in 2014 as a national major scientific instrument development project. This project will develop the first mid-infrared solar magnetic observation instrument in the world aiming at increasing the precision of the transverse magnetic field measurement by one order of magnitude. For future ground-based plans, we promote the Deep-space Solar Observatory (DSO) with 1-m aperture telescope to be formally funded. The ASO-S (an Advanced Space-based Solar Observatory) has been supported in background phase by Space Science Program as a small mission. Other related space solar

  4. Filling the Data Gaps in Mountain Climate Observatories Through Advanced Technology, Refined Instrument Siting, and a Focus on Gradients

    Directory of Open Access Journals (Sweden)

    Scotty Strachan

    2016-11-01

    Full Text Available The mountain research community is still contending with the need to monitor ecosystems, both to improve local management practices and to address regional and global science questions related to the Future Earth themes of Dynamic Planet, Global Sustainable Development, and Transformations Towards Sustainability. How such efforts may be designed and coordinated remains an open question. Historical climate and ecological observatories and networks typically have not represented the scope or spatial and topographic distribution of near-surface processes in mountains, creating knowledge gaps. Grassroots, in situ investigations have revealed the existence of topoclimates that are not linearly related to general atmospheric conditions, and are also not adequately represented in gridded model products. In this paper, we describe how some of the disconnects between data, models, and applications in mountains can be addressed using a combination of gradient monitoring, uniform observational siting and standards, and modern technology (cyberinfrastructure. Existing observational studies need to expand their topographic niches, and future observatories should be planned to span entire gradients. Use of cyberinfrastructure tools such as digital telemetry and Internet Protocol networks can reduce costs and data gaps while improving data quality control processes and widening audience outreach. Embracing this approach and working toward common sets of comparable measurements should be goals of emerging mountain observatories worldwide.

  5. Volcano-Monitoring Instrumentation in the United States, 2008

    Science.gov (United States)

    Guffanti, Marianne; Diefenbach, Angela K.; Ewert, John W.; Ramsey, David W.; Cervelli, Peter F.; Schilling, Steven P.

    2010-01-01

    The United States is one of the most volcanically active countries in the world. According to the global volcanism database of the Smithsonian Institution, the United States (including its Commonwealth of the Northern Mariana Islands) is home to about 170 volcanoes that are in an eruptive phase, have erupted in historical time, or have not erupted recently but are young enough (eruptions within the past 10,000 years) to be capable of reawakening. From 1980 through 2008, 30 of these volcanoes erupted, several repeatedly. Volcano monitoring in the United States is carried out by the U.S. Geological Survey (USGS) Volcano Hazards Program, which operates a system of five volcano observatories-Alaska Volcano Observatory (AVO), Cascades Volcano Observatory (CVO), Hawaiian Volcano Observatory (HVO), Long Valley Observatory (LVO), and Yellowstone Volcano Observatory (YVO). The observatories issue public alerts about conditions and hazards at U.S. volcanoes in support of the USGS mandate under P.L. 93-288 (Stafford Act) to provide timely warnings of potential volcanic disasters to the affected populace and civil authorities. To make efficient use of the Nation's scientific resources, the volcano observatories operate in partnership with universities and other governmental agencies through various formal agreements. The Consortium of U.S. Volcano Observatories (CUSVO) was established in 2001 to promote scientific cooperation among the Federal, academic, and State agencies involved in observatory operations. Other groups also contribute to volcano monitoring by sponsoring long-term installation of geophysical instruments at some volcanoes for specific research projects. This report describes a database of information about permanently installed ground-based instruments used by the U.S. volcano observatories to monitor volcanic activity (unrest and eruptions). The purposes of this Volcano-Monitoring Instrumentation Database (VMID) are to (1) document the Nation's existing

  6. Site Protection Program and Progress Report of Ali Observatory, Tibet

    Science.gov (United States)

    Yao, Yongqiang; Zhou, Yunhe; Wang, Xiaohua; He, Jun; Zhou, Shu

    2015-08-01

    The Ali observatory, Tibet, is a promising new site identified through ten year site survey over west China, and it is of significance to establish rules of site protection during site development. The site protection program is described with five aspects: site monitoring, technical support, local government support, specific organization, and public education. The long-term sky brightness monitoring is ready with site testing instruments and basic for light pollution measurement; the monitoring also includes directions of main light sources, providing periodical reports and suggestions for coordinating meetings. The technical supports with institutes and manufacturers help to publish lighting standards and replace light fixtures; the research pays special attention to the blue-rich sources, which impact the important application of high altitude sites. An official leading group towards development and protection of astronomical resources has been established by Ali government; one of its tasks is to issue regulations against light pollution, including special restrictions of airport, mine, and winter heating, and to supervise lighting inspection and rectification. A site protection office under the official group and local astronomical society are organized by Ali observatory; the office can coordinate in government levels and promote related activities. A specific website operated by the protection office releases activity propaganda, evaluation results, and technical comparison with other observatories. Both the site protection office and Ali observatory take responsibility for public education, including popular science lectures, light pollution and energy conservation education. Ali Night Sky Park has been constructed and opens in 2014, and provides a popular place and observational experience. The establishment of Ali Observatory and Night Sky Park brings unexpected social influence, and the starry sky trip to Ali becomes a new format of culture

  7. WFIRST: Update on the Coronagraph Science Requirements

    Science.gov (United States)

    Douglas, Ewan S.; Cahoy, Kerri; Carlton, Ashley; Macintosh, Bruce; Turnbull, Margaret; Kasdin, Jeremy; WFIRST Coronagraph Science Investigation Teams

    2018-01-01

    The WFIRST Coronagraph instrument (CGI) will enable direct imaging and low resolution spectroscopy of exoplanets in reflected light and imaging polarimetry of circumstellar disks. The CGI science investigation teams were tasked with developing a set of science requirements which advance our knowledge of exoplanet occurrence and atmospheric composition, as well as the composition and morphology of exozodiacal debris disks, cold Kuiper Belt analogs, and protoplanetary systems. We present the initial content, rationales, validation, and verification plans for the WFIRST CGI, informed by detailed and still-evolving instrument and observatory performance models. We also discuss our approach to the requirements development and management process, including the collection and organization of science inputs, open source approach to managing the requirements database, and the range of models used for requirements validation. These tools can be applied to requirements development processes for other astrophysical space missions, and may ease their management and maintenance. These WFIRST CGI science requirements allow the community to learn about and provide insights and feedback on the expected instrument performance and science return.

  8. Identifying clouds over the Pierre Auger Observatory using infrared satellite data

    Energy Technology Data Exchange (ETDEWEB)

    Abreu, Pedro; et al.,

    2013-12-01

    We describe a new method of identifying night-time clouds over the Pierre Auger Observatory using infrared data from the Imager instruments on the GOES-12 and GOES-13 satellites. We compare cloud identifications resulting from our method to those obtained by the Central Laser Facility of the Auger Observatory. Using our new method we can now develop cloud probability maps for the 3000 km^2 of the Pierre Auger Observatory twice per hour with a spatial resolution of ~2.4 km by ~5.5 km. Our method could also be applied to monitor cloud cover for other ground-based observatories and for space-based observatories.

  9. The Hydrological Open Air Laboratory (HOAL) in Petzenkirchen: a hypotheses driven observatory

    Science.gov (United States)

    Blöschl, G.; Blaschke, A. P.; Broer, M.; Bucher, C.; Carr, G.; Chen, X.; Eder, A.; Exner-Kittridge, M.; Farnleitner, A.; Flores-Orozco, A.; Haas, P.; Hogan, P.; Kazemi Amiri, A.; Oismüller, M.; Parajka, J.; Silasari, R.; Stadler, P.; Strauß, P.; Vreugdenhil, M.; Wagner, W.; Zessner, M.

    2015-07-01

    Hydrological observatories bear a lot of resemblance to the more traditional research catchment concept but tend to differ in providing more long term facilities that transcend the lifetime of individual projects, are more strongly geared towards performing interdisciplinary research, and are often designed as networks to assist in performing collaborative science. This paper illustrates how the experimental and monitoring setup of an observatory, the 66 ha Hydrological Open Air Laboratory (HOAL) in Petzenkirchen, Lower Austria, has been established in a way that allows meaningful hypothesis testing. The overarching science questions guided site selection, identifying dissertation topics and the base monitoring. The specific hypotheses guided the dedicated monitoring and sampling, individual experiments, and repeated experiments with controlled boundary conditions. The purpose of the HOAL is to advance the understanding of water related flow and transport processes involving sediments, nutrients and microbes in small catchments. The HOAL catchment is ideally suited for this purpose, because it features a range of different runoff generation processes (surface runoff, springs, tile drains, wetlands), the nutrient inputs are known, and it is convenient from a logistic point of view as all instruments can be connected to the power grid and a high speed glassfibre Local Area Network. The multitude of runoff generation mechanisms in the catchment provide a genuine laboratory where hypotheses of flow and transport can be tested, either by controlled experiments or by contrasting sub-regions of different characteristics. This diversity also ensures that the HOAL is representative of a range of catchments around the world and the specific process findings from the HOAL are applicable to a variety of agricultural catchment settings. The HOAL is operated jointly by the Vienna University of Technology and the Federal Agency for Water Management and takes advantage of the

  10. Low-T, Low-Q Cryocoolers for Science Instruments

    Data.gov (United States)

    National Aeronautics and Space Administration — The purpose of the planned research is to advance the current space science instruments through the development of light weight and low power cryocoolers. Currently,...

  11. Localization of the solar flare SF900610 in X-rays with the WATCH instrument of the GRANAT observatory

    DEFF Research Database (Denmark)

    Terekhov, O.V.; Kuzmin, A.G.; Shevchenko, A.V.

    2002-01-01

    -ray source do not coincide with the coordinates of the Ha-line flare. The X-ray source moved over the solar disk during the flare. This probably implies that, as the X-ray emission was generated, different parts of one loop or a system of magnetic loops dominated at different flare times.......During the solar flare of June 10, 1990, the WATCH instrument of the GRANAT space observatory obtained 110 localizations of the X-ray source in the X-ray range 8-20 keV. Its coordinates were measured with an accuracy of similar to2 arcmin at a 3sigma confidence level. The coordinates of the X...

  12. The University of Montana's Blue Mountain Observatory

    Science.gov (United States)

    Friend, D. B.

    2004-12-01

    The University of Montana's Department of Physics and Astronomy runs the state of Montana's only professional astronomical observatory. The Observatory, located on nearby Blue Mountain, houses a 16 inch Boller and Chivens Cassegrain reflector (purchased in 1970), in an Ash dome. The Observatory sits just below the summit ridge, at an elevation of approximately 6300 feet. Our instrumentation includes an Op-Tec SSP-5A photoelectric photometer and an SBIG ST-9E CCD camera. We have the only undergraduate astronomy major in the state (technically a physics major with an astronomy option), so our Observatory is an important component of our students' education. Students have recently carried out observing projects on the photometry of variable stars and color photometry of open clusters and OB associations. In my poster I will show some of the data collected by students in their observing projects. The Observatory is also used for public open houses during the summer months, and these have become very popular: at times we have had 300 visitors in a single night.

  13. The Science of the Sudbury Neutrino Observatory (SNO) and SNOLAB

    CERN Multimedia

    CERN. Geneva

    2017-01-01

    A description of the science associated with the Sudbury Neutrino Observatory and its relation to other neutrino measurements will be given, along with a discussion of the new set of experiments that are at various stages of development or operation at SNOLAB. These experiments will perform measurements of neutrino properties and seek direct detection of Weakly-Interacting Massive Particles (WIMPS) as Dark Matter candidates. The experiments include SNO+, in which the central element of the SNO detector will be liquid scintillator with Te dissolved for neutrino-less double beta decay; DEAP, using about 3300 kg of liquid argon for single phase direct Dark Matter detection; SuperCDMS, a solid state bolometer system to start construction at SNOLAB in the near future; PICO, a direct Dark Matter experiment using bubble formation for detection and NEWS, a direct Dark Matter detector using high pressure gasses for low-mass WIMP detection.

  14. Press Meeting 20 January 2003: First Light for Europe's Virtual Observatory

    Science.gov (United States)

    2002-12-01

    Observatory (VO) so that astronomers can explore the digital Universe in the new archives across the entire spectrum. Similarly to how a real observatory consists of telescopes, each with a collection of unique astronomical instruments, the VO consists of a collection of data centres each with unique collections of astronomical data, software systems, and processing capabilities. The Astrophysical Virtual Observatory Project (AVO) will conduct a research and demonstration programme on the scientific requirements and technologies necessary to build a VO for European astronomy. The AVO has been jointly funded by the European Commission (under FP5 - Fifth Framework Programme) with six European organisations participating in a three year Phase-A work programme, valued at 5 million Euro. The partner organisations are the European Southern Observatory (ESO) in Munich, Germany, the European Space Agency (ESA), AstroGrid (funded by PPARC as part of the UK's E-Science programme), the CNRS-supported Centre de Données Astronomiques de Strasbourg (CDS), the University Louis Pasteur in Strasbourg, France, the CNRS-supported TERAPIX astronomical data centre at the Institut d'Astrophysique in Paris, France, and the Jodrell Bank Observatory of the Victoria University of Manchester, United Kingdom. The Phase A program will focus its effort in the following areas: * A detailed description of the science requirements for the AVO will be constructed, following the experience gained in a smaller-scale science demonstration program called ASTROVIRTEL (Accessing Astronomical Archives as Virtual Telescopes). * The difficult issue of data and archive interoperability will be addressed by new standards definitions for astronomical data and trial programmes of "joins" between specific target archives within the project team. * The necessary GRID and database technologies will be assessed and tested for use within a full AVO implementation. The AVO project is currently working in conjunction with other

  15. ESO's Two Observatories Merge

    Science.gov (United States)

    2005-02-01

    , a unique instrument capable of measuring stellar radial velocities with an unsurpassed accuracy better than 1 m/s, making it a very powerful tool for the discovery of extra-solar planets. In addition, astronomers have also access to the 2.2-m ESO/MPG telescope with its Wide Field Imager camera. A new control room, the RITZ (Remote Integrated Telescope Zentrum), allows operating all three ESO telescopes at La Silla from a single place. The La Silla Observatory is also the first world-class observatory to have been granted certification for the International Organization for Standardization (ISO) 9001 Quality Management System. Moreover, the infrastructure of La Silla is still used by many of the ESO member states for targeted projects such as the Swiss 1.2-m Euler telescope and the robotic telescope specialized in the follow-up of gamma-ray bursts detected by satellites, the Italian REM (Rapid Eye Mount). In addition, La Silla is in charge of the APEX (Atacama Pathfinder Experiment) 12-m sub-millimetre telescope which will soon start routine observations at Chajnantor, the site of the future Atacama Large Millimeter Array (ALMA). The APEX project is a collaboration between the Max Planck Society in Germany, Onsala Observatory in Sweden and ESO. ESO also operates Paranal, home of the Very Large Telescope (VLT) and the VLT Interferometer (VLTI). Antu, the first 8.2-m Unit Telescope of the VLT, saw First Light in May 1998, starting what has become a revolution in European astronomy. Since then, the three other Unit Telescopes - Kueyen, Melipal and Yepun - have been successfully put into operation with an impressive suite of the most advanced astronomical instruments. The interferometric mode of the VLT (VLTI) is also operational and fully integrated in the VLT data flow system. In the VLTI mode, one state-of-the-art instrument is already available and another will follow soon. With its remarkable resolution and unsurpassed surface area, the VLT is at the forefront of

  16. Searching the Heavens and the Earth: This History of Jesuit Observatories

    Science.gov (United States)

    Udías, Agustín

    2003-10-01

    Jesuits established a large number of astronomical, geophysical and meteorological observatories during the 17th and 18th centuries and again during the 19th and 20th centuries throughout the world. The history of these observatories has never been published in a complete form. Many early European astronomical observatories were established in Jesuit colleges. During the 17th and 18th centuries Jesuits were the first western scientists to enter into contact with China and India. It was through them that western astronomy was first introduced in these countries. They made early astronomical observations in India and China and they directed for 150 years the Imperial Observatory of Beijing. In the 19th and 20th centuries a new set of observatories were established. Besides astronomy these now included meteorology and geophysics. Jesuits established some of the earliest observatories in Africa, South America and the Far East. Jesuit observatories constitute an often forgotten chapter of the history of these sciences. This volume is aimed at all scientists and students who do not want to forget the Jesuit contributions to science. Link: http://www.wkap.nl/prod/b/1-4020-1189-X

  17. Fine Guidance Sensing for Coronagraphic Observatories

    Science.gov (United States)

    Brugarolas, Paul; Alexander, James W.; Trauger, John T.; Moody, Dwight C.

    2011-01-01

    Three options have been developed for Fine Guidance Sensing (FGS) for coronagraphic observatories using a Fine Guidance Camera within a coronagraphic instrument. Coronagraphic observatories require very fine precision pointing in order to image faint objects at very small distances from a target star. The Fine Guidance Camera measures the direction to the target star. The first option, referred to as Spot, was to collect all of the light reflected from a coronagraph occulter onto a focal plane, producing an Airy-type point spread function (PSF). This would allow almost all of the starlight from the central star to be used for centroiding. The second approach, referred to as Punctured Disk, collects the light that bypasses a central obscuration, producing a PSF with a punctured central disk. The final approach, referred to as Lyot, collects light after passing through the occulter at the Lyot stop. The study includes generation of representative images for each option by the science team, followed by an engineering evaluation of a centroiding or a photometric algorithm for each option. After the alignment of the coronagraph to the fine guidance system, a "nulling" point on the FGS focal point is determined by calibration. This alignment is implemented by a fine alignment mechanism that is part of the fine guidance camera selection mirror. If the star images meet the modeling assumptions, and the star "centroid" can be driven to that nulling point, the contrast for the coronagraph will be maximized.

  18. Experience in CCD Photometry at the Tartu Observatory

    Directory of Open Access Journals (Sweden)

    Tuvikene T.

    2003-12-01

    Full Text Available We give overview of the CCD instrumentation and data reduction techniques used at the Tartu Observatory. The first results from photometric observations of the peculiar variable V838 Mon are presented.

  19. EVALSO: A New High-speed Data Link to Chilean Observatories

    Science.gov (United States)

    2010-11-01

    the new generation of VLT instruments coming online in the next few years. This means that for much of the data coming from Paranal, the only practical way to send it to ESO Headquarters has been to save it onto hard drives and send these by airmail. This can mean a wait of days or even weeks before observations from VISTA are ready for analysis. Even with this careful rationing of the connection and sophisticated data management to use the connection as efficiently as possible, the link can get saturated at peak times. While this causes no major problems at present, it indicates that the link is reaching capacity. ESO Director General Tim de Zeeuw said: "ESO's observatory at Paranal is growing, with new telescopes and instruments coming online. Our world-class scientific observatories need state-of-the-art infrastructure." In the place of the existing connection, which has a limit of 16 megabit/s (similar to home ADSL broadband), EVALSO will provide a much faster 10 gigabit/s link - a speed fast enough to transfer an entire DVD movie in a matter of seconds [3]. Mario Campolargo, Director, Emerging Technologies and Infrastructures at the European Commission, said: "It is strategically important that the community of astronomers of Europe gets the best access possible to the ESO observatories: this is one of the reasons why the European Union supports the deployment of regional e-infrastructures for science in Latin America and interlinks them with GÉANT [4] and other EU e-infrastructures." The dramatic increase in bandwidth will allow increased use of Paranal's data from a distance, in real-time. It will allow easier monitoring of the VISTA telescope's performance, and quicker access to VLT data, increasing the responsiveness of quality control. And with the expanded bandwidth, new opportunities will open up, such as astronomers and technicians taking part in meetings via high-definition videoconferencing without having to travel to Chile. Moreover, looking forward

  20. Remote Access to Instrumental Analysis for Distance Education in Science

    Directory of Open Access Journals (Sweden)

    Dietmar Kennepohl

    2005-11-01

    Full Text Available Remote access to experiments offers distance educators another tool to integrate a strong laboratory component within a science course. Since virtually all modern chemical instrumental analysis in industry now use devices operated by a computer interface, remote control of instrumentation is not only relatively facile, it enhances students’ opportunity to learn the subject matter and be exposed to “real world” contents. Northern Alberta Institute of Technology (NAIT and Athabasca University are developing teaching laboratories based on the control of analytical instruments in real-time via an Internet connection. Students perform real-time analysis using equipment, methods, and skills that are common to modern analytical laboratories (or sophisticated teaching laboratories. Students obtain real results using real substances to arrive at real conclusions, just as they would if they were in a physical laboratory with the equipment; this approach allows students to access to conduct instrumental science experiments, thus providing them with an advantageous route to upgrade their laboratory skills while learning at a distance.

  1. Astronomy Against Terrorism: an Educational Astronomical Observatory Project in Peru

    Science.gov (United States)

    Ishitsuka, M.; Montes, H.; Kuroda, T.; Morimoto, M.; Ishitsuka, J.

    2003-05-01

    The Cosmos Coronagraphic Observatory was completely destroyed by terrorists in 1988. In 1995, in coordination with the Minister of Education of Peru, a project to construct a new Educational Astronomical Observatory has been executed. The main purpose of the observatory is to promote an interest in basic space sciences in young students from school to university levels, through basic astronomical studies and observations. The planned observatory will be able to lodge 25 visitors; furthermore an auditorium, a library and a computer room will be constructed to improve the interest of people in astronomy. Two 15-cm refractor telescopes, equipped with a CCD camera and a photometer, will be available for observations. Also a 6-m dome will house a 60-cm class reflector telescope, which will be donated soon, thanks to a fund collected and organized by the Nishi-Harima Astronomical Observatory in Japan. In addition a new modern planetarium donated by the Government of Japan will be installed in Lima, the capital of Peru. These installations will be widely open to serve the requirements of people interested in science.

  2. Instrumentation for Scientific Computing in Neural Networks, Information Science, Artificial Intelligence, and Applied Mathematics.

    Science.gov (United States)

    1987-10-01

    include Security Classification) Instrumentation for scientific computing in neural networks, information science, artificial intelligence, and...instrumentation grant to purchase equipment for support of research in neural networks, information science, artificail intellignece , and applied mathematics...in Neural Networks, Information Science, Artificial Intelligence, and Applied Mathematics Contract AFOSR 86-0282 Principal Investigator: Stephen

  3. Wavefront-Error Performance Characterization for the James Webb Space Telescope (JWST) Integrated Science Instrument Module (ISIM) Science Instruments

    Science.gov (United States)

    Aronstein, David L.; Smith, J. Scott; Zielinski, Thomas P.; Telfer, Randal; Tournois, Severine C.; Moore, Dustin B.; Fienup, James R.

    2016-01-01

    The science instruments (SIs) comprising the James Webb Space Telescope (JWST) Integrated Science Instrument Module (ISIM) were tested in three cryogenic-vacuum test campaigns in the NASA Goddard Space Flight Center (GSFC)'s Space Environment Simulator (SES). In this paper, we describe the results of optical wavefront-error performance characterization of the SIs. The wavefront error is determined using image-based wavefront sensing (also known as phase retrieval), and the primary data used by this process are focus sweeps, a series of images recorded by the instrument under test in its as-used configuration, in which the focal plane is systematically changed from one image to the next. High-precision determination of the wavefront error also requires several sources of secondary data, including 1) spectrum, apodization, and wavefront-error characterization of the optical ground-support equipment (OGSE) illumination module, called the OTE Simulator (OSIM), 2) plate scale measurements made using a Pseudo-Nonredundant Mask (PNRM), and 3) pupil geometry predictions as a function of SI and field point, which are complicated because of a tricontagon-shaped outer perimeter and small holes that appear in the exit pupil due to the way that different light sources are injected into the optical path by the OGSE. One set of wavefront-error tests, for the coronagraphic channel of the Near-Infrared Camera (NIRCam) Longwave instruments, was performed using data from transverse translation diversity sweeps instead of focus sweeps, in which a sub-aperture is translated andor rotated across the exit pupil of the system.Several optical-performance requirements that were verified during this ISIM-level testing are levied on the uncertainties of various wavefront-error-related quantities rather than on the wavefront errors themselves. This paper also describes the methodology, based on Monte Carlo simulations of the wavefront-sensing analysis of focus-sweep data, used to establish the

  4. The Material Culture of Nineteenth-Century Astrometry, its Circulation and Heritage at the Astronomical Observatory of Lisbon

    Science.gov (United States)

    Raposo, Pedro

    The Astronomical Observatory of Lisbon was founded in 1857 in the sequence of a controversy on stellar parallax measurements involving astronomers from the Observatory of Paris and the Observatory of Pulkovo. The development of this discussion led the contenders to recognize Lisbon as a suitable place to carry out this kind of measurements and to foster the field of stellar astronomy. Some local actors strived to keep up with this wave of international interest and establish a first-rank astronomical institution in the Portuguese capital. In order to fulfil this goal, correspondence was intensively exchanged with leading foreign astronomers and instrument makers. Besides, a Portuguese Navy officer bound to become the first director of the new institution was commissioned to visit several observatories and instrument workshops abroad, and to spend a few years in Pulkovo as a trainee astronomer. Although founded with generous financial support from the Portuguese crown and lavishly equipped and constructed, the Observatory of Lisbon was later affected by limiting budgets and a shortage of qualified personnel. Nevertheless, local efforts to improve instruments as well as observation and calculation techniques enabled its astronomers to yield important contributions to positional astronomy, especially towards the end of the nineteenth century and the beginnings of the twentieth century. The original instruments and spaces of the Observatory of Lisbon, strongly modelled on those of Pulkovo, are very well preserved, constituting an outstanding extant example of a mid-nineteenth century advanced observatory. The history they embody testifies the connectedness of the astronomical heritage worldwide.

  5. Boosting disability research in the engineering sciences. The recommendations of the National Observatory for Training, Research and Innovation on Disability (ONFRIH).

    Science.gov (United States)

    Ravaud, J-F; Boissonnat, V

    2011-02-01

    In 2005, the National Observatory for Training, Research and Innovation on Disability (ONFRIH) was established by French law (Law 2005-102). The mission of ONFRIH is to provide an overview and recommendations for research, training and prevention in the field of disability. In this paper, the authors, respectively the Chairman and Rapporteur of the ONFRIH Working Group "Research and Innovation", present the Observatory's conclusions reached in its 2009 report about engineering sciences research and innovation. After introducing the ONFRIH and recalling the stakes and working methods, they highlight the current state of French research in this area and their thoughts about innovation chain. They evoke the broad outlines of their working group's analysis of this inventory. They conclude by identifying four action plans that express the Observatory's recommendations and were submitted to the responsible ministers. The four main objectives proposed are: (1) to consolidate disability as a major challenge for engineering sciences applications; (2) to reinforce the cooperation between operators at all levels of research and innovation; (3) to encourage the expression of needs within the research and innovation process, and (4) to facilitate the access of disabled people to technological innovations that promote their autonomy and social inclusion. Copyright © 2010 Elsevier Masson SAS. All rights reserved.

  6. Integrating Near Fault Observatories (NFO) for EPOS Implementation Phase

    Science.gov (United States)

    Chiaraluce, Lauro

    2015-04-01

    Following the European Plate Observing System (EPOS) project vision aimed at creating a pan-European infrastructure for Earth sciences to support science for a more sustainable society, we are working on the integration of Near-Fault Observatories (NFOs). NFOs are state of the art research infrastructures consisting of advanced networks of multi-parametric sensors continuously monitoring the chemical and physical processes related to the common underlying earth instabilities governing active faults evolution and the genesis of earthquakes. Such a methodological approach, currently applicable only at the local scale (areas of tens to few hundreds of kilometres), is based on extremely dense networks and less common instruments deserving an extraordinary work on data quality control and multi-parameter data description. These networks in fact usually complement regional seismic and geodetic networks (typically with station spacing of 50-100km) with high-density distributions of seismic, geodetic, geochemical and geophysical sensors located typically within 10-20 km of active faults where large earthquakes are expected in the future. In the initial phase of EPOS-IP, seven NFO nodes will be linked: the Alto Tiberina and Irpinia Observatories in Italy, the Corinth Observatory in Greece, the South-Iceland Seismic Zone, the Valais Observatory in Switzerland, Marmara Sea GEO Supersite in Turkey (EU MARSite) and the Vrancea Observatory in Romania. Our work is aimed at establishing standards and integration within this first core group of NFOs while other NFOs are expected to be installed in the next years adopting the standards established and developed within the EPOS Thematic Core Services (TCS). The goal of our group is to build upon the initial development supported by these few key national observatories coordinated under previous EU projects (NERA and REAKT), inclusive and harmonised TCS supporting the installation over the next decade of tens of near

  7. Building a pipeline of talent for operating radio observatories

    Science.gov (United States)

    Wingate, Lory M.

    2016-07-01

    The National Radio Astronomy Observatory's (NRAO) National and International Non-Traditional Exchange (NINE) Program teaches concepts of project management and systems engineering in a focused, nine-week, continuous effort that includes a hands-on build project with the objective of constructing and verifying the performance of a student-level basic radio instrument. The combination of using a project management (PM)/systems engineering (SE) methodical approach based on internationally recognized standards in completing this build is to demonstrate clearly to the learner the positive net effects of following methodical approaches to achieving optimal results. It also exposes the learner to basic radio science theory. An additional simple research project is used to impress upon the learner both the methodical approach, and to provide a basic understanding of the functional area of interest to the learner. This program is designed to teach sustainable skills throughout the full spectrum of activities associated with constructing, operating and maintaining radio astronomy observatories. NINE Program learners thereby return to their host sites and implement the program in their own location as a NINE Hub. This requires forming a committed relationship (through a formal Letter of Agreement), establishing a site location, and developing a program that takes into consideration the needs of the community they represent. The anticipated outcome of this program is worldwide partnerships with fast growing radio astronomy communities designed to facilitate the exchange of staff and the mentoring of under-represented1 groups of learners, thereby developing a strong pipeline of global talent to construct, operate and maintain radio astronomy observatories.

  8. The EGSE science software of the IBIS instrument on-board INTEGRAL satellite

    International Nuclear Information System (INIS)

    La Rosa, Giovanni; Fazio, Giacomo; Segreto, Alberto; Gianotti, Fulvio; Stephen, John; Trifoglio, Massimo

    2000-01-01

    IBIS (Imager on Board INTEGRAL Satellite) is one of the key instrument on-board the INTEGRAL satellite, the follow up mission of the high energy missions CGRO and Granat. The EGSE of IBIS is composed by a Satellite Interface Simulator, a Control Station and a Science Station. Here are described the solutions adopted for the architectural design of the software running on the Science Station. Some preliminary results are used to show the science functionality, that allowed to understand the instrument behavior, all along the test and calibration campaigns of the Engineering Model of IBIS

  9. From research institution to astronomical museum: a history of the Stockholm Observatory

    Science.gov (United States)

    Yaskell, Steven Haywood

    2008-07-01

    The Royal Swedish Academy of Sciences (RSAS) (or Kungliga Vetenskapsakademien [KvA] in Swedish) founded 1739, opened its first permanent building, an astronomical and meteorological observatory, on 20 September 1753. This was situated at Brunkebergsåsen (formerly Observatorie Lunden, or Observatory Hill), on a high terrace in a northern quarter of Stockholm. This historic building is still sometimes called Gamla Observatoriet (the Old Observatory) and now is formally the Observatory Museum. This paper reviews the history of the Observatory from its function as a scientific astronomical institution to its relatively-recent relegation to museum status.

  10. GAIA virtual observatory - development and practices

    Science.gov (United States)

    Syrjäsuo, Mikko; Marple, Steve

    2010-05-01

    The Global Auroral Imaging Access, or GAIA, is a virtual observatory providing quick access to summary data from satellite and ground-based instruments that remote sense auroral precipitation (http://gaia-vxo.org). This web-based service facilitates locating data relevant to particular events by simultaneously displaying summary images from various data sets around the world. At the moment, there are GAIA server nodes in Canada, Finland, Norway and the UK. The development is an international effort and the software and metadata are freely available. The GAIA system is based on a relational database which is queried by a dedicated software suite that also creates the graphical end-user interface if such is needed. Most commonly, the virtual observatory is used interactively by using a web browser: the user provides the date and the type of data of interest. As the summary data from multiple instruments are displayed simultaneously, the user can conveniently explore the recorded data. The virtual observatory provides essentially instant access to the images originating from all major auroral instrument networks including THEMIS, NORSTAR, GLORIA and MIRACLE. The scientific, educational and outreach use is limited by creativity rather than access. The first version of the GAIA was developed at the University of Calgary (Alberta, Canada) in 2004-2005. This proof-of-concept included mainly THEMIS and MIRACLE data, which comprised of millions of summary plots and thumbnail images. However, it was soon realised that a complete re-design was necessary to increase flexibility. In the presentation, we will discuss the early history and motivation of GAIA as well as how the development continued towards the current version. The emphasis will be on practical problems and their solutions. Relevant design choices will also be highlighted.

  11. Multinational History of Strasbourg Astronomical Observatory

    CERN Document Server

    Heck, André

    2005-01-01

    Strasbourg Astronomical Observatory is quite an interesting place for historians: several changes of nationality between France and Germany, high-profile scientists having been based there, big projects born or installed in its walls, and so on. Most of the documents circulating on the history of the Observatory and on related matters have however been so far poorly referenced, if at all. This made necessary the compilation of a volume such as this one, offering fully-documented historical facts and references on the first decades of the Observatory history, authored by both French and German specialists. The experts contributing to this book have done their best to write in a way understandable to readers not necessarily hyperspecialized in astronomy nor in the details of European history. After an introductory chapter by the Editor, contributions by Wolfschmidt and by Duerbeck respectively deal extensively with the German periods and review people and instrumentation, while another paper by Duerbeck is more...

  12. Data, instruments, and theory a dialectical approach to understanding science

    CERN Document Server

    Ackermann, Robert John

    1985-01-01

    Robert John Ackermann deals decisively with the problem of relativism that has plagued post-empiricist philosophy of science. Recognizing that theory and data are mediated by data domains (bordered data sets produced by scientific instruments), he argues that the use of instruments breaks the dependency of observation on theory and thus creates a reasoned basis for scientific objectivity.

  13. Astrophysics science operations - Near-term plans and vision

    Science.gov (United States)

    Riegler, Guenter R.

    1991-01-01

    Astrophysics science operations planned by the Science Operations branch of NASA Astrophysics Division for the 1990s for the purpose of gathering spaceborne astronomical data are described. The paper describes the near-future plans of the Science Operations in the areas of the preparation of the proposal; the planning and execution of spaceborne observations; the collection, processing, and analysis data; and the dissemination of results. Also presented are concepts planned for introduction at the beginning of the 20th century, including the concepts of open communications, transparent instrument and observatory operations, a spiral requirements development method, and an automated research assistant.

  14. Construction and Validation of an Instrument to Measure Taiwanese Elementary Students' Attitudes toward Their Science Class

    Science.gov (United States)

    Wang, Tzu-Ling; Berlin, Donna

    2010-12-01

    The main purpose of this study is to develop a valid and reliable instrument for measuring the attitudes toward science class of fourth- and fifth-grade students in an Asian school culture. Specifically, the development focused on three science attitude constructs-science enjoyment, science confidence, and importance of science as related to science class experiences. A total of 265 elementary school students in Taiwan responded to the instrument developed. Data analysis indicated that the instrument exhibited satisfactory validity and reliability with the Taiwan population used. The Cronbach's alpha coefficient was 0.93 for the entire instrument indicating a satisfactory level of internal consistency. However, both principal component analysis and parallel analysis showed that the three attitude scales were not unique and should be combined and used as a general "attitudes toward science class" scale. The analysis also showed that there were no gender or grade-level differences in students' overall attitudes toward science class.

  15. Local Observations, Global Connections: An Educational Program Using Ocean Networks Canada's Community-Based Observatories

    Science.gov (United States)

    Pelz, M.; Hoeberechts, M.; Ewing, N.; Davidson, E.; Riddell, D. J.

    2014-12-01

    Schools on Canada's west coast and in the Canadian Arctic are participating in the pilot year of a novel educational program based on analyzing, understanding and sharing ocean data collected by cabled observatories. The core of the program is "local observations, global connections." First, students develop an understanding of ocean conditions at their doorstep through the analysis of community-based observatory data. Then, they connect that knowledge with the health of the global ocean by engaging with students at other schools participating in the educational program and through supplemental educational resources. Ocean Networks Canada (ONC), an initiative of the University of Victoria, operates cabled ocean observatories which supply continuous power and Internet connectivity to a broad suite of subsea instruments from the coast to the deep sea. This Internet connectivity permits researchers, students and members of the public to download freely available data on their computers anywhere around the globe, in near real-time. In addition to the large NEPTUNE and VENUS cabled observatories off the coast of Vancouver Island, British Columbia, ONC has been installing smaller, community-based cabled observatories. Currently two are installed: one in Cambridge Bay, Nunavut and one at Brentwood College School, on Mill Bay in Saanich Inlet, BC. Several more community-based observatories are scheduled for installation within the next year. The observatories support a variety of subsea instruments, such as a video camera, hydrophone and water quality monitor and shore-based equipment including a weather station and a video camera. Schools in communities hosting an observatory are invited to participate in the program, alongside schools located in other coastal and inland communities. Students and teachers access educational material and data through a web portal, and use video conferencing and social media tools to communicate their findings. A series of lesson plans

  16. The Hydrological Open Air Laboratory (HOAL) in Petzenkirchen: a hypothesis-driven observatory

    Science.gov (United States)

    Blöschl, G.; Blaschke, A. P.; Broer, M.; Bucher, C.; Carr, G.; Chen, X.; Eder, A.; Exner-Kittridge, M.; Farnleitner, A.; Flores-Orozco, A.; Haas, P.; Hogan, P.; Kazemi Amiri, A.; Oismüller, M.; Parajka, J.; Silasari, R.; Stadler, P.; Strauss, P.; Vreugdenhil, M.; Wagner, W.; Zessner, M.

    2016-01-01

    Hydrological observatories bear a lot of resemblance to the more traditional research catchment concept, but tend to differ in providing more long-term facilities that transcend the lifetime of individual projects, are more strongly geared towards performing interdisciplinary research, and are often designed as networks to assist in performing collaborative science. This paper illustrates how the experimental and monitoring set-up of an observatory, the 66 ha Hydrological Open Air Laboratory (HOAL) in Petzenkirchen, Lower Austria, has been established in a way that allows meaningful hypothesis testing. The overarching science questions guided site selection, identification of dissertation topics and the base monitoring. The specific hypotheses guided the dedicated monitoring and sampling, individual experiments, and repeated experiments with controlled boundary conditions. The purpose of the HOAL is to advance the understanding of water-related flow and transport processes involving sediments, nutrients and microbes in small catchments. The HOAL catchment is ideally suited for this purpose, because it features a range of different runoff generation processes (surface runoff, springs, tile drains, wetlands), the nutrient inputs are known, and it is convenient from a logistic point of view as all instruments can be connected to the power grid and a high-speed glassfibre local area network (LAN). The multitude of runoff generation mechanisms in the catchment provides a genuine laboratory where hypotheses of flow and transport can be tested, either by controlled experiments or by contrasting sub-regions of different characteristics. This diversity also ensures that the HOAL is representative of a range of catchments around the world, and the specific process findings from the HOAL are applicable to a variety of agricultural catchment settings. The HOAL is operated jointly by the Vienna University of Technology and the Federal Agency for Water Management and takes

  17. Polar Motion Studies and NOAA's Legacy of International Scientific Cooperation: Ukiah and Gaithersburg Latitude Observatories

    Science.gov (United States)

    Caccamise, D. J., II; Stone, W. A.

    2017-12-01

    In 1895, the International Geodetic Association invited the United States Coast and Geodetic Survey (USC&GS) to join in an unprecedented international effort to observe and measure the earth's polar motion. This effort was in response to the American astronomer Seth C. Chandler Jr. announcing his 1891 discovery that the earth's axis of rotation—and hence the direction of true north—wobbles within the earth with a period of about 14 months, varying latitude everywhere on the globe. In 1899, two astro-geodetic observatories were built in Gaithersburg, Maryland and Ukiah, California with three others in Caloforte, Italy; Kitab, Russia (now Uzbekistan); and Mizusawa, Japan. (A sixth station was located and operated at an astronomical observatory in Cincinnati, Ohio until 1916 using instruments loaned by USC&GS). All five observatories were located along the same parallel - approximately 35 degrees - 8 minutes. The observatories were decommissioned in 1982, and subsequently, NOAA deeded the two remaining U.S. observatories to the cities of Gaithersburg and Ukiah. The observatories and adjacent property were to be used as parkland. Both cities have restored the observatories and opened public parks. Recently, Gaithersburg (Ukiah in progress) has had its latitude observatory dedicated as a National Historic Landmark. In 2014-15, the National Geodetic Survey (NGS, the present-day NOAA successor to the USC&GS) loaned the original zenith telescopes to the communities, returning the observatories to their original configuration. The contribution of NOAA observers and the data collected is still important to astronomers and geophysicists and has practical applications in spacecraft navigation and geospatial positioning. This poster will bring to fruition this multiyear effort among partners by providing examples of NOAA's mission and contribution to science, service, and stewardship at both geodetic observatories, through programs and historic exhibits for students and the

  18. The History of Radio Astronomy and the National Radio Astronomy Observatory: Evolution Toward Big Science

    Science.gov (United States)

    Malphrus, Benjamin Kevin

    1990-01-01

    The purpose of this study is to examine the sequence of events that led to the establishment of the NRAO, the construction and development of instrumentation and the contributions and discovery events and to relate the significance of these events to the evolution of the sciences of radio astronomy and cosmology. After an overview of the resources, a brief discussion of the early days of the science is given to set the stage for an examination of events that led to the establishment of the NRAO. The developmental and construction phases of the major instruments including the 85-foot Tatel telescope, the 300-foot telescope, the 140-foot telescope, and the Green Bank lnterferometer are examined. The technical evolution of these instruments is traced and their relevance to scientific programs and discovery events is discussed. The history is told in narrative format that is interspersed with technical and scientific explanations. Through the use of original data technical and scientific information of historical concern is provided to elucidate major developments and events. An interpretive discussion of selected programs, events and technological developments that epitomize the contributions of the NRAO to the science of radio astronomy is provided. Scientific programs conducted with the NRAO instruments that were significant to galactic and extragalactic astronomy are presented. NRAO research programs presented include continuum and source surveys, mapping, a high precision verification of general relativity, and SETI programs. Cosmic phenomena investigated in these programs include galactic and extragalactic HI and HII, emission nebula, supernova remnants, cosmic masers, giant molecular clouds, radio stars, normal and radio galaxies, and quasars. Modern NRAO instruments including the VLA and VLBA and their scientific programs are presented in the final chapter as well as plans for future NRAO instruments such as the GBT.

  19. A Dedicated Space Observatory For Time-domain Solar System Science

    Science.gov (United States)

    Wong, Michael H.; Ádámkovics, M.; Benecchi, S.; Bjoraker, G.; Clarke, J. T.; de Pater, I.; Hendrix, A. R.; Marchis, F.; McGrath, M.; Noll, K.; Rages, K. A.; Retherford, K.; Smith, E. H.; Strange, N. J.

    2009-09-01

    Time-variable phenomena with scales ranging from minutes to decades have led to a large fraction of recent advances in many aspects of solar system science. We present the scientific motivation for a dedicated space observatory for solar system science. This facility will ideally conduct repeated imaging and spectroscopic observations over a period of 10 years or more. It will execute a selection of long-term projects with interleaved scheduling, resulting in the acquisition of data sets with consistent calibration, long baselines, and optimized sampling intervals. A sparse aperture telescope would be an ideal configuration for the mission, trading decreased sensitivity for reduced payload mass, while preserving spatial resolution. Ultraviolet capability is essential, especially once the Hubble Space Telescope retires. Specific investigations will include volcanism and cryovolcanism (on targets including Io, Titan, Venus, Mars, and Enceladus); zonal flow, vortices, and storm evolution on the giant planets; seasonal cycles in planetary atmospheres; mutual events and orbit determination of multiple small solar system bodies; auroral activity and solar wind interactions; and cometary evolution. The mission will produce a wealth of data products--such as multi-year time-lapse movies of planetary atmospheres--with significant education and public outreach potential. Existing and planned ground- and space-based facilities are not suitable for these time-domain optimized planetary dynamics studies for numerous reasons, including: oversubscription by astrophysical users, field-of-regard limitations, sensitive detector saturation limits that preclude bright planetary targets, and limited mission duration. The abstract author list is a preliminary group of scientists who have shown interest in prior presentations on this topic; interested parties may contact the lead author by 1 September to sign the associated Planetary Science Decadal Survey white paper or by 1 October to

  20. Prototyping a Global Soft X-Ray Imaging Instrument for Heliophysics, Planetary Science, and Astrophysics Science

    Science.gov (United States)

    Collier, M. R.; Porter, F. S.; Sibeck, D. G.; Carter, J. A.; Chiao, M. P.; Chornay, D. J.; Cravens, T.; Galeazzi, M.; Keller, J. W.; Koutroumpa, D.; hide

    2012-01-01

    We describe current progress in the development of a prototype wide field-of-view soft X-ray imager that employs Lobstereye optics and targets heliophysics, planetary, and astrophysics science. The prototype will provide proof-of-concept for a future flight instrument capable of imaging the entire dayside magnetosheath from outside the magnetosphere. Such an instrument was proposed for the ESA AXIOM mission.

  1. Prototyping a Global Soft X-ray Imaging Instrument for Heliophysics, Planetary Science, and Astrophysics Science

    Science.gov (United States)

    Collier, Michael R.; Porter, F. Scott; Sibeck, David G.; Carter, Jenny A.; Chiao, Meng P.; Chornay, Dennis J.; Cravens, Thomas; Galeazzi, Massimiliano; Keller, John W.; Koutroumpa, Dimitra; hide

    2012-01-01

    We describe current progress in the development of a prototype wide field-of-view soft X-ray imager that employs Lobster-eye optics and targets heliophysics, planetary, and astrophysics science. The prototype will provide proof-of-concept for a future flight instrument capable of imaging the entire dayside magnetosheath from outside the magnetosphere. Such an instrument was proposed for the FSA AXIOM mission

  2. Ten years of the Spanish Virtual Observatory

    Science.gov (United States)

    Solano, E.

    2015-05-01

    The main objective of the Virtual Observatory (VO) is to guarantee an easy and efficient access and analysis of the information hosted in astronomical archives. The Spanish Virtual Observatory (SVO) is a project that was born in 2004 with the goal of promoting and coordinating the VO-related activities at national level. SVO is also the national contact point for the international VO initiatives, in particular the International Virtual Observatory Alliance (IVOA) and the Euro-VO project. The project, led by Centro de Astrobiología (INTA-CSIC), is structured around four major topics: a) VO compliance of astronomical archives, b) VO-science, c) VO- and data mining-tools, and d) Education and outreach. In this paper I will describe the most important results obtained by the Spanish Virtual Observatory in its first ten years of life as well as the future lines of work.

  3. Jantar Mantar: Observatories of Jai Singh (with pop-up pages)

    Indian Academy of Sciences (India)

    BOOK REVIEW. Jantar Mantar: Observatories of Jai. Singh (with pop-up pages). Biman Nath. Jantar Mantar: Observatories of Jai Singh. By: B S Shylaja and V S S Sastry. Bilingual Edition: English and Kannada. Published by Bangalore Association for. Science Education, Price:|500. Most of us have looked at the giant ...

  4. OSoMe: the IUNI observatory on social media

    Directory of Open Access Journals (Sweden)

    Clayton A. Davis

    2016-10-01

    Full Text Available The study of social phenomena is becoming increasingly reliant on big data from online social networks. Broad access to social media data, however, requires software development skills that not all researchers possess. Here we present the IUNI Observatory on Social Media, an open analytics platform designed to facilitate computational social science. The system leverages a historical, ongoing collection of over 70 billion public messages from Twitter. We illustrate a number of interactive open-source tools to retrieve, visualize, and analyze derived data from this collection. The Observatory, now available at osome.iuni.iu.edu, is the result of a large, six-year collaborative effort coordinated by the Indiana University Network Science Institute.

  5. The Large Observatory For x-ray Timing

    DEFF Research Database (Denmark)

    Feroci, M.; Herder, J. W. den; Bozzo, E.

    2014-01-01

    The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study th...

  6. The Atomic, Molecular and Optical Science instrument at the Linac Coherent Light Source

    Energy Technology Data Exchange (ETDEWEB)

    Ferguson, Ken R. [Linac Coherent Light Source, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025 (United States); Department of Applied Physics, Stanford University, 348 Via Pueblo, Stanford, CA 94305 (United States); Bucher, Maximilian; Bozek, John D.; Carron, Sebastian; Castagna, Jean-Charles [Linac Coherent Light Source, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025 (United States); Coffee, Ryan [Linac Coherent Light Source, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025 (United States); Pulse Institute, Stanford University and SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025 (United States); Curiel, G. Ivan; Holmes, Michael; Krzywinski, Jacek; Messerschmidt, Marc; Minitti, Michael; Mitra, Ankush; Moeller, Stefan; Noonan, Peter; Osipov, Timur; Schorb, Sebastian; Swiggers, Michele; Wallace, Alexander; Yin, Jing [Linac Coherent Light Source, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025 (United States); Bostedt, Christoph, E-mail: bostedt@slac.stanford.edu [Linac Coherent Light Source, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025 (United States); Pulse Institute, Stanford University and SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025 (United States)

    2015-04-17

    A description of the Atomic, Molecular and Optical Sciences (AMO) instrument at the Linac Coherent Light Source is presented. Recent scientific highlights illustrate the imaging, time-resolved spectroscopy and high-power density capabilities of the AMO instrument. The Atomic, Molecular and Optical Science (AMO) instrument at the Linac Coherent Light Source (LCLS) provides a tight soft X-ray focus into one of three experimental endstations. The flexible instrument design is optimized for studying a wide variety of phenomena requiring peak intensity. There is a suite of spectrometers and two photon area detectors available. An optional mirror-based split-and-delay unit can be used for X-ray pump–probe experiments. Recent scientific highlights illustrate the imaging, time-resolved spectroscopy and high-power density capabilities of the AMO instrument.

  7. The architecture of Hamburg-Bergedorf Observatory 1906 - 1912, compared with other observatories (German Title: Die Architektur der Hamburg-Bergedorfer Sternwarte 1906 - 1912 im Vergleich mit anderen Observatorien)

    Science.gov (United States)

    Müller, Peter

    The foundation of the astrophysical observatories in Potsdam-Telegrafenberg in 1874, in Meudon near Paris in 1875 and in Mount Hamilton in California in 1875 resulted in a complete change of observatory architecture. Astrometry had become irrelevant; meridian halls, i.e. an exact north-south orientation, were no longer necessary. The location in the centre of a (university) town was disadvantageous, due to vibrations caused by traffic and artificial light at night. New principles were defined: considerable distance (from the city center), secluded and exposed position (on a mountain) and construction of pavilions: inside a park a pavilion was built for each instrument. Other observatories of this type are: Pic du Midi in the French Alps, built as from 1878 as the first permanent observatory in the high mountains; Nice, Mont Gros, (1879); Brussels, Uccle (1883); Edinburgh, Blackford Hill (1892); Heidelberg, Königstuhl (1896); Barcelona, Monte Tibidado (1902). The original Hamburg Observatory was a modest rectangular building near the Millernrtor; in 1833 it became a State institute. As from 1906 erection of a spacious complex in Bergedorf, 20 km northeast of the city center, took place. Except for the unavailable position on a mountain, this complex fulfilled all principles of a modern observatory: in a park pavilion architecture in an elegant neo-baroque style designed by Albert Erbe (architect of the new Hamburger Kunsthalle with cupola). At the Hamburg Observatory the domed structures were cleverly hierarchised leaving an open view to the south. At the beginning astrometry and astrophysics were equally important; there was still a meridian circle. Apart from that, the instruments were manifold: a large refractor 0.60 m (installed by Repsold/Hamburg, 9 m focal length) and a large reflector 1 m (Zeiss/Jena, 3m focal length). Both were the largest instruments of their kind in the German Empire. In addition, there was the Lippert Astrograph on an elegant polar

  8. Spectroscopic characterization of extrasolar planets from ground-, space- and airborne-based observatories

    Science.gov (United States)

    Angerhausen, Daniel

    2010-11-01

    reductions were unable to achieve this feat. This work shows that systematic effecting the spectrophotometric light-curves in HST can be removed to levels needed to observe features in the relatively small scale-height atmospheres of hot Neptune class planets orbiting nearby stars. In the third and final part of this thesis, I develop and discuss possible science cases for the airborne Stratospheric Observatory for Infrared Astronomy (SOFIA) in the field of detection and characterization of extrasolar planets. The principle advantages of SOFIA and its suite of instrumentation is illustrated and possible targets are introduced. Possible next generation instrumentation (dedicated to exoplanetary science) is discussed.

  9. Fault Detection and Correction for the Solar Dynamics Observatory Attitude Control System

    Science.gov (United States)

    Starin, Scott R.; Vess, Melissa F.; Kenney, Thomas M.; Maldonado, Manuel D.; Morgenstern, Wendy M.

    2007-01-01

    The Solar Dynamics Observatory is an Explorer-class mission that will launch in early 2009. The spacecraft will operate in a geosynchronous orbit, sending data 24 hours a day to a devoted ground station in White Sands, New Mexico. It will carry a suite of instruments designed to observe the Sun in multiple wavelengths at unprecedented resolution. The Atmospheric Imaging Assembly includes four telescopes with focal plane CCDs that can image the full solar disk in four different visible wavelengths. The Extreme-ultraviolet Variability Experiment will collect time-correlated data on the activity of the Sun's corona. The Helioseismic and Magnetic Imager will enable study of pressure waves moving through the body of the Sun. The attitude control system on Solar Dynamics Observatory is responsible for four main phases of activity. The physical safety of the spacecraft after separation must be guaranteed. Fine attitude determination and control must be sufficient for instrument calibration maneuvers. The mission science mode requires 2-arcsecond control according to error signals provided by guide telescopes on the Atmospheric Imaging Assembly, one of the three instruments to be carried. Lastly, accurate execution of linear and angular momentum changes to the spacecraft must be provided for momentum management and orbit maintenance. In thsp aper, single-fault tolerant fault detection and correction of the Solar Dynamics Observatory attitude control system is described. The attitude control hardware suite for the mission is catalogued, with special attention to redundancy at the hardware level. Four reaction wheels are used where any three are satisfactory. Four pairs of redundant thrusters are employed for orbit change maneuvers and momentum management. Three two-axis gyroscopes provide full redundancy for rate sensing. A digital Sun sensor and two autonomous star trackers provide two-out-of-three redundancy for fine attitude determination. The use of software to maximize

  10. Cryo Testing of tbe James Webb Space Telescope's Integrated Science Instrument Module

    Science.gov (United States)

    VanCampen, Julie

    2004-01-01

    The Integrated Science Instrument Module (ISIM) of the James Webb Space Telescope will be integrated and tested at the Environmental Test Facilities at Goddard Space Flight Center (GSFC). The cryogenic thermal vacuum testing of the ISIM will be the most difficult and problematic portion of the GSFC Integration and Test flow. The test is to validate the coupled interface of the science instruments and the ISIM structure and to sufficiently stress that interface while validating image quality of the science instruments. The instruments and the structure are not made from the same materials and have different CTE. Test objectives and verification rationale are currently being evaluated in Phase B of the project plan. The test program will encounter engineering challenges and limitations, which are derived by cost and technology many of which can be mitigated by facility upgrades, creative GSE, and thorough forethought. The cryogenic testing of the ISIM will involve a number of risks such as the implementation of unique metrology techniques, mechanical, electrical and optical simulators housed within the cryogenic vacuum environment. These potential risks are investigated and possible solutions are proposed.

  11. From AISR to the Virtual Observatory

    Science.gov (United States)

    Szalay, Alexander S.

    2014-01-01

    The talk will provide a retrospective on important results enabled by the NASA AISR program. The program had a unique approach to funding research at the intersection of astrophysics, applied computer science and statistics. It had an interdisciplinary angle, encouraged high risk, high return projects. Without this program the Virtual Observatory would have never been started. During its existence the program has funded some of the most innovative applied computer science projects in astrophysics.

  12. Smartphone measurement engineering - Innovative challenges for science & education, instrumentation & training

    Science.gov (United States)

    Hofmann, D.; Dittrich, P.-G.; Duentsch, E.

    2010-07-01

    Smartphones have an enormous conceptual and structural influence on measurement science & education, instrumentation & training. Smartphones are matured. They became convenient, reliable and affordable. In 2009 worldwide 174 million Smartphones has been delivered. Measurement with Smartphones is ready for the future. In only 10 years the German vision industry tripled its global sales volume to one Billion Euro/Year. Machine vision is used for mobile object identification, contactless industrial quality control, personalized health care, remote facility and transport management, safety critical surveillance and all tasks which are too complex for the human eye or too monotonous for the human brain. Aim of the paper is to describe selected success stories for the application of Smartphones for measurement engineering in science and education, instrumentation and training.

  13. Quartz tube extensometer for observation of Earth tides and local tectonic deformations at the Sopronbanfalva Geodynamic Observatory, Hungary

    International Nuclear Information System (INIS)

    Mentes, Gy.

    2010-01-01

    In May 1990, a quartz tube extensometer was installed in the Sopronbanfalva Geodynamic Observatory of the Geodetic and Geophysical Research Institute (GGRI) of the Hungarian Academy of Sciences for recording Earth tides and recent tectonic movements. The paper describes the construction of the extensometer and a portable calibrator used for the in situ calibration of the instrument. The extensometer is very sensitive. Its scale factor is 2.093±0.032 nm/mV according to the highly precise calibration method developed at the GGRI. Since the stability of extensometers is strongly influenced by the geological structure and properties of the rocks in the vicinity of the recording site, the observatory instrument system was tested by coherence analysis between theoretical (as the input signal) and measured tidal data series (as the output signal). In the semidiurnal tidal frequency band the coherence is better than 0.95, while in the diurnal band it is about 0.8. Probably this is due to the fact that the noise is higher in the diurnal band (0.4-0.5 nstr) than in the semidiurnal band (0.19-0.22 nstr). Coherence analysis between theoretical and measured data corrected for barometric changes yielded a small improvement of coherence in both frequency bands, while using temperature data correction, no observable improvement was obtained. Results of the tidal analysis also show that the observatory instrument system is suitable for recording very small tectonic movements. The 18 years of continuous data series measured by the extensometer prove the high quality of the extensometer. On the basis of investigations, it was pointed out that further efforts should be done to improve the barometric correction method and that correction for ocean load, as well as considering topographic and cavity effects are necessary to increase the accuracy of determining tidal parameters.

  14. ExoMars Trace Gas Orbiter Instrument Modelling Approach to Streamline Science Operations

    Science.gov (United States)

    Munoz Fernandez, Michela; Frew, David; Ashman, Michael; Cardesin Moinelo, Alejandro; Garcia Beteta, Juan Jose; Geiger, Bernhard; Metcalfe, Leo; Nespoli, Federico; Muniz Solaz, Carlos

    2018-05-01

    ExoMars Trace Gas Orbiter (TGO) science operations activities are centralised at ESAC's Science Operations Centre (SOC). The SOC receives the inputs from the principal investigators (PIs) in order to implement and deliver the spacecraft pointing requests and instrument timelines to the Mission Operations Centre (MOC). The high number of orbits per planning cycle has made it necessary to abstract the planning interactions between the SOC and the PI teams at the observation level. This paper describes the modelling approach we have conducted for TGOís instruments to streamline science operations. We have created dynamic observation types that scale to adapt to the conditions specified by the PI teams including observation timing, and pointing block parameters calculated from observation geometry. This approach is considered and improvement with respect to previous missions where the generation of the observation pointing and commanding requests was performed manually by the instrument teams. Automation software assists us to effectively handle the high density of planned orbits with increasing volume of scientific data and to successfully meet opportunistic scientific goals and objectives. Our planning tool combines the instrument observation definition files provided by the PIs together with the flight dynamics products to generate the Pointing Requests and the instrument timeline (ITL). The ITL contains all the validated commands at the TC sequence level and computes the resource envelopes (data rate, power, data volume) within the constraints. At the SOC, our main goal is to maximise the science output while minimising the number of iterations among the teams, ensuring that the timeline does not violate the state transitions allowed in the Mission Operations Rules and Constraints Document.

  15. Role of the Chandra X-Ray Observatory Observations for the Study of Ionized Plasmas

    Science.gov (United States)

    Weisskopf, Martin C.

    2010-01-01

    The Chandra X-Ray Observatory, launched in 1999, is now beginning its 12-th year of operation. Chandra, the X-ray component of NASA s Great Observatory program, continues to operate efficiently, somewhat remarkable considering that the Observatory was designed for three years of operation with a goal of five. The Observatory features X-ray optics with sub-arcsecond angular resolution and a small suite of instruments, including transmission gratings, which allow for high-resolution spectroscopy of point sources. We will detail the capabilities of the Observatory for making such spectroscopic measurements and discuss a number of examples of what has been learned about the astrophysical plasmas capable of producing bright X-ray emission.

  16. MMT OBSERVATORY 6.5M CLIO CALIBRATED OBSERVATIONS OF LCROSS

    Data.gov (United States)

    National Aeronautics and Space Administration — This archive contains calibrated observations of the 2009-10-09 impact of the LCROSS spacecraft on the moon by the CLIO instrument on the MMT Observatory 6.5m...

  17. What Are They Thinking? The Development and Use of an Instrument that Identifies Common Science Misconceptions

    Science.gov (United States)

    Stein, Mary; Barman, Charles R.; Larrabee, Timothy

    2007-01-01

    This article describes the rationale for, and development of, an online instrument that helps identify commonly held science misconceptions. Science Beliefs is a 47-item instrument that targets topics in chemistry, physics, biology, earth science, and astronomy. It utilizes a true or false, along with a written-explanation, format. The true or…

  18. Strategies for personnel sustainable lifecycle at astronomical observatories and local industry development

    Science.gov (United States)

    Bendek, Eduardo A.; Leatherbee, Michael; Smith, Heather; Strappa, Valentina; Zinnecker, Hans; Perez, Mario

    2014-08-01

    Specialized manpower required to efficiently operate world-class observatories requires large investments in time and resources to train personnel in very specific areas of engineering. Isolation and distances to mayor cities pose a challenge to retain motivated and qualified personnel on the mountain. This paper presents strategies that we believe may be effective for retaining this specific know-how in the astronomy field; while at the same time develop a local support industry for observatory operations and astronomical instrumentation development. For this study we choose Chile as a research setting because it will host more than 60% of the world's ground based astronomical infrastructure by the end of the decade, and because the country has an underdeveloped industry for astronomy services. We identify the astronomical infrastructure that exists in the country as well as the major research groups and industrial players. We further identify the needs of observatories that could be outsourced to the local economy. As a result, we suggest spin-off opportunities that can be started by former observatory employees and therefore retaining the knowhow of experienced people that decide to leave on-site jobs. We also identify tools to facilitate this process such as the creation of a centralized repository of local capabilities and observatory needs, as well as exchange programs within astronomical instrumentation groups. We believe that these strategies will contribute to a positive work environment at the observatories, reduce the operation and development costs, and develop a new industry for the host country.

  19. Remote observatories for amateur astronomers using high-powered telescopes from home

    CERN Document Server

    Hubbell, Gerald R; Billard, Linda M

    2015-01-01

    Amateur astronomers who want to enhance their capabilities to contribute to science need look no farther than this guide to using remote observatories.  The contributors cover how to build your own remote observatory as well as the existing infrastructure of commercial networks of remote observatories that are available to the amateur. They provide specific advice on which programs to use based on your project objectives and offer practical project suggestions. Remotely controlled observatories have many advantages—the most obvious that the observer does not have to be physically present to carry out observations. Such an observatory can also be used more fully because its time can be scheduled and usefully shared among several astronomers working on different observing projects. More and more professional-level observatories are open to use by amateurs in this way via the Internet, and more advanced amateur astronomers can even build their own remote observatories for sharing among members of a society ...

  20. View of Nature of Science (VNOS Form B: An Instrument for Assessing Preservice Teachers View of Nature of Science at Borneo University Tarakan

    Directory of Open Access Journals (Sweden)

    Listiani Listiani

    2017-03-01

    Full Text Available NOS form B is an instrument that has been developed and revised to assess the view of nature of science of preservice science teachers through nature of science aspects.Indeed, students and teachers have to have the view of nature of science to avoid misconceptions of science concepts. Unfortunately, research on the view of Nature of Science is less conducted in Indonesia. This is a qualitative research that was conducted in Borneo University Tarakan. Respondents are preservice biology teachers in the sixth semester. The first step of this research is translating and adapting the VNOS form B into Bahasa Indonesia to make sure that the instrument is culturally fit to Indonesian and the transadapted instrument then given to the respondents. The result shows that the VNOS form B can be applied to assess the view of nature of science of preservice biology teachers. However, the result also shows that most of preservice biology teachers have few understanding on aspects of nature of scince.

  1. MMS Observatory TV Results Contamination Summary

    Science.gov (United States)

    Rosecrans, Glenn; Brieda, Lubos; Errigo, Therese

    2014-01-01

    The Magnetospheric Multiscale (MMS) mission is a constellation of 4 observatories designed to investigate the fundamental plasma physics of reconnection in the Earth's magnetosphere. The various instrument suites measure electric and magnetic fields, energetic particles, and plasma composition. Each spacecraft has undergone extensive environmental testing to prepare it for its minimum 2 year mission. In this paper, we report on the extensive thermal vacuum testing campaign. The testing was performed at the Naval Research Laboratory utilizing the "Big Blue" vacuum chamber. A total of ten thermal vacuum tests were performed, including two chamber certifications, three dry runs, and five tests of the individual MMS observatories. During the test, the observatories were enclosed in a thermal enclosure known as the "hamster cage". The enclosure allowed for a detailed thermal control of various observatory zone, but at the same time, imposed additional contamination and system performance requirements. The environment inside the enclosure and the vacuum chamber was actively monitored by several QCMs, RGA, and up to 18 ion gauges. Each spacecraft underwent a bakeout phase, which was followed by 4 thermal cycles. Unique aspects of the TV campaign included slow pump downs with a partial represses, thruster firings, Helium identification, and monitoring pressure spikes with ion gauges. Selected data from these TV tests is presented along with lessons learned.

  2. OBSERVATIONS OF BINARY STARS WITH THE DIFFERENTIAL SPECKLE SURVEY INSTRUMENT. I. INSTRUMENT DESCRIPTION AND FIRST RESULTS

    International Nuclear Information System (INIS)

    Horch, Elliott P.; Veillette, Daniel R.; Shah, Sagar C.; O'Rielly, Grant V.; Baena Galle, Roberto; Van Altena, William F.

    2009-01-01

    First results of a new speckle imaging system, the Differential Speckle Survey Instrument, are reported. The instrument is designed to take speckle data in two filters simultaneously with two independent CCD imagers. This feature results in three advantages over other speckle cameras: (1) twice as many frames can be obtained in the same observation time which can increase the signal-to-noise ratio for astrometric measurements, (2) component colors can be derived from a single observation, and (3) the two colors give substantial leverage over atmospheric dispersion, allowing for subdiffraction-limited separations to be measured reliably. Fifty-four observations are reported from the first use of the instrument at the Wisconsin-Indiana-Yale-NOAO 3.5 m Telescope 9 The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatories. in 2008 September, including seven components resolved for the first time. These observations are used to judge the basic capabilities of the instrument.

  3. NASA Names Premier X-Ray Observatory and Schedules Launch

    Science.gov (United States)

    1998-12-01

    NASA's Advanced X-ray Astrophysics Facility has been renamed the Chandra X-ray Observatory in honor of the late Indian-American Nobel laureate, Subrahmanyan Chandrasekhar. The telescope is scheduled to be launched no earlier than April 8, 1999 aboard the Space Shuttle Columbia mission STS-93, commanded by astronaut Eileen Collins. Chandrasekhar, known to the world as Chandra, which means "moon" or "luminous" in Sanskrit, was a popular entry in a recent NASA contest to name the spacecraft. The contest drew more than six thousand entries from fifty states and sixty-one countries. The co-winners were a tenth grade student in Laclede, Idaho, and a high school teacher in Camarillo, CA. The Chandra X-ray Observatory Center (CXC), operated by the Smithsonian Astrophysical Observatory, will control science and flight operations of the Chandra X-ray Observatory for NASA from Cambridge, Mass. "Chandra is a highly appropriate name," said Harvey Tananbaum, Director of the CXC. "Throughout his life Chandra worked tirelessly and with great precision to further our understanding of the universe. These same qualities characterize the many individuals who have devoted much of their careers to building this premier X-ray observatory." "Chandra probably thought longer and deeper about our universe than anyone since Einstein," said Martin Rees, Great Britain's Astronomer Royal. "Chandrasekhar made fundamental contributions to the theory of black holes and other phenomena that the Chandra X-ray Observatory will study. His life and work exemplify the excellence that we can hope to achieve with this great observatory," said NASA Administrator Dan Goldin. Widely regarded as one of the foremost astrophysicists of the 20th century, Chandrasekhar won the Nobel Prize in 1983 for his theoretical studies of physical processes important to the structure and evolution of stars. He and his wife immigrated from India to the U.S. in 1935. Chandrasekhar served on the faculty of the University of

  4. Training Early Career Scientists in Flight Instrument Design Through Experiential Learning: NASA Goddard's Planetary Science Winter School.

    Science.gov (United States)

    Bleacher, L. V.; Lakew, B.; Bracken, J.; Brown, T.; Rivera, R.

    2017-01-01

    The NASA Goddard Planetary Science Winter School (PSWS) is a Goddard Space Flight Center-sponsored training program, managed by Goddard's Solar System Exploration Division (SSED), for Goddard-based postdoctoral fellows and early career planetary scientists. Currently in its third year, the PSWS is an experiential training program for scientists interested in participating on future planetary science instrument teams. Inspired by the NASA Planetary Science Summer School, Goddard's PSWS is unique in that participants learn the flight instrument lifecycle by designing a planetary flight instrument under actual consideration by Goddard for proposal and development. They work alongside the instrument Principal Investigator (PI) and engineers in Goddard's Instrument Design Laboratory (IDL; idc.nasa.gov), to develop a science traceability matrix and design the instrument, culminating in a conceptual design and presentation to the PI, the IDL team and Goddard management. By shadowing and working alongside IDL discipline engineers, participants experience firsthand the science and cost constraints, trade-offs, and teamwork that are required for optimal instrument design. Each PSWS is collaboratively designed with representatives from SSED, IDL, and the instrument PI, to ensure value added for all stakeholders. The pilot PSWS was held in early 2015, with a second implementation in early 2016. Feedback from past participants was used to design the 2017 PSWS, which is underway as of the writing of this abstract.

  5. Semantically-enabled Knowledge Discovery in the Deep Carbon Observatory

    Science.gov (United States)

    Wang, H.; Chen, Y.; Ma, X.; Erickson, J. S.; West, P.; Fox, P. A.

    2013-12-01

    The Deep Carbon Observatory (DCO) is a decadal effort aimed at transforming scientific and public understanding of carbon in the complex deep earth system from the perspectives of Deep Energy, Deep Life, Extreme Physics and Chemistry, and Reservoirs and Fluxes. Over the course of the decade DCO scientific activities will generate a massive volume of data across a variety of disciplines, presenting significant challenges in terms of data integration, management, analysis and visualization, and ultimately limiting the ability of scientists across disciplines to make insights and unlock new knowledge. The DCO Data Science Team (DCO-DS) is applying Semantic Web methodologies to construct a knowledge representation focused on the DCO Earth science disciplines, and use it together with other technologies (e.g. natural language processing and data mining) to create a more expressive representation of the distributed corpus of DCO artifacts including datasets, metadata, instruments, sensors, platforms, deployments, researchers, organizations, funding agencies, grants and various awards. The embodiment of this knowledge representation is the DCO Data Science Infrastructure, in which unique entities within the DCO domain and the relations between them are recognized and explicitly identified. The DCO-DS Infrastructure will serve as a platform for more efficient and reliable searching, discovery, access, and publication of information and knowledge for the DCO scientific community and beyond.

  6. Solaris: a global network of autonomous observatories in the southern hemisphere

    Science.gov (United States)

    Kozłowski, S. K.; Sybilski, P.; Konacki, Maciej; Pawłaszek, R. K.; Ratajczak, Milena; Helminiak, K. G.

    2014-07-01

    We present Project Solaris, a network of four autonomous observatories in the Southern Hemisphere. The Project's primary goal is to detect and characterize circumbinary planets using the eclipse timing approach. This method requires high-cadence and long time-span photometric coverage of the binaries' eclipses, hence the observatories are located at sites having similar separation in longitude and nearly identical latitudes: South African Astronómical Observatory, Republic of South Africa (Solaris-1 and -2), Siding Spring Observatory, Australia (Solaris-3) and Complejo Astronomico El Leoncito, Argentina (Solaris-4). The headquarters coordinating and monitoring the network is based in Toruń, Poland. All four sites are operational as of December 2013. The instrument and hardware configurations are nearly identical. Each site is equipped with a 0.5-m Ritchey-Chrétien or Schmidt-Cassegrain optical tube assembly mounted on a direct-drive modified German equatorial mount along with a set of instruments. Computer, power and networking components are installed in rack cabinets. Everything is housed in sandwiched fiberglass clamshell 3.5-m diameter robotized domes. The Argentinian site is additionally equipped with a 20-ft office container. We discuss the design requirements of robotic observatories aimed to operate autonomously as a global network with concentration on efficiency, robustness and modularity. We also present a newly introduced spectroscopic mode of operation commissioned on the Solaris-1 telescope. Using a compact échelle spectrograph (20 000 resolution) mounted directly on the imaging train of the telescope, we are able to remotely acquire spectra. A fully robotic spectroscopic mode is planned for 2015.

  7. Mars Science Laboratory Using Laser Instrument, Artist's Concept

    Science.gov (United States)

    2007-01-01

    This artist's conception of NASA's Mars Science Laboratory portrays use of the rover's ChemCam instrument to identify the chemical composition of a rock sample on the surface of Mars. ChemCam is innovative for planetary exploration in using a technique referred to as laser breakdown spectroscopy to determine the chemical composition of samples from distances of up to about 8 meters (25 feet) away. ChemCam is led by a team at the Los Alamos National Laboratory and the Centre d'Etude Spatiale des Rayonnements in Toulouse, France. Mars Science Laboratory, a mobile robot for investigating Mars' past or present ability to sustain microbial life, is in development at NASA's Jet Propulsion Laboratory for a launch opportunity in 2009. The mission is managed by JPL, a division of the California Institute of Technology, Pasadena, Calif., for the NASA Science Mission Directorate, Washington.

  8. Big Science

    Energy Technology Data Exchange (ETDEWEB)

    Anon.

    1986-05-15

    Astronomy, like particle physics, has become Big Science where the demands of front line research can outstrip the science budgets of whole nations. Thus came into being the European Southern Observatory (ESO), founded in 1962 to provide European scientists with a major modern observatory to study the southern sky under optimal conditions.

  9. Simultaneous control of multiple instruments at the Advanced Technology Solar Telescope

    Science.gov (United States)

    Johansson, Erik M.; Goodrich, Bret

    2012-09-01

    The Advanced Technology Solar Telescope (ATST) is a 4-meter solar observatory under construction at Haleakala, Hawaii. The simultaneous use of multiple instruments is one of the unique capabilities that makes the ATST a premier ground based solar observatory. Control of the instrument suite is accomplished by the Instrument Control System (ICS), a layer of software between the Observatory Control System (OCS) and the instruments. The ICS presents a single narrow interface to the OCS and provides a standard interface for the instruments to be controlled. It is built upon the ATST Common Services Framework (CSF), an infrastructure for the implementation of a distributed control system. The ICS responds to OCS commands and events, coordinating and distributing them to the various instruments while monitoring their progress and reporting the status back to the OCS. The ICS requires no specific knowledge about the instruments. All information about the instruments used in an experiment is passed by the OCS to the ICS, which extracts and forwards the parameters to the appropriate instrument controllers. The instruments participating in an experiment define the active instrument set. A subset of those instruments must complete their observing activities in order for the experiment to be considered complete and are referred to as the must-complete instrument set. In addition, instruments may participate in eavesdrop mode, outside of the control of the ICS. All instrument controllers use the same standard narrow interface, which allows new instruments to be added without having to modify the interface or any existing instrument controllers.

  10. Observatory Sponsoring Astronomical Image Contest

    Science.gov (United States)

    2005-05-01

    Forget the headphones you saw in the Warner Brothers thriller Contact, as well as the guttural throbs emanating from loudspeakers at the Very Large Array in that 1997 movie. In real life, radio telescopes aren't used for "listening" to anything - just like visible-light telescopes, they are used primarily to make images of astronomical objects. Now, the National Radio Astronomy Observatory (NRAO) wants to encourage astronomers to use radio-telescope data to make truly compelling images, and is offering cash prizes to winners of a new image contest. Radio Galaxy Fornax A Radio Galaxy Fornax A Radio-optical composite image of giant elliptical galaxy NGC 1316, showing the galaxy (center), a smaller companion galaxy being cannibalized by NGC 1316, and the resulting "lobes" (orange) of radio emission caused by jets of particles spewed from the core of the giant galaxy Click on image for more detail and images CREDIT: Fomalont et al., NRAO/AUI/NSF "Astronomy is a very visual science, and our radio telescopes are capable of producing excellent images. We're sponsoring this contest to encourage astronomers to make the extra effort to turn good images into truly spectacular ones," said NRAO Director Fred K.Y. Lo. The contest, offering a grand prize of $1,000, was announced at the American Astronomical Society's meeting in Minneapolis, Minnesota. The image contest is part of a broader NRAO effort to make radio astronomical data and images easily accessible and widely available to scientists, students, teachers, the general public, news media and science-education professionals. That effort includes an expanded image gallery on the observatory's Web site. "We're not only adding new radio-astronomy images to our online gallery, but we're also improving the organization and accessibility of the images," said Mark Adams, head of education and public outreach (EPO) at NRAO. "Our long-term goal is to make the NRAO Image Gallery an international resource for radio astronomy imagery

  11. Exploring the Digital Universe with Europe's Astrophysical Virtual Observatory

    Science.gov (United States)

    2001-12-01

    digitally reconstructed in the databanks! The richness and complexity of data and information available to the astronomers is overwhelming. This has created a major problem as to how astronomers can manage, distribute and analyse this great wealth of data . The Astrophysical Virtual Observatory (AVO) will allow astronomers to overcome the challenges and enable them to "put the Universe online". AVO is supported by the European Commission The AVO is a three-year project, funded by the European Commission under its Research and Technological Development (RTD) scheme, to design and implement a virtual observatory for the European astronomical community. The European Commission awarded a contract valued at 4 million Euro for the AVO project , starting 15 November 2001. AVO will provide software tools to enable astronomers to access the multi-wavelength data archives over the Internet and so give them the capability to resolve fundamental questions about the Universe by probing the digital sky. Equivalent searches of the 'real' sky would, in comparison, be both costly and take far too long. Towards a Global Virtual Observatory The need for virtual observatories has also been recognised by other astronomical communities. The National Science Foundation in the USA has awarded 10 million Dollar (approx. 11.4 million Euro) for a National Virtual Observatory (NVO). The AVO project team has formed a close alliance with the NVO and both teams have representatives on their respective committees. It is clear to the NVO and AVO communities that there are no intrinsic boundaries to the virtual observatory concept and that all astronomers should be working towards a truly global virtual observatory that will enable new science to be carried out on the wealth of astronomical data held in the growing number of first class international astronomical archives. The AVO involves six partner organisations led by the European Southern Observatory (ESO) in Munich (Germany). The other partner

  12. MMT OBSERVATORY 6.5M CLIO RAW DATA OBSERVATIONS OF LCROSS

    Data.gov (United States)

    National Aeronautics and Space Administration — This archive contains raw observations of the 2009-10-09 impact of the LCROSS spacecraft on the moon by the CLIO instrument on the MMT Observatory 6.5m telescope....

  13. The design and implementation of the Dynamic Ionosphere Cubesat Experiment (DICE) science instruments

    Science.gov (United States)

    Burr, Steven Reed

    Dynamic Ionosphere Cubesat Experiment (DICE) is a satellite project funded by the National Science Foundation (NSF) to study the ionosphere, more particularly Storm Enhanced Densities (SED) with a payload consisting of plasma diagnostic instrumentation. Three instruments onboard DICE include an Electric Field Probe (EFP), Ion Langmuir Probe (ILP), and Three Axis Magnetometer (TAM). The EFP measures electric fields from +/-8V and consists of three channels a DC to 40Hz channel, a Floating Potential Probe (FPP), and an spectrographic channel with four bands from 16Hz to 512Hz. The ILP measures plasma densities from 1x104 cm--3 to 2x107 cm--3. The TAM measures magnetic field strength with a range +/-0.5 Gauss with a sensitivity of 2nT. To achieve desired mission requirements careful selection of instrument requirements and planning of the instrumentation design to achieve mission success. The analog design of each instrument is described in addition to the digital framework required to sample the science data at a 70Hz rate and prepare the data for the Command and Data Handing (C&DH) system. Calibration results are also presented and show fulfillment of the mission and instrumentation requirements.

  14. Status And Performance Of The Virgin Islands Robotic Telescope at Etelman Observatory

    Science.gov (United States)

    Morris, David C.; Gendre, Bruce; Neff, James E.; Giblin, Timothy W.

    2016-01-01

    The Virgin Islands Robotic Telescope is an 0.5m robotic telescope located at the easternmost and southernmost optical observatory in the United States at a latitude of 18.5N and longitude of 65W. The observatory is located on the island of St Thomas in the USVI. Astronomers from the College of Charleston, the US Air Force Academy, and the University of the Virgin Islands collaborate to maintain and operate the facility. The primary scientific focus of the facility is the optical follow-up of high-energy transients though a variety of other science interests are also being pursued including follow-up of candidate extra-solar planets, rotation studies of cool stars, and near-Earth asteroid and space situational awareness studies. The facility also supports a wide-reaching education and outreach program dedicated to raising the level of STEAM engagement and enrichment in the USVI. We detail the characteristics, capabilities, and early results from the observatory. The observatory is growing its staff and science activities and potential topics for collaboration will be discussed.

  15. Sierra Stars Observatory Network: An Accessible Global Network

    Science.gov (United States)

    Williams, Richard; Beshore, Edward

    2011-03-01

    The Sierra Stars Observatory Network (SSON) is a unique partnership among professional observatories that provides its users with affordable high-quality calibrated image data. SSON comprises observatories in the Northern and Southern Hemisphere and is in the process of expanding to a truly global network capable of covering the entire sky 24 hours a day in the near future. The goal of SSON is to serve the needs of science-based projects and programs. Colleges, universities, institutions, and individuals use SSON for their education and research projects. The mission of SSON is to promote and expand the use of its facilities among the thousands of colleges and schools worldwide that do not have access to professional-quality automated observatory systems to use for astronomy education and research. With appropriate leadership and guidance educators can use SSON to help teach astronomy and do meaningful scientific projects. The relatively small cost of using SSON for this type of work makes it affordable and accessible for educators to start using immediately. Remote observatory services like SSON need to evolve to better support education and research initiatives of colleges, institutions and individual investigators. To meet these needs, SSON is developing a sophisticated interactive scheduling system to integrate among the nodes of the observatory network. This will enable more dynamic observations, including immediate priority interrupts, acquiring moving objects using ephemeris data, and more.

  16. System Definition of the James Webb Space Telescope (JWST) Integrated Science Instrument Module (ISIM)

    Science.gov (United States)

    Lundquist, Ray; Aymergen, Cagatay; VanCampen, Julie; Abell, James; Smith, Miles; Driggers, Phillip

    2008-01-01

    The Integrated Science Instrument Module (ISIM) for the James Webb Space Telescope (JWST) provides the critical functions and the environment for the four science instruments on JWST. This complex system development across many international organizations presents unique challenges and unique solutions. Here we describe how the requirement flow has been coordinated through the documentation system, how the tools and processes are used to minimize impact to the development of the affected interfaces, how the system design has matured, how the design review process operates, and how the system implementation is managed through reporting to ensure a truly world class scientific instrument compliment is created as the final product.

  17. The James Webb Space Telescope's Plan for Operations and Instrument Capabilities for Observations in the Solar System

    Science.gov (United States)

    Milam, Stefanie N.; Stansberry, John A.; Sonneborn, George; Thomas, Cristina

    2016-01-01

    The James Webb Space Telescope (JWST) is optimized for observations in the near- and mid-infrared and will provide essential observations for targets that cannot be conducted from the ground or other missions during its lifetime. The state-of-the-art science instruments, along with the telescope's moving target tracking, will enable the infrared study, with unprecedented detail, for nearly every object (Mars and beyond) in the Solar System. The goals of this special issue are to stimulate discussion and encourage participation in JWST planning among members of the planetary science community. Key science goals for various targets, observing capabilities for JWST, and highlights for the complementary nature with other missions/observatories are described in this paper.

  18. Development and Validation of an Instrument to Measure Students' Motivation and Self-Regulation in Science Learning

    Science.gov (United States)

    Velayutham, Sunitadevi; Aldridge, Jill; Fraser, Barry

    2011-10-01

    Students' motivational beliefs and self-regulatory practices have been identified as instrumental in influencing the engagement of students in the learning process. An important aim of science education is to empower students by nurturing the belief that they can succeed in science learning and to cultivate the adaptive learning strategies required to help to bring about that success. This article reports the development and validation of an instrument to measure salient factors related to the motivation and self-regulation of students in lower secondary science classrooms. The development of the instrument involved identifying key determinants of students' motivation and self-regulation in science learning based on theoretical and research underpinnings. Once the instrument was developed, a pilot study involving 52 students from two Grade 8 science classes was undertaken. Quantitative data were collected from 1,360 students in 78 classes across Grades 8, 9, and 10, in addition to in-depth qualitative information gathered from 10 experienced science teachers and 12 Grade 8 students. Analyses of the data suggest that the survey has strong construct validity when used with lower secondary students. This survey could be practically valuable as a tool for gathering information that may guide classroom teachers in refocusing their teaching practices and help to evaluate the effectiveness of intervention programmes.

  19. NASA's Earth Observatory: 16 Years of Communicating with and for Scientists

    Science.gov (United States)

    Ward, K.; Carlowicz, M. J.; Allen, J.; Voiland, A.; Przyborski, P.; Hansen, K.; Stevens, J.

    2015-12-01

    For the past 16 years NASA's Earth Observatory website has featured stories that are driven by strong visualization and in-depth reporting and storytelling. The Earth Observatory Image of the Day is published 365 days a year and is a syndication staple for major news outlets, science-related publications, blogs and social media outlets. The daily publication pace requires that we cover a wide range of topics within NASA's portfolio of Earth science research. To meet our deadlines, and to do so competently and with the authority that a NASA-branded publication warrants, we have developed relationships with scientists from throughout the agency who both provide us with ideas for stories and review our content for accuracy. This symbiotic relationship insures that the Earth Observatory has a quality product that is syndicated, repurposed and sourced throughout popular media, resulting in science content reaching the public that might not otherwise be reported. We will discuss how we have developed our relationships and processes over the years, how we work with scientists to see the potential stories in their data, and how we package and promote these stories and visualizations for maximum exposure and reuse.

  20. Addressing the social dimensions of citizen observatories: The Ground Truth 2.0 socio-technical approach for sustainable implementation of citizen observatories

    Science.gov (United States)

    Wehn, Uta; Joshi, Somya; Pfeiffer, Ellen; Anema, Kim; Gharesifard, Mohammad; Momani, Abeer

    2017-04-01

    Owing to ICT-enabled citizen observatories, citizens can take on new roles in environmental monitoring, decision making and co-operative planning, and environmental stewardship. And yet implementing advanced citizen observatories for data collection, knowledge exchange and interactions to support policy objectives is neither always easy nor successful, given the required commitment, trust, and data reliability concerns. Many efforts are facing problems with the uptake and sustained engagement by citizens, limited scalability, unclear long-term sustainability and limited actual impact on governance processes. Similarly, to sustain the engagement of decision makers in citizen observatories, mechanisms are required from the start of the initiative in order to have them invest in and, hence, commit to and own the entire process. In order to implement sustainable citizen observatories, these social dimensions therefore need to be soundly managed. We provide empirical evidence of how the social dimensions of citizen observatories are being addressed in the Ground Truth 2.0 project, drawing on a range of relevant social science approaches. This project combines the social dimensions of citizen observatories with enabling technologies - via a socio-technical approach - so that their customisation and deployment is tailored to the envisaged societal and economic impacts of the observatories. The projects consists of the demonstration and validation of six scaled up citizen observatories in real operational conditions both in the EU and in Africa, with a specific focus on flora and fauna as well as water availability and water quality for land and natural resources management. The demonstration cases (4 EU and 2 African) cover the full 'spectrum' of citizen-sensed data usage and citizen engagement, and therefore allow testing and validation of the socio-technical concept for citizen observatories under a range of conditions.

  1. Astronomy from the Moon and International Lunar Observatory Missions

    Science.gov (United States)

    Durst, S.; Takahashi, Y. D.

    2018-04-01

    Astronomy from the Moon provides a promising new frontier for 21st century astrophysics and related science activity. International Lunar Observatory Association is an enterprise advancing missions to the Moon for observation and communication.

  2. The Second Flight of the Sunrise Balloon-borne Solar Observatory: Overview of Instrument Updates, the Flight, the Data, and First Results

    Energy Technology Data Exchange (ETDEWEB)

    Solanki, S. K.; Riethmüller, T. L.; Barthol, P.; Danilovic, S.; Deutsch, W.; Doerr, H.-P.; Feller, A.; Gandorfer, A.; Germerott, D.; Gizon, L.; Grauf, B.; Heerlein, K.; Hirzberger, J.; Kolleck, M.; Lagg, A.; Meller, R.; Tomasch, G.; Noort, M. van [Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, D-37077 Göttingen (Germany); Rodríguez, J. Blanco; Blesa, J. L. Gasent, E-mail: solanki@mps.mpg.de [Grupo de Astronomía y Ciencias del Espacio, Universidad de Valencia, E-46980 Paterna, Valencia (Spain); and others

    2017-03-01

    The Sunrise balloon-borne solar observatory, consisting of a 1 m aperture telescope that provides a stabilized image to a UV filter imager and an imaging vector polarimeter, carried out its second science flight in 2013 June. It provided observations of parts of active regions at high spatial resolution, including the first high-resolution images in the Mg ii k line. The obtained data are of very high quality, with the best UV images reaching the diffraction limit of the telescope at 3000 Å after Multi-Frame Blind Deconvolution reconstruction accounting for phase-diversity information. Here a brief update is given of the instruments and the data reduction techniques, which includes an inversion of the polarimetric data. Mainly those aspects that evolved compared with the first flight are described. A tabular overview of the observations is given. In addition, an example time series of a part of the emerging active region NOAA AR 11768 observed relatively close to disk center is described and discussed in some detail. The observations cover the pores in the trailing polarity of the active region, as well as the polarity inversion line where flux emergence was ongoing and a small flare-like brightening occurred in the course of the time series. The pores are found to contain magnetic field strengths ranging up to 2500 G, and while large pores are clearly darker and cooler than the quiet Sun in all layers of the photosphere, the temperature and brightness of small pores approach or even exceed those of the quiet Sun in the upper photosphere.

  3. Astronomy in Research-Based Science Education (A-RBSE): A Review of a Decade of Professional Development Programs in Support of Teacher and Student Research at the National Optical Astronomy Observatory

    Science.gov (United States)

    Pompea, S. M.; Garmany, C. D.; Walker, C. E.; Croft, S. K.

    2006-12-01

    We will review the evolution of the Research Based Science Education (RBSE) and Teacher Leaders in Research Based Science (TLRBSE) programs at the National Optical Astronomy Observatory over the last eleven years. The program has evolved from an NSF-funded program in teacher enhancement to an observatory-supported core education initiative. The present manifestation of our program is an umbrella of programs designed to aid teachers in doing research with astronomical data archives, small telescopes, large research-grade telescopes, and the Spitzer Space Telescope. The professional development program has addressed basic questions on the nature of research, best techniques to bring it into the classroom, the value of authentic research, and the mix of on-line versus in- person professional development. The current program is used to test new models of teacher professional development that for outreach programs for the Large Synoptic Survey Telescope program, the Thirty-Meter Telescope program, and the National Virtual Observatory program. We will describe a variety of lessons learned (and relearned) and try to describe best practices in promoting teacher and student research. The TLRBSE Program has been funded by the National Science Foundation under ESI 0101982, funded through the AURA/NSF Cooperative Agreement AST-9613615. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under cooperative agreement with the National Science Foundation.

  4. The Impact of an Authentic Science Experience on STEM Identity: A Preliminary Analysis of YouthAstroNet and MicroObservatory Telescope Network Participant Data

    Science.gov (United States)

    Dussault, Mary E.; Wright, Erika A.; Sadler, Philip; Sonnert, Gerhard; ITEAMS II Team

    2018-01-01

    Encouraging students to pursue careers in science, technology, engineering, and mathematics (STEM) is a high priority for national K-12 education improvement initiatives in the United States. Many educators have claimed that a promising strategy for nurturing early student interest in STEM is to engage them in authentic inquiry experiences. “Authentic” refers to investigations in which the questions are of genuine interest and importance to students, and the inquiry more closely resembles the way real science is done. Science education researchers and practitioners at the Harvard-Smithsonian Center for Astrophysics have put this theory into action with the development of YouthAstroNet, a nationwide online learning community of middle-school aged students, educators, and STEM professionals that features the MicroObservatory Robotic Telescope Network, professional image analysis software, and complementary curricula for use in a variety of learning settings. This preliminary study examines factors that influence YouthAstroNet participants' Science Affinity, STEM Identity, and STEM Career Interest, using the matched pre/post survey results of 261 participants as the data source. The pre/post surveys included some 40 items measuring affinity, identity, knowledge, and career interest. In addition, the post intervention instrument included a number of items in which students reported the instructional strategies they experienced as part of the program. A simple analysis of pre-post changes in affinity and interest revealed very little significant change, and for those items where a small pre-post effect was observed, the average change was most often negative. However, after accounting for students' different program treatment experiences and for their prior attitudes and interests, a predictor of significant student gains in Affinity, STEM Identity, Computer/Math Identity, and STEM Career Interest could be identified. This was the degree to which students reported

  5. OZCAR: the French network of Critical Zone Observatories: principles and scientific objectives

    Science.gov (United States)

    Braud, Isabelle; Gaillardet, Jérôme; Hankard, Fatim; Le Borgne, Tanguy; Nord, Guillaume; Six, Delphine; Galy, Catherine; Laggoun-Défarge, Fatima; Tallec, Tiphaine; Pauwels, Hélène

    2017-04-01

    This contribution aims at presenting the principles that underlined the creation of the OZCAR research infrastructure, gathering various Critical Zone Observatories in France, and the scientific questions that drives the observation settings. The Critical Zone includes the fine zone between the lower atmosphere at the top of the canopy down to the bedrock-soil interface. This lithosphere-atmosphere boundary is critical for the availability of life-sustaining resources and critical for humanity because this is the zone where we live, where we build our cities, from which we extract our food and our water and where we release most of our wastes. This is the fragile zone on which the natural ecosystem relies because this is where nutrients are being released from the rocks. OZCAR is a distributed research infrastructure gathering instrumented sites and catchments on continental surfaces all dedicated to the observation and monitoring of the different compartments of the Critical Zone at the national scale. All these observatories (more that 40) were all built up on specific questions (acid deposition, flood prediction, urban hydrology…), some of them more than 50 years ago, but they have all in common to be highly instrumented, permanently funded as infrastructures. They all share the same overarching goal of understanding and predicting the Critical Zone in a changing world. OZCAR gathers instrumented catchments, hydrogeological sites, peatlands, glacier and permafrost regions and a spatial observatory under the common umbrella of understanding water and biogeochemical cycles and the associated fluxes of energy by using natural gradients and experimentation. Based on the collaboration with Southern Countries, OZCAR's sites have a global coverage including tropical areas and high mountainous regions in the Andes and the Himalaya. OZCAR benefits from a French investments project called CRITEX (Innovative equipment for the critical zone, https://www.critex.fr/critex-3

  6. Saint Petersburg magnetic observatory: from Voeikovo subdivision to INTERMAGNET certification

    Science.gov (United States)

    Sidorov, Roman; Soloviev, Anatoly; Krasnoperov, Roman; Kudin, Dmitry; Grudnev, Andrei; Kopytenko, Yury; Kotikov, Andrei; Sergushin, Pavel

    2017-11-01

    Since June 2012 the Saint Petersburg magnetic observatory is being developed and maintained by two institutions of the Russian Academy of Sciences (RAS) - the Geophysical Center of RAS (GC RAS) and the Saint Petersburg branch of the Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation of RAS (IZMIRAN SPb). On 29 April 2016 the application of the Saint Petersburg observatory (IAGA code SPG) for introduction into the INTERMAGNET network was accepted after approval by the experts of the first definitive dataset over 2015, produced by the GC RAS, and on 9 June 2016 the SPG observatory was officially certified. One of the oldest series of magnetic observations, originating in 1834, was resumed in the 21st century, meeting the highest quality standards and all modern technical requirements. In this paper a brief historical and scientific background of the SPG observatory foundation and development is given, the stages of its renovation and upgrade in the 21st century are described, and information on its current state is provided. The first results of the observatory functioning are discussed and geomagnetic variations registered at the SPG observatory are assessed and compared with geomagnetic data from the INTERMAGNET observatories located in the same region.

  7. Saint Petersburg magnetic observatory: from Voeikovo subdivision to INTERMAGNET certification

    Directory of Open Access Journals (Sweden)

    R. Sidorov

    2017-11-01

    Full Text Available Since June 2012 the Saint Petersburg magnetic observatory is being developed and maintained by two institutions of the Russian Academy of Sciences (RAS – the Geophysical Center of RAS (GC RAS and the Saint Petersburg branch of the Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation of RAS (IZMIRAN SPb. On 29 April 2016 the application of the Saint Petersburg observatory (IAGA code SPG for introduction into the INTERMAGNET network was accepted after approval by the experts of the first definitive dataset over 2015, produced by the GC RAS, and on 9 June 2016 the SPG observatory was officially certified. One of the oldest series of magnetic observations, originating in 1834, was resumed in the 21st century, meeting the highest quality standards and all modern technical requirements. In this paper a brief historical and scientific background of the SPG observatory foundation and development is given, the stages of its renovation and upgrade in the 21st century are described, and information on its current state is provided. The first results of the observatory functioning are discussed and geomagnetic variations registered at the SPG observatory are assessed and compared with geomagnetic data from the INTERMAGNET observatories located in the same region.

  8. Development of Armenian-Georgian Virtual Observatory

    Science.gov (United States)

    Mickaelian, Areg; Kochiashvili, Nino; Astsatryan, Hrach; Harutyunian, Haik; Magakyan, Tigran; Chargeishvili, Ketevan; Natsvlishvili, Rezo; Kukhianidze, Vasil; Ramishvili, Giorgi; Sargsyan, Lusine; Sinamyan, Parandzem; Kochiashvili, Ia; Mikayelyan, Gor

    2009-10-01

    The Armenian-Georgian Virtual Observatory (ArGVO) project is the first initiative in the world to create a regional VO infrastructure based on national VO projects and regional Grid. The Byurakan and Abastumani Astrophysical Observatories are scientific partners since 1946, after establishment of the Byurakan observatory . The Armenian VO project (ArVO) is being developed since 2005 and is a part of the International Virtual Observatory Alliance (IVOA). It is based on the Digitized First Byurakan Survey (DFBS, the digitized version of famous Markarian survey) and other Armenian archival data. Similarly, the Georgian VO will be created to serve as a research environment to utilize the digitized Georgian plate archives. Therefore, one of the main goals for creation of the regional VO is the digitization of large amounts of plates preserved at the plate stacks of these two observatories. The total amount of plates is more than 100,000 units. Observational programs of high importance have been selected and some 3000 plates will be digitized during the next two years; the priority is being defined by the usefulness of the material for future science projects, like search for new objects, optical identifications of radio, IR, and X-ray sources, study of variability and proper motions, etc. Having the digitized material in VO standards, a VO database through the regional Grid infrastructure will be active. This partnership is being carried out in the framework of the ISTC project A-1606 "Development of Armenian-Georgian Grid Infrastructure and Applications in the Fields of High Energy Physics, Astrophysics and Quantum Physics".

  9. The Einstein Observatory: A New Public/Private Observatory Complex for Community Education and Scientific Research

    Science.gov (United States)

    Sowell, J.

    1999-12-01

    The Development Authority of Cherokee County (Georgia) is leading a public/private partnership of business/industry professionals, educators, and university scientists that seeks to develop a national prototype educational and scientific research facility for grades K-12, as well as college-level research, that will inspire our youth to become literate in science and technology. In particular, the goal is to make this complex a science, math, and engineering magnet learning facility and to raise the average SAT scores of local area students by 100 points. A dark-site mountain, nestled on the foothills of the Blue Ridge Mountains at the northern-most edge of Atlanta, will become the home for the "Einstein" Observatory. The complex will have four telescopes: one 50-inch, one 24-inch, and two 16-inch telescopes. Each telescope will have digital cameras and an optic-fiber feed to a single, medium-resolution spectroscope. All four telescopes will be electronically accessible from local schools. Professional astronomers will establish suitable observational research projects and will lead K-12 and college students in the acquisition and analysis of data. Astronomers will also assist the local area schoolteachers in methods for nurturing children's scientific inquiry. The observatory mountain will have 100 platform locations for individual viewing by visiting families, school groups, and amateur astronomers. The Atlanta Astronomer Club will provide numerous evening programs and viewing opportunities for the general public. An accompanying Planetarium & Science Center will be located on the nearby campus of Reinhardt College. The Planetarium & Science Center will be integrated with Reinhardt College's theme of learning focused upon studying the past and present as a basis for projecting the future.

  10. `Science to the Glory of God'. The Popular Science Magazine Ibérica and its Coverage of Radioactivity, 1914-1936

    Science.gov (United States)

    Herran, Néstor

    2012-03-01

    This paper provides a first approach to the history of Ibérica, one of the most important popular science magazines published in Spain before the Civil War. Founded in 1914 by members of the Society of Jesus based at the Ebro Observatory, Ibérica reached a weekly circulation of about 10,000 in the mid 1920s, and was instrumental in extending science education in Jesuit education facilities and in developing a "reactionary modernist" culture that embraced Catholicism and modernisation. By focusing on its coverage of radioactivity and the radium industry, the article aims to examine the magazine's popularising style and ideology, and to determine its role in the debates regarding the cultural value of science in the first decades of twentieth century Spain.

  11. Ground Validation Assessments of GPM Core Observatory Science Requirements

    Science.gov (United States)

    Petersen, Walt; Huffman, George; Kidd, Chris; Skofronick-Jackson, Gail

    2017-04-01

    NASA Global Precipitation Measurement (GPM) Mission science requirements define specific measurement error standards for retrieved precipitation parameters such as rain rate, raindrop size distribution, and falling snow detection on instantaneous temporal scales and spatial resolutions ranging from effective instrument fields of view [FOV], to grid scales of 50 km x 50 km. Quantitative evaluation of these requirements intrinsically relies on GPM precipitation retrieval algorithm performance in myriad precipitation regimes (and hence, assumptions related to physics) and on the quality of ground-validation (GV) data being used to assess the satellite products. We will review GPM GV products, their quality, and their application to assessing GPM science requirements, interleaving measurement and precipitation physical considerations applicable to the approaches used. Core GV data products used to assess GPM satellite products include 1) two minute and 30-minute rain gauge bias-adjusted radar rain rate products and precipitation types (rain/snow) adapted/modified from the NOAA/OU multi-radar multi-sensor (MRMS) product over the continental U.S.; 2) Polarimetric radar estimates of rain rate over the ocean collected using the K-Pol radar at Kwajalein Atoll in the Marshall Islands and the Middleton Island WSR-88D radar located in the Gulf of Alaska; and 3) Multi-regime, field campaign and site-specific disdrometer-measured rain/snow size distribution (DSD), phase and fallspeed information used to derive polarimetric radar-based DSD retrievals and snow water equivalent rates (SWER) for comparison to coincident GPM-estimated DSD and precipitation rates/types, respectively. Within the limits of GV-product uncertainty we demonstrate that the GPM Core satellite meets its basic mission science requirements for a variety of precipitation regimes. For the liquid phase, we find that GPM radar-based products are particularly successful in meeting bias and random error requirements

  12. Designing a network of critical zone observatories to explore the living skin of the terrestrial Earth

    Directory of Open Access Journals (Sweden)

    S. L. Brantley

    2017-12-01

    Full Text Available The critical zone (CZ, the dynamic living skin of the Earth, extends from the top of the vegetative canopy through the soil and down to fresh bedrock and the bottom of the groundwater. All humans live in and depend on the CZ. This zone has three co-evolving surfaces: the top of the vegetative canopy, the ground surface, and a deep subsurface below which Earth's materials are unweathered. The network of nine CZ observatories supported by the US National Science Foundation has made advances in three broad areas of CZ research relating to the co-evolving surfaces. First, monitoring has revealed how natural and anthropogenic inputs at the vegetation canopy and ground surface cause subsurface responses in water, regolith structure, minerals, and biotic activity to considerable depths. This response, in turn, impacts aboveground biota and climate. Second, drilling and geophysical imaging now reveal how the deep subsurface of the CZ varies across landscapes, which in turn influences aboveground ecosystems. Third, several new mechanistic models now provide quantitative predictions of the spatial structure of the subsurface of the CZ.Many countries fund critical zone observatories (CZOs to measure the fluxes of solutes, water, energy, gases, and sediments in the CZ and some relate these observations to the histories of those fluxes recorded in landforms, biota, soils, sediments, and rocks. Each US observatory has succeeded in (i synthesizing research across disciplines into convergent approaches; (ii providing long-term measurements to compare across sites; (iii testing and developing models; (iv collecting and measuring baseline data for comparison to catastrophic events; (v stimulating new process-based hypotheses; (vi catalyzing development of new techniques and instrumentation; (vii informing the public about the CZ; (viii mentoring students and teaching about emerging multidisciplinary CZ science; and (ix discovering new insights about the CZ. Many

  13. Designing a network of critical zone observatories to explore the living skin of the terrestrial Earth

    Science.gov (United States)

    Brantley, Susan L.; McDowell, William H.; Dietrich, William E.; White, Timothy S.; Kumar, Praveen; Anderson, Suzanne P.; Chorover, Jon; Lohse, Kathleen Ann; Bales, Roger C.; Richter, Daniel D.; Grant, Gordon; Gaillardet, Jérôme

    2017-12-01

    The critical zone (CZ), the dynamic living skin of the Earth, extends from the top of the vegetative canopy through the soil and down to fresh bedrock and the bottom of the groundwater. All humans live in and depend on the CZ. This zone has three co-evolving surfaces: the top of the vegetative canopy, the ground surface, and a deep subsurface below which Earth's materials are unweathered. The network of nine CZ observatories supported by the US National Science Foundation has made advances in three broad areas of CZ research relating to the co-evolving surfaces. First, monitoring has revealed how natural and anthropogenic inputs at the vegetation canopy and ground surface cause subsurface responses in water, regolith structure, minerals, and biotic activity to considerable depths. This response, in turn, impacts aboveground biota and climate. Second, drilling and geophysical imaging now reveal how the deep subsurface of the CZ varies across landscapes, which in turn influences aboveground ecosystems. Third, several new mechanistic models now provide quantitative predictions of the spatial structure of the subsurface of the CZ.Many countries fund critical zone observatories (CZOs) to measure the fluxes of solutes, water, energy, gases, and sediments in the CZ and some relate these observations to the histories of those fluxes recorded in landforms, biota, soils, sediments, and rocks. Each US observatory has succeeded in (i) synthesizing research across disciplines into convergent approaches; (ii) providing long-term measurements to compare across sites; (iii) testing and developing models; (iv) collecting and measuring baseline data for comparison to catastrophic events; (v) stimulating new process-based hypotheses; (vi) catalyzing development of new techniques and instrumentation; (vii) informing the public about the CZ; (viii) mentoring students and teaching about emerging multidisciplinary CZ science; and (ix) discovering new insights about the CZ. Many of these

  14. A small Internet controllable observatory for research and education at the University of North Dakota

    Science.gov (United States)

    Hardersen, P. S.; de Silva, S.; Reddy, V.; Cui, P.; Kumar, S.; Gaffey, M. J.

    2006-06-01

    One of the challenges in astronomy education today is to introduce college students to the real-world practice and science of observational astronomy. Along with a good theoretical background, college students can gain an earlier, deeper understanding of the astronomy profession through direct observational and data reduction experience. However, building and managing a modest observatory is still too costly for many colleges and universities. Fortunately, advances in commercial astronomical hardware and software now allow universities to build and operate small Internet controllable observatories for a modest investment. The advantages of an Internet observatory include: 1) remote operation from a comfortable location, 2) immediate data access, 3) telescope control via a web browser, and 4) allowing both on-campus and distance education students the ability to conduct a variety of observing projects. Internet capabilities vastly expand the number of students who will be able to use the observatory, thus exposing them to astronomy as a science and as a potential career. In September 2005, the University of North Dakota (UND) Department of Space Studies began operating a small, recently renovated Internet controllable observatory. Housed within a roll-off roof 10 miles west of UND, the observatory includes a Meade 16-inch, f/10 Schmidt-Cassegrain telescope, an SBIG STL-6303e CCD with broadband filters, ACP observatory control software, focuser, and associated equipment. The observatory cost \\25,000 to build in 1996; 2005 renovation costs total \\28,000. An observatory operator prepares the telescope for use each night. Through remote operation, the roof is opened and the telescope/CCD power is turned on. The telescope is then aligned and focused before allowing students to access the observatory. Students communicate with the observatory operator via an online chat room and via telephone, if necessary, to answer questions and resolve any problems. Additional

  15. The Aula Espazio Gela Observatory: A tool for Solar System Education and Outreach

    Science.gov (United States)

    Rojas, J. F.; Perez-Hoyos, S.; Hueso, R.; Mendikoa, I.; Sanchez-Lavega, A.

    2011-10-01

    We present a summary of the activities undertaken over the first year of operations of the "Aula Espazio Gela Observatory", with teaching and astronomy outreach purposes. The observatory belongs to the Universidad del País Vasco and is a fundamental part of the "Master en Ciencia y Tecnología Espacial" (Space Science and Technology master). It is an urban observatory with the dome located on the roof of the School of Engineering at the Universidad del Pais Vasco in Bilbao (Spain).

  16. Recent results from the Compton Observatory

    Energy Technology Data Exchange (ETDEWEB)

    Michelson, P.F.; Hansen, W.W. [Stanford Univ., CA (United States)

    1994-12-01

    The Compton Observatory is an orbiting astronomical observatory for gamma-ray astronomy that covers the energy range from about 30 keV to 30 GeV. The Energetic Gamma Ray Experiment Telescope (EGRET), one of four instruments on-board, is capable of detecting and imaging gamma radiation from cosmic sources in the energy range from approximately 20 MeV to 30 GeV. After about one month of tests and calibration following the April 1991 launch, a 15-month all sky survey was begun. This survey is now complete and the Compton Observatory is well into Phase II of its observing program which includes guest investigator observations. Among the highlights from the all-sky survey discussed in this presentation are the following: detection of five pulsars with emission above 100 MeV; detection of more than 24 active galaxies, the most distant at redshift greater than two; detection of many high latitude, unidentified gamma-ray sources, some showing significant time variability; detection of at least two high energy gamma-ray bursts, with emission in one case extending to at least 1 GeV. EGRET has also detected gamma-ray emission from solar flares up to energies of at least 2 GeV and has observed gamma-rays from the Large Magellanic Cloud.

  17. ISO science - observations of dusty discs.

    Science.gov (United States)

    Heske, A.

    1992-12-01

    ISO, the Infrared Space Observatory, will be an infrared observing facility in space. Via submission of observing proposals, use of this facility will be open to the astronomical community. The scientific payload consists of two spectrometers, a camera and a photo-polarimeter. Following an overview of the ISO mission, this paper describes the highlights of the Central Programme - proposals which are being prepared by the instrument groups, the mission scientists and the astronomers of the ISO Science Operations Team - with special emphasis on the proposals concerned with dusty discs.

  18. The Infrared-Optical Telescope (IRT) of the Exist Observatory

    Science.gov (United States)

    Kutyrev, Alexander; Bloom, Joshua; Gehrels, Neil; Golisano, Craig; Gong, Quan; Grindlay, Jonathan; Moseley, Samuel; Woodgate, Bruce

    2010-01-01

    The IRT is a 1.1m visible and infrared passively cooled telescope, which can locate, identify and obtain spectra of GRB afterglows at redshifts up to z 20. It will also acquire optical-IR, imaging and spectroscopy of AGN and transients discovered by the EXIST (The Energetic X-ray Imaging Survey Telescope). The IRT imaging and spectroscopic capabilities cover a broad spectral range from 0.32.2m in four bands. The identical fields of view in the four instrument bands are each split in three subfields: imaging, objective prism slitless for the field and objective prism single object slit low resolution spectroscopy, and high resolution long slit on single object. This allows the instrument, to do simultaneous broadband photometry or spectroscopy of the same object over the full spectral range, thus greatly improving the efficiency of the observatory and its detection limits. A prompt follow up (within three minutes) of the transient discovered by the EXIST makes IRT a unique tool for detection and study of these events, which is particularly valuable at wavelengths unavailable to the ground based observatories.

  19. Development and Large-Scale Validation of an Instrument to Assess Arabic-Speaking Students' Attitudes Toward Science

    Science.gov (United States)

    Abd-El-Khalick, Fouad; Summers, Ryan; Said, Ziad; Wang, Shuai; Culbertson, Michael

    2015-11-01

    This study is part of a large-scale project focused on 'Qatari students' Interest in, and Attitudes toward, Science' (QIAS). QIAS aimed to gauge Qatari student attitudes toward science in grades 3-12, examine factors that impact these attitudes, and assess the relationship between student attitudes and prevailing modes of science teaching in Qatari schools. This report details the development and validation of the 'Arabic-Speaking Students' Attitudes toward Science Survey' (ASSASS), which was specifically developed for the purposes of the QIAS project. The theories of reasoned action and planned behavior (TRAPB) [Ajzen, I., & Fishbein, M. (2005). The influence of attitudes on behavior. In D. Albarracín, B. T. Johnson, & M. P. Zanna (Eds.), The handbook of attitudes (pp. 173-221). Mahwah, NJ: Erlbaum] guided the instrument development. Development and validation of the ASSASS proceeded in 3 phases. First, a 10-member expert panel examined an initial pool of 74 items, which were revised and consolidated into a 60-item version of the instrument. This version was piloted with 369 Qatari students from the target schools and grade levels. Analyses of pilot data resulted in a refined version of the ASSASS, which was administered to a national probability sample of 3027 participants representing all students enrolled in grades 3-12 in the various types of schools in Qatar. Of the latter, 1978 students completed the Arabic version of the instrument. Analyses supported a robust, 5-factor model for the instrument, which is consistent with the TRAPB framework. The factors were: Attitudes toward science and school science, unfavorable outlook on science, control beliefs about ability in science, behavioral beliefs about the consequences of engaging with science, and intentions to pursue science.

  20. Colloid Microthruster Feed System Development for Fine Pointing and Drag-Free Control of Multi-Year Astronomical Observatories

    Science.gov (United States)

    Ziemer, John; Mueller, J.; Spence, D.; Hruby, V.

    2014-01-01

    A new Colloid Microthruster feed system, including a propellant tank and redundant Microvalves, is being developed for fine pointing and drag-free operations of multi-year astronomical observatories under the PCOS SAT program. Almost all Gravitational Wave Observatory (GWO) concepts require microthrusters to maintain a drag-free environment for the inertial sensor instrument to meet the mission science objectives. The current state-of-the-art microthruster in the US is the Busek Colloid Micro-Newton Thruster (CMNT) originally developed under the New Millennium Program for the Space Technology 7 (ST7) and ESA's LISA Pathfinder (LPF) technology demonstration mission. The ST7 CMNT design includes a bellows propellant storage tank that is sized to provide up to 90 days of maximum thrust (30 µN). The new propellant tank is based on a blow-down, metal-diaphragm spherical tank design with enough capacity for a 5-year GWO mission. The new feed system will also include the third generation of Busek’s Microvalve, currently being developed under a NASA Phase II SBIR. The Microvalve is responsible for the picoliter per second control of the propellant from the tank to the thruster head, demanding parts with micron-level tolerances, critical alignments, and challenging acceptance test protocols. This microthruster system could also be considered for replacement of reaction wheels for slewing and fine pointing of other astronomical observatories, including Exo-Planet Observatory concepts. The goal of the PCOS SAT effort is to raise the new system to TRL 5 with performance and environmental testing within the next two years.

  1. The EUI Data Center at the Royal Observatory of Belgium: challenges and solutions

    Science.gov (United States)

    Verbeeck, Cis; Stegen, Koen; Berghmans, David; West, Matthew; Kraaikamp, Emil; Gissot, Samuel; Giordanengo, Boris; Nicula, Bogdan

    ESA’s Solar Orbiter mission is conceived to perform a close-up study of the Sun and the inner heliosphere. With a perihelion close at 0.29 AU and a maximum aphelion at about 0.85 AU, Solar Orbiter ventures closer to the Sun than any spacecraft before. Furthermore, about 3 years after launch, the spacecraft will begin an out-of-ecliptic phase, with inclinations gradually increasing up to 30 degrees. Solar Orbiter will be launched in 2017 and its nominal mission will last until 2024 (with the possibility of an extended mission until 2026). It will provide unique data and imagery of the Sun. The Extreme Ultraviolet Imager (EUI) suite onboard Solar Orbiter is composed of two High Resolution Imagers (HRI, one at Lyman-alpha and one at 174 Angstrom), and one dual band Full-Sun imager (FSI) working alternatively at the 174 and 304 Angstrom EUV passbands. The EUI Data Center (EDC), under PI supervision and located at the Royal Observatory of Belgium (Brussels), will be the single point of contact for instrument planning activities and for data deliveries to the Solar Orbiter archive at ESAC (Madrid), and is currently in its design phase. The EUI Data Center will be responsible for delivery to ESAC and the maintenance of the pipeline software that will process EUI data from telemetry packets to higher level data products. It will also ensure the delivery of these data products to the Solar Orbiter Data Archive, and maintain the instrument user manual that documents the processing of EUI non-science TM packets at ESOC (Darmstadt). The EDC will monitor any anomaly affecting the EUI instrument and produce on a regular basis the Instrument Operations Reports including an instrument health and science performance review. Here, we present an overview of the EDC and how it envisages to tackle some specific challenges. Since EUI will only observe during three “science windows” of 10 days each per orbit of about 165 days and in view of a severely limited telemetry, it is

  2. Low-noise magnetic observatory variometer with race-track sensors

    International Nuclear Information System (INIS)

    Janošek, M; Petrucha, V; Vlk, M

    2016-01-01

    We present a low-noise, high-stability observatory magnetometer with race-track sensors, as developed by the Czech Technical University in Prague for National Observatory of Athens. As opposed to the standard instruments, we used our novel race-track fluxgate sensors with planar oval core which were cut by state-of-the art pico-second UV-laser. The noise performance of the complete electronics and sensor chain is below 6 pT/√Hz @ 1 Hz. The electronics uses 24-bit 200-Hz A/D converter with simultaneous sampling and all digital processing is done in FPGA. The variometer with the sensors mounted on a MACOR cube has been successfully calibrated by scalar method. (paper)

  3. The Importance of Marine Observatories and of RAIA in Particular

    Directory of Open Access Journals (Sweden)

    Luísa Bastos

    2016-08-01

    Full Text Available Coastal and Oceanic Observatories are important tools to provide information on ocean state, phenomena and processes. They meet the need for a better understanding of coastal and ocean dynamics, revealing regional characteristics and vulnerabilities. These observatories are extremely useful to guide human actions in response to natural events and potential climate change impacts, anticipating the occurrence of extreme weather and oceanic events and helping to minimize consequent personal and material damages and costs.International organizations and local governments have shown an increasing interest in operational oceanography and coastal, marine and oceanic observations, which resulted in substantial investments in these areas. A variety of physical, chemical and biological data have been collected to better understand the specific characteristics of each ocean area and its importance in the global context. Also the general public’s interest in marine issues and observatories has been raised, mainly in relation to vulnerability, sustainability and climate change issues. Data and products obtained by an observatory are hence useful to a broad range of stakeholders, from national and local authorities to the population in general.An introduction to Ocean Observatories, including their national and regional importance, and a brief analysis of the societal interest in these observatories and related issues are presented. The potential of a Coastal and Ocean Observatory is then demonstrated using the RAIA observatory as example. This modern and comprehensive observatory is dedicated to improve operational oceanography, technology and marine science for the North Western Iberian coast, and to provide services to a large range of stakeholders.

  4. First results from the Penn State Allsky Imager at the Arecibo Observatory

    Science.gov (United States)

    Seker, I.; Mathews, J. D.; Wiig, J.; Gutierrez, P. F.; Friedman, J. S.; Tepley, C. A.

    2007-03-01

    The Penn State Allsky imager (PSASI), a user-owned-public-access (UOPA) instrument installed at Arecibo Observatory (AO: 18.3°N, 66.75°W; altitude: 350 m a.s.l.; L = 1.43 at 300 km; dip angle: 46°; geomagnetic coordinates: 29°N, 5.5°E), is a CCD-based high-resolution allsky optical imager that has been collecting ionospheric airglow data at night since May 2003. The computer controlled six-position filter wheel is equipped with three filters at 630 nm (red), 557.7 nm (green), and 777.4 nm (near-IR), respectively, which correspond to ionosphere-related oxygen emissions. The imager data, taken for more than 3.5 years now, is being used to study various ionospheric processes, such as mapped equatorial spread-F plumes, E-region gravity waves, among other, in conjunction with the AO incoherent scatter radar (ISR), mesosphere and lower thermosphere (MLT) metals lidar, and other instruments, including microbarographs. Data availability and quality as well as specific airglow events on both small/large time/spatial scales are examined, categorized, and made freely available at a data-server website. Our goal here is to briefly review the airglow science enabled by allsky imaging at AO, to describe the instrument and the data-collection methodology, and to present some of the significant results, including airglow events that correspond to ISR results.

  5. Quality Assurance of Real-Time Oceanographic Data from the Cabled Array of the Ocean Observatories Initiative

    Science.gov (United States)

    Kawka, O. E.; Nelson, J. S.; Manalang, D.; Kelley, D. S.

    2016-02-01

    The Cabled Array component of the NSF-funded Ocean Observatories Initiative (OOI) provides access to real-time physical, chemical, geological, and biological data from water column and seafloor platforms/instruments at sites spanning the southern half of the Juan de Fuca Plate. The Quality Assurance (QA) program for OOI data is designed to ensure that data products meet OOI science requirements. This overall data QA plan establishes the guidelines for assuring OOI data quality and summarizes Quality Control (QC) protocols and procedures, based on best practices, which can be utilized to ensure the highest quality data across the OOI program. This presentation will highlight, specifically, the QA/QC approach being utilized for the OOI Cabled Array infrastructure and data and will include a summary of both shipboard and shore-based protocols currently in use. Aspects addressed will be pre-deployment instrument testing and calibration checks, post-deployment and pre-recovery field verification of data, and post-recovery "as-found" testing of instruments. Examples of QA/QC data will be presented and specific cases of cabled data will be discussed in the context of quality assessments and adjustment/correction of OOI datasets overall for inherent sensor drift and/or instrument fouling.

  6. Smartphone measurement engineering - Innovative challenges for science and education, instrumentation and training

    Energy Technology Data Exchange (ETDEWEB)

    Hofmann, D; Dittrich, P-G; Duentsch, E [Senior Network Manager NEMO SpectroNet, Technologie- und Innovationspark Jena GmbH, Wildenbruchstrasse 15, D-07745 Jena (Germany)

    2010-07-01

    Smartphones have an enormous conceptual and structural influence on measurement science and education, instrumentation and training. Smartphones are matured. They became convenient, reliable and affordable. In 2009 worldwide 174 million Smartphones has been delivered. Measurement with Smartphones is ready for the future. In only 10 years the German vision industry tripled its global sales volume to one Billion Euro/Year. Machine vision is used for mobile object identification, contactless industrial quality control, personalized health care, remote facility and transport management, safety critical surveillance and all tasks which are too complex for the human eye or too monotonous for the human brain. Aim of the paper is to describe selected success stories for the application of Smartphones for measurement engineering in science and education, instrumentation and training.

  7. Smartphone measurement engineering - Innovative challenges for science and education, instrumentation and training

    International Nuclear Information System (INIS)

    Hofmann, D; Dittrich, P-G; Duentsch, E

    2010-01-01

    Smartphones have an enormous conceptual and structural influence on measurement science and education, instrumentation and training. Smartphones are matured. They became convenient, reliable and affordable. In 2009 worldwide 174 million Smartphones has been delivered. Measurement with Smartphones is ready for the future. In only 10 years the German vision industry tripled its global sales volume to one Billion Euro/Year. Machine vision is used for mobile object identification, contactless industrial quality control, personalized health care, remote facility and transport management, safety critical surveillance and all tasks which are too complex for the human eye or too monotonous for the human brain. Aim of the paper is to describe selected success stories for the application of Smartphones for measurement engineering in science and education, instrumentation and training.

  8. TMT in the Astronomical Landscape of the 2020s

    Science.gov (United States)

    Dickinson, Mark; Inami, Hanae

    2014-07-01

    Thirty Meter Telescope Observatory and NOAO will host the second TMT Science Forum at Loews Ventana Canyon Resort in Tucson, Arizona. The TMT Science Forum is an an annual gathering of astronomers, educators, and observatory staff, who meet to explore TMT science, instrumentation, observatory operations, archiving and data processing, astronomy education, and science, technology, engineering, and math (STEM) issues. It is an opportunity for astronomers from the international TMT partners and from the US-at-large community to learn about the observatory status, discuss and plan cutting-edge science, establish collaborations, and to help shape the future of TMT. One important theme for this year's Forum will be the synergy between TMT and other facilities in the post-2020 astronomical landscape. There will be plenary sessions, an instrumentation workshop, topical science sessions and meetings of the TMT International Science Development Teams (ISDTs).

  9. International Conference on Bio-Medical Instrumentation and related Engineering and Physical Sciences (BIOMEP 2015)

    Science.gov (United States)

    2015-09-01

    The International Conference on Bio-Medical Instrumentation and related Engineering and Physical Sciences (BIOMEP 2015) took place in the Technological Educational Institute (TEI) of Athens, Greece on June 18-20, 2015 and was organized by the Department of Biomedical Engineering. The scope of the conference was to provide a forum on the latest developments in Biomedical Instrumentation and related principles of Physical and Engineering sciences. Scientists and engineers from academic, industrial and health disciplines were invited to participate in the Conference and to contribute both in the promotion and dissemination of the scientific knowledge.

  10. Armagh Observatory - Historic Building Information Modelling for Virtual Learning in Building Conservation

    Science.gov (United States)

    Murphy, M.; Chenaux, A.; Keenaghan, G.; GIbson, V..; Butler, J.; Pybusr, C.

    2017-08-01

    In this paper the recording and design for a Virtual Reality Immersive Model of Armagh Observatory is presented, which will replicate the historic buildings and landscape with distant meridian markers and position of its principal historic instruments within a model of the night sky showing the position of bright stars. The virtual reality model can be used for educational purposes allowing the instruments within the historic building model to be manipulated within 3D space to demonstrate how the position measurements of stars were made in the 18th century. A description is given of current student and researchers activities concerning on-site recording and surveying and the virtual modelling of the buildings and landscape. This is followed by a design for a Virtual Reality Immersive Model of Armagh Observatory use game engine and virtual learning platforms and concepts.

  11. Lockheed Solar Observatory and the Discovery of Moreton-Ramsey Waves

    Science.gov (United States)

    Tarbell, Theodore D.

    2014-06-01

    Moreton Waves are high-speed disturbances seen traveling away from large solar flares in H-alpha movies of the solar chromosphere. They were discovered by the observer Harry Ramsey in the late 1950s, and then published and publicized by the director Gail Moreton, both of the Lockheed Solar Observatory in the Hollywood Hills of Southern California. These efforts established the scientific reputation and secured continuing funding of the observatory, whose present-day successor is the Lockheed Martin Solar and Astrophysics Lab in Palo Alto. Moreton waves are rare, and there was limited interest in them until the EIT instrument on SOHO began seeing large numbers of similar waves in the corona in the late 1990s. The exact relation between the two observations is still a research topic today. This talk will describe some of the history of the observatory and the discovery and early interpretation of the waves.

  12. Building galaxies, stars, planets and the ingredients for life between the stars. The science behind the European Ultraviolet-Visible Observatory

    Science.gov (United States)

    Gómez de Castro, Ana I.; Appourchaux, Thierry; Barstow, Martin A.; Barthelemy, Mathieu; Baudin, Frederic; Benetti, Stefano; Blay, Pere; Brosch, Noah; Bunce, Emma; de Martino, Domitilla; Deharveng, Jean-Michel; Ferlet, Roger; France, Kevin; García, Miriam; Gänsicke, Boris; Gry, Cecile; Hillenbrand, Lynne; Josselin, Eric; Kehrig, Carolina; Lamy, Laurent; Lapington, Jon; Lecavelier des Etangs, Alain; LePetit, Frank; López-Santiago, Javier; Milliard, Bruno; Monier, Richard; Naletto, Giampiero; Nazé, Yael; Neiner, Coralie; Nichols, Jonathan; Orio, Marina; Pagano, Isabella; Peroux, Céline; Rauw, Gregor; Shore, Steven; Spaans, Marco; Tovmassian, Gagik; ud-Doula, Asif; Vilchez, José

    2014-11-01

    This contribution gathers the contents of the white paper submitted by the UV community to the Call issued by the European Space Agency in March 2013, for the definition of the L2 and L3 missions in the ESA science program. We outlined the key science that a large UV facility would make possible and the instrumentation to be implemented. The growth of luminous structures and the building blocks of life in the Universe began as primordial gas was processed in stars and mixed at galactic scales. The mechanisms responsible for this development are not well-understood and have changed over the intervening 13 billion years. To follow the evolution of matter over cosmic time, it is necessary to study the strongest (resonance) transitions of the most abundant species in the Universe. Most of them are in the ultraviolet (UV; 950 Å-3000 Å) spectral range that is unobservable from the ground. A versatile space observatory with UV sensitivity a factor of 50-100 greater than existing facilities will revolutionize our understanding of the Universe. Habitable planets grow in protostellar discs under ultraviolet irradiation, a by-product of the star-disk interaction that drives the physical and chemical evolution of discs and young planetary systems. The electronic transitions of the most abundant molecules are pumped by this UV field, providing unique diagnostics of the planet-forming environment that cannot be accessed from the ground. Earth's atmosphere is in constant interaction with the interplanetary medium and the solar UV radiation field. A 50-100 times improvement in sensitivity would enable the observation of the key atmospheric ingredients of Earth-like exoplanets (carbon, oxygen, ozone), provide crucial input for models of biologically active worlds outside the solar system, and provide the phenomenological baseline to understand the Earth atmosphere in context.

  13. TRW Ships NASA's Chandra X-ray Observatory To Kennedy Space Center

    Science.gov (United States)

    1999-04-01

    Two U.S. Air Force C-5 Galaxy transport planes carrying the observatory and its ground support equipment landed at Kennedy's Space Shuttle Landing Facility at 2:40 p.m. EST this afternoon. REDONDO BEACH, CA.--(Business Wire)--Feb. 4, 1999--TRW has shipped NASA's Chandra X-ray Observatory ("Chandra") to the Kennedy Space Center (KSC), in Florida, in preparation for a Space Shuttle launch later this year. The 45-foot-tall, 5-ton science satellite will provide astronomers with new information on supernova remnants, the surroundings of black holes, and other celestial phenomena that produce vast quantities of X-rays. Cradled safely in the cargo hold of a tractor-trailer rig called the Space Cargo Transportation System (SCTS), NASA's newest space telescope was ferried on Feb. 4 from Los Angeles International Airport to KSC aboard an Air Force C-5 Galaxy transporter. The SCTS, an Air Force container, closely resembles the size and shape of the Shuttle cargo bay. Over the next few months, Chandra will undergo final tests at KSC and be mated to a Boeing-provided Inertial Upper Stage for launch aboard Space Shuttle Columbia. A launch date for the Space Shuttle STS-93 mission is expected to be announced later this week. The third in NASA's family of Great Observatories that includes the Hubble Space Telescope and the TRW-built Compton Gamma Ray observatory, Chandra will use the world's most powerful X-ray telescope to allow scientists to "see" and monitor cosmic events that are invisible to conventional optical telescopes. Chandra's X-ray images will yield new insight into celestial phenomena such as the temperature and extent of gas clouds that comprise clusters of galaxies and the superheating of gas and dust particles as they swirl into black holes. A TRW-led team that includes the Eastman Kodak Co., Raytheon Optical Systems Inc., and Ball Aerospace & Technologies Corp. designed and built the Chandra X-ray Observatory for NASA's Marshall Space Flight Center. The

  14. Private Observatories in South Africa

    Science.gov (United States)

    Rijsdijk, C.

    2016-12-01

    Descriptions of private observatories in South Africa, written by their owners. Positions, equipment descriptions and observing programmes are given. Included are: Klein Karoo Observatory (B. Monard), Cederberg Observatory (various), Centurion Planetary and Lunar Observatory (C. Foster), Le Marischel Observatory (L. Ferreira), Sterkastaaing Observatory (M. Streicher), Henley on Klip (B. Fraser), Archer Observatory (B. Dumas), Overbeek Observatory (A. Overbeek), Overberg Observatory (A. van Staden), St Cyprian's School Observatory, Fisherhaven Small Telescope Observatory (J. Retief), COSPAR 0433 (G. Roberts), COSPAR 0434 (I. Roberts), Weltevreden Karoo Observatory (D. Bullis), Winobs (M. Shafer)

  15. The Chandra X-ray Observatory data processing system

    Science.gov (United States)

    Evans, Ian; Cresitello-Dittmar, Mark; Doe, Stephen; Evans, Janet; Fabbiano, Giuseppina; Germain, Gregg; Glotfelty, Kenny; Plummer, David; Zografou, Panagoula

    2006-06-01

    Raw data from the Chandra X-ray Observatory are processed by a set of standard data processing pipelines to create scientifically useful data products appropriate for further analysis by end users. Fully automated pipelines read the dumped raw telemetry byte stream from the spacecraft and perform the common reductions and calibrations necessary to remove spacecraft and instrumental signatures and convert the data into physically meaningful quantities that can be further analyzed by observers. The resulting data products are subject to automated validation to ensure correct pipeline processing and verify that the spacecraft configuration and scheduling matched the observers request and any constraints. In addition, pipeline processing monitors science and engineering data for anomalous indications and trending, and triggers alerts if appropriate. Data products are ingested and stored in the Chandra Data Archive, where they are made available for downloading by users. In this paper, we describe the architecture of the data processing system, including the scientific algorithms that are applied to the data, and interfaces to other subsystems. We place particular emphasis on the impacts of design choices on system integrity and maintainability. We review areas where algorithmic improvements or changes in instrument characteristics have required significant enhancements, and the mechanisms used to effect these changes while assuring continued scientific integrity and robustness. We discuss major enhancements to the data processing system that are currently being developed to automate production of the Chandra Source Catalog.

  16. The Paris Observatory has 350 years

    Science.gov (United States)

    Lequeux, James

    2017-01-01

    The Paris Observatory is the oldest astronomical observatory that has worked without interruption since its foundation to the present day. The building due to Claude Perrault is still in existence with few modifications, but of course other buildings have been added all along the centuries for housing new instruments and laboratories. In particular, a large dome has been built on the terrace in 1847, with a 38-cm diameter telescope completed in 1857: both are still visible. The main initial purpose of the Observatory was to determine longitudes. This was achieved by Jean-Dominique Cassini using the eclipses of the satellites of Jupiter: a much better map of France was the produced using this method, which unfortunately does not work at sea. Incidentally, the observation of these eclipses led to the discovery in 1676 of the finite velocity of light by Cassini and Rømer. Cassini also discovered the differential rotation of Jupiter and four satellites of Saturn. Then, geodesy was to be the main activity of the Observatory for more than a century, culminating in the famous Cassini map of France completed around 1790. During the first half of the 19th century, under François Arago, the Observatory was at the centre of French physics, which then developed very rapidly. Arago initiated astrophysics in 1810 by showing that the Sun and stars are made of incandescent gas. In 1854, the new director, Urbain Le Verrier, put emphasis on astrometry and celestial mechanics, discovering in particular the anomalous advance of the perihelion of Mercury, which was later to be a proof of General Relativity. In 1858, Leon Foucault built the first modern reflecting telescopes with their silvered glass mirror. Le Verrier created on his side modern meteorology, including some primitive forecasts. The following period was not so bright, due to the enormous project of the Carte du Ciel, which took much of the forces of the Observatory for half a century with little scientific return. In

  17. Mass composition studies using the surface detector of the Pierre Auger Observatory

    International Nuclear Information System (INIS)

    Wahlberg, Hernan

    2009-01-01

    The mass composition of ultra-high energy cosmic rays is a critical issue to understand their origin and nature. The Pierre Auger Observatory is a hybrid instrument which provides a powerful environment for the determination of the primary mass. The Surface Detector of the Pierre Auger Observatory alone allows the study of several shower parameters with high discriminating power between primary elements. Novel analysis techniques using different features of signals in the Cherenkov stations are discussed. These are the signal risetime, the azimuthal time asymmetry and the muon density of the showers.

  18. Error Budget for a Calibration Demonstration System for the Reflected Solar Instrument for the Climate Absolute Radiance and Refractivity Observatory

    Science.gov (United States)

    Thome, Kurtis; McCorkel, Joel; McAndrew, Brendan

    2013-01-01

    A goal of the Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission is to observe highaccuracy, long-term climate change trends over decadal time scales. The key to such a goal is to improving the accuracy of SI traceable absolute calibration across infrared and reflected solar wavelengths allowing climate change to be separated from the limit of natural variability. The advances required to reach on-orbit absolute accuracy to allow climate change observations to survive data gaps exist at NIST in the laboratory, but still need demonstration that the advances can move successfully from to NASA and/or instrument vendor capabilities for spaceborne instruments. The current work describes the radiometric calibration error budget for the Solar, Lunar for Absolute Reflectance Imaging Spectroradiometer (SOLARIS) which is the calibration demonstration system (CDS) for the reflected solar portion of CLARREO. The goal of the CDS is to allow the testing and evaluation of calibration approaches, alternate design and/or implementation approaches and components for the CLARREO mission. SOLARIS also provides a test-bed for detector technologies, non-linearity determination and uncertainties, and application of future technology developments and suggested spacecraft instrument design modifications. The resulting SI-traceable error budget for reflectance retrieval using solar irradiance as a reference and methods for laboratory-based, absolute calibration suitable for climatequality data collections is given. Key components in the error budget are geometry differences between the solar and earth views, knowledge of attenuator behavior when viewing the sun, and sensor behavior such as detector linearity and noise behavior. Methods for demonstrating this error budget are also presented.

  19. Plans for a Northern Cascadia Subduction Zone Observatory

    Science.gov (United States)

    Heesemann, M.; Wang, K.; Davis, E.; Chadwell, C. D.; Nissen, E.; Moran, K.; Scherwath, M.

    2017-12-01

    To accurately assess earthquake and tsunami hazards posed by the Cascadia Subduction Zone, it is critically important to know which area of the plate interface is locked and whether or not part of the energy is being released aseismically by slow creep on the fault. Deeper locking that extends further to the coast produces stronger shaking in population centers. Shallow locking, on the other hand, leads to bigger tsunamis. We will report on and discuss plans for a new amphibious Northern Cascadia Subduction Zone Observatory (NCSZO) that will leverage the existing NEPTUNE cabled seafloor observatory, which is operated by Ocean Networks Canada (ONC), and the onshore network of geodetic stations, which is operated by Natural Resources Canada (NRCan). To create a NCSZO we plan to (1) add a network of seven GPS-Acoustic (GPS-A) sites offshore Vancouver Island, (2) establish a Deformation Front Observatory, and (3) improve the existing onshore geodetic network (see Figure below). The GPS-A stations will provide the undisturbed motion of the Juan de Fuca (JdF) Plate (1), deformation of the JdF plate (2), deformation of the overriding plate (3-7) and a cabled laboratory to study the potential for continuous GPS-A measurements (6). The Deformation Front Observatory will be used to study possible transient slip events using seafloor pressure and tilt instruments and fluid flux meters.

  20. Chandra: Ten Years of Amazing Science with a Great Observatory

    Science.gov (United States)

    Weisskopf, Martin C.

    2009-01-01

    We review briefly review the history of the development of the Chandra X-Ray Observatory, highlighting certain details that many attendees of this Conference might not be aware of. We then present a selection of scientific highlights of the first 10 years of this remarkable and unique mission.

  1. Real-Time On-Board Airborne Demonstration of High-Speed On-Board Data Processing for Science Instruments (HOPS)

    Science.gov (United States)

    Beyon, Jeffrey Y.; Ng, Tak-Kwong; Davis, Mitchell J.; Adams, James K.; Bowen, Stephen C.; Fay, James J.; Hutchinson, Mark A.

    2015-01-01

    The project called High-Speed On-Board Data Processing for Science Instruments (HOPS) has been funded by NASA Earth Science Technology Office (ESTO) Advanced Information Systems Technology (AIST) program since April, 2012. The HOPS team recently completed two flight campaigns during the summer of 2014 on two different aircrafts with two different science instruments. The first flight campaign was in July, 2014 based at NASA Langley Research Center (LaRC) in Hampton, VA on the NASA's HU-25 aircraft. The science instrument that flew with HOPS was Active Sensing of CO2 Emissions over Nights, Days, and Seasons (ASCENDS) CarbonHawk Experiment Simulator (ACES) funded by NASA's Instrument Incubator Program (IIP). The second campaign was in August, 2014 based at NASA Armstrong Flight Research Center (AFRC) in Palmdale, CA on the NASA's DC-8 aircraft. HOPS flew with the Multifunctional Fiber Laser Lidar (MFLL) instrument developed by Excelis Inc. The goal of the campaigns was to perform an end-to-end demonstration of the capabilities of the HOPS prototype system (HOPS COTS) while running the most computationally intensive part of the ASCENDS algorithm real-time on-board. The comparison of the two flight campaigns and the results of the functionality tests of the HOPS COTS are presented in this paper.

  2. The Goldstone solar system radar: A science instrument for planetary research

    Science.gov (United States)

    Dvorsky, J. D.; Renzetti, N. A.; Fulton, D. E.

    1992-01-01

    The Goldstone Solar System Radar (GSSR) station at NASA's Deep Space Communications Complex in California's Mojave Desert is described. A short chronological account of the GSSR's technical development and scientific discoveries is given. This is followed by a basic discussion of how information is derived from the radar echo and how the raw information can be used to increase understanding of the solar system. A moderately detailed description of the radar system is given, and the engineering performance of the radar is discussed. The operating characteristics of the Arcibo Observatory in Puerto Rico are briefly described and compared with those of the GSSR. Planned and in-process improvements to the existing radar, as well as the performance of a hypothetical 128-m diameter antenna radar station, are described. A comprehensive bibliography of referred scientific and engineering articles presenting results that depended on data gathered by the instrument is provided.

  3. A New Observatory for Eastern College: A Dream Realized

    Science.gov (United States)

    Bradstreet, D. H.

    1996-12-01

    The Eastern College Observatory began as a rooftop observing deck with one Celestron 8 telescope in 1976 as the workhorse instrument of the observational astronomy lab within the core curriculum. For 20 years the observing deck served as the crude observatory, being augmented through the years by other computerized Celestron 8's and a 17.5" diameter Dobsonian with computerized setting circles. The lab consisted primarily of visual observations and astrophotography. In 1987 plans were set into motion to raise money to build a permanent Observatory on the roof of the main classroom building. Fundraising efforts included three Jog-A-Thons (raising more than $40,000) and many donations from individuals and foundations. The fundraising was completed in 1996 and a two telescope observatory was constructed in the summer of 1996 complete with warm room, CCD cameras, computers, spectrograph, video network, and computerized single channel photometer. The telescopes are computerized 16" diameter Meade LX200 Schmidt-Cassegrains, each coupled to Gateway Pentium Pro 200 MHz computers. SBIG ST-8 CCD cameras were also secured for each telescope and an Optec SSP-7 photometer and Optomechanics Research 10C Spectrograph were also purchased. A Daystar H-alpha solar filter and Thousand Oaks visual light solar filter have expanded the Observatory's functionality to daytime observing as well. This is especially useful for the thousands of school children who frequent the Planetarium each year. The Observatory primarily serves the core astronomy lab where students must observe and photograph a prescribed number of celestial objects in a semester. Advanced students can take directed studies where they conduct photometry on eclipsing binaries or other variable stars or search for new asteroids. In addition, the Observatory and Planetarium are open to the public. Interested members of the community can reserve time on the telescopes and receive training and supervision from lab assistants

  4. The IceCube Neutrino Observatory: instrumentation and online systems

    International Nuclear Information System (INIS)

    Aartsen, M.G.; Ackermann, M.; Adams, J.; Aguilar, J.A.; Ansseau, I.; Ahlers, M.; Auer, R.; Baccus, J.; Barnet, S.; Ahrens, M.; Altmann, D.; Anton, G.; Andeen, K.; Anderson, T.; Archinger, M.; Argüelles, C.; Axani, S.; Auffenberg, J.; Bai, X.; Barwick, S.W.

    2017-01-01

    The IceCube Neutrino Observatory is a cubic-kilometer-scale high-energy neutrino detector built into the ice at the South Pole. Construction of IceCube, the largest neutrino detector built to date, was completed in 2011 and enabled the discovery of high-energy astrophysical neutrinos. We describe here the design, production, and calibration of the IceCube digital optical module (DOM), the cable systems, computing hardware, and our methodology for drilling and deployment. We also describe the online triggering and data filtering systems that select candidate neutrino and cosmic ray events for analysis. Due to a rigorous pre-deployment protocol, 98.4% of the DOMs in the deep ice are operating and collecting data. IceCube routinely achieves a detector uptime of 99% by emphasizing software stability and monitoring. Detector operations have been stable since construction was completed, and the detector is expected to operate at least until the end of the next decade.

  5. Developing a Virtual Network of Research Observatories

    Science.gov (United States)

    Hooper, R. P.; Kirschtl, D.

    2008-12-01

    The hydrologic community has been discussing the concept of a network of observatories for the advancement of hydrologic science in areas of scaling processes, in testing generality of hypotheses, and in examining non-linear couplings between hydrologic, biotic, and human systems. The Consortium of Universities for the Advancement of Hydrologic Science, Inc. (CUAHSI) is exploring the formation of a virtual network of observatories, formed from existing field studies without regard to funding source. Such a network would encourage sharing of data, metadata, field methods, and data analysis techniques to enable multidisciplinary synthesis, meta-analysis, and scientific collaboration in hydrologic and environmental science and engineering. The virtual network would strive to provide both the data and the environmental context of the data through advanced cyberinfrastructure support. The foundation for this virtual network is Water Data Services that enable the publication of time-series data collected at fixed points using a services-oriented architecture. These publication services, developed in the CUAHSI Hydrologic Information Systems project, permit the discovery of data from both academic and government sources through a single portal. Additional services under consideration are publication of geospatial data sets, immersive environments based upon site digital elevation models, and a common web portal to member sites populated with structured data about the site (such as land use history and geologic setting) to permit understanding the environmental context of the data being shared.

  6. Testing of Environmental Satellite Bus-Instrument Interfaces Using Engineering Models

    Science.gov (United States)

    Gagnier, Donald; Hayner, Rick; Nosek, Thomas; Roza, Michael; Hendershot, James E.; Razzaghi, Andrea I.

    2004-01-01

    This paper discusses the formulation and execution of a laboratory test of the electrical interfaces between multiple atmospheric scientific instruments and the spacecraft bus that carries them. The testing, performed in 2002, used engineering models of the instruments and the Aura spacecraft bus electronics. Aura is one of NASA s Earth Observatory System missions. The test was designed to evaluate the complex interfaces in the command and data handling subsystems prior to integration of the complete flight instruments on the spacecraft. A problem discovered during the flight integration phase of the observatory can cause significant cost and schedule impacts. The tests successfully revealed problems and led to their resolution before the full-up integration phase, saving significant cost and schedule. This approach could be beneficial for future environmental satellite programs involving the integration of multiple, complex scientific instruments onto a spacecraft bus.

  7. Developing instruments concerning scientific epistemic beliefs and goal orientations in learning science: a validation study

    Science.gov (United States)

    Lin, Tzung-Jin; Tsai, Chin-Chung

    2017-11-01

    The purpose of this study was to develop and validate two survey instruments to evaluate high school students' scientific epistemic beliefs and goal orientations in learning science. The initial relationships between the sampled students' scientific epistemic beliefs and goal orientations in learning science were also investigated. A final valid sample of 600 volunteer Taiwanese high school students participated in this survey by responding to the Scientific Epistemic Beliefs Instrument (SEBI) and the Goal Orientations in Learning Science Instrument (GOLSI). Through both exploratory and confirmatory factor analyses, the SEBI and GOLSI were proven to be valid and reliable for assessing the participants' scientific epistemic beliefs and goal orientations in learning science. The path analysis results indicated that, by and large, the students with more sophisticated epistemic beliefs in various dimensions such as Development of Knowledge, Justification for Knowing, and Purpose of Knowing tended to adopt both Mastery-approach and Mastery-avoidance goals. Some interesting results were also found. For example, the students tended to set a learning goal to outperform others or merely demonstrate competence (Performance-approach) if they had more informed epistemic beliefs in the dimensions of Multiplicity of Knowledge, Uncertainty of Knowledge, and Purpose of Knowing.

  8. Progress on VESPA, a community-driven Virtual Observatory in Planetary Science

    Science.gov (United States)

    Erard, S.; Cecconi, B.; Le Sidaner, P.; Rossi, A. P.; Capria, M. T.; Schmitt, B.; Genot, V. N.; André, N.; Vandaele, A. C.; Scherf, M.; Hueso, R.; Maattanen, A. E.; Carry, B.; Achilleos, N.; Marmo, C.; Santolik, O.; Benson, K.; Fernique, P.

    2017-12-01

    The Europlanet H2020 program started on 1/9/2015 for 4 years. It includes an activity to adapt Virtual Observatory (VO) techniques to Planetary Science data called VESPA. The objective is to facilitate searches in big archives as well as sparse databases, to provide simple data access and on-line visualization, and to allow small data providers to make their data available in an interoperable environment with minimum effort. The VESPA system, based on a prototype developed in a previous program [1], has been hugely improved during the first two years of Europlanet H2020: the infrastructure has been upgraded to describe data in many fields more accurately; the main user search interface (http://vespa.obspm.fr) has been redesigned to provide more flexibility; alternative ways to access Planetary Science data services from VO tools have been implemented; VO tools are being improved to handle specificities of Solar System data, e.g. measurements in reflected light, coordinate systems, etc. Current steps include the development of a connection between the VO world and GIS tools, and integration of Heliophysics, planetary plasmas, and mineral spectroscopy data to support of the analysis of observations. Existing data services have been updated, and new ones have been designed. The global objective is already overstepped, with 34 services open and 20 more being finalized. A procedure to install data services has been documented, and hands-on sessions are organized twice a year at EGU and EPSC; this is intended to favour the installation of services by individual research teams, e.g. to distribute derived data related to a published study. In complement, regular discussions are held with big data providers, starting with space agencies (IPDA). Common projects with ESA and NASA's PDS have been engaged, with the goal to connect PDS4 and EPN-TAP. In parallel, a Solar System Interest Group has just been started in IVOA; the goal is here to adapt existing astronomy standards to

  9. NASA Chandra X-ray Observatory Selected as Editor's Choice in 2000 Discover Magazine Awards for Technological Innovation

    Science.gov (United States)

    2000-06-01

    The Chandra X-ray Observatory, NASA's newest and most powerful X-ray space telescope, has been selected as the winner of the Editor's Choice category of the 2000 Discover Magazine Awards for Technological Innovation. The team of government, industry, university and research institutions that designed, built and deployed Chandra for NASA's Marshall Space Flight Center, Huntsville, Ala, will be formally recognized June 24 at a gala awards celebration at Epcot at the Walt Disney World Resort in Orlando, Fl. Dr. Harvey Tananbaum, director of the Smithsonian Astrophysical Observatory's Chandra X-ray Science Center, Cambridge, Mass., which conducts the Chandra science mission for NASA, will receive the award on behalf of the team. "Chandra has opened a new window for astronomers into the universe of high-energy cosmic events such as pulsars, supernova remnants and black holes," said Tananbaum. "We're now able to create spectacularly detailed images of celestial phenomena whose mere existence we could only hypothesize before." Among Chandra's most significant discoveries to date, he lists the detection of a giant ring around the heart of the Crab Nebula, details of the shock wave created by an exploding star and resolution of the high-energy X-ray "glow" in the universe into millions of specific light sources. "The successful launch, deployment and on-orbit operations of NASA's Chandra X-ray Observatory is a testament to the solid partnership between TRW, NASA and the science community that has been enabling NASA's most important space science missions for the past 40 years," said Timothy W. Hannemann, executive vice president and general manager, TRW Space & Electronics Group. "The extraordinary images that Chandra is delivering daily speaks loudly not only to the quality of the science instruments on board, but also to the engineering talents and dedication to mission success exhibited by every member of NASA's Chandra mission team." Chandra, named in honor of Nobel

  10. IYA Outreach Plans for Appalachian State University's Observatories

    Science.gov (United States)

    Caton, Daniel B.; Pollock, J. T.; Saken, J. M.

    2009-01-01

    Appalachian State University will provide a variety of observing opportunities for the public during the International Year of Astronomy. These will be focused at both the campus GoTo Telescope Facility used by Introductory Astronomy students and the research facilities at our Dark Sky Observatory. The campus facility is composed of a rooftop deck with a roll-off roof housing fifteen Celestron C11 telescopes. During astronomy lab class meetings these telescopes are used either in situ or remotely by computer control from the adjacent classroom. For the IYA we will host the public for regular observing sessions at these telescopes. The research facility features a 32-inch DFM Engineering telescope with its dome attached to the Cline Visitor Center. The Visitor Center is still under construction and we anticipate its completion for a spring opening during IYA. The CVC will provide areas for educational outreach displays and a view of the telescope control room. Visitors will view celestial objects directly at the eyepiece. We are grateful for the support of the National Science Foundation, through grant number DUE-0536287, which provided instrumentation for the GoTO facility, and to J. Donald Cline for support of the Visitor Center.

  11. Fostering Collaboration Across the U.S. Critical Zone Observatories Network

    Science.gov (United States)

    Sharkey, S.; White, T. S.

    2017-12-01

    The Critical Zone (CZ) is defined as the permeable layer from the top of the vegetation canopy to the bottom of freely circulating groundwater where rock, soil, water, air and life meet. The study of the CZ is motivated by an overall lack of understanding of the coupled physical, chemical, and biological processes in this zone at differing spatial and temporal scales. Critical Zone Observatories (CZOs), supported by the U.S. National Science Foundation's Geosciences Directorate, are natural laboratories that aim to provide infrastructure, data and models to gain understanding of the evolution and function of the CZ from grain-to-watershed scales. The nine U.S. observatories span a range of climatic, ecologic, geologic, and physiographic environments from California to Puerto Rico, working on site-specific hypotheses and network-scale goals. CZO research infrastructure allows for teams of cross-disciplinary scientists at each site to further CZ science using field and theoretical approaches, education and outreach, and cross-CZO science. Cross-CZO science emerges from a set of common CZ science questions and hypotheses focused on CZ structure and evolution, event-based and continuous fluxes across CZ interfaces, and changes in storage of major CZ reservoirs at the catchment scale. CZO research seeks to understand coupled processes across all timescales using quantitative models parameterized from observations of meteorological variables, streams, and groundwater, and sampling and analyzing landforms, bedrock, soils, and ecosystems. Each observatory strives to apply common infrastructure, protocols and measurements that help quantify the composition and fluxes of energy, water, solutes, sediments, energy, and mass across boundaries of the CZ system through both space and time. This type of approach enables researchers to access and integrate data in a way that allows for the isolation of environmental variables and comparison of processes and responses across

  12. New Hubble Servicing Mission to upgrade instruments

    Science.gov (United States)

    2006-10-01

    The history of the NASA/ESA Hubble Space Telescope is dominated by the familiar sharp images and amazing discoveries that have had an unprecedented scientific impact on our view of the world and our understanding of the universe. Nevertheless, such important contributions to science and humankind have only been possible as result of regular upgrades and enhancements to Hubble’s instrumentation. Using the Space Shuttle for this fifth Servicing Mission underlines the important role that astronauts have played and continue to play in increasing the Space Telescope’s lifespan and scientific power. Since the loss of Columbia in 2003, the Shuttle has been successfully launched on three missions, confirming that improvements made to it have established the required high level of safety for the spacecraft and its crew. “There is never going to be an end to the science that we can do with a machine like Hubble”, says David Southwood, ESA’s Director of Science. “Hubble is our way of exploring our origins. Everyone should be proud that there is a European element to it and that we all are part of its success at some level.” This Servicing Mission will not just ensure that Hubble can function for perhaps as much as another ten years; it will also increase its capabilities significantly in key areas. This highly visible mission is expected to take place in 2008 and will feature several space walks. As part of the upgrade, two new scientific instruments will be installed: the Cosmic Origins Spectrograph and Wide Field Camera 3. Each has advanced technology sensors that will dramatically improve Hubble’s potential for discovery and enable it to observe faint light from the youngest stars and galaxies in the universe. With such an astounding increase in its science capabilities, this orbital observatory will continue to penetrate the most distant regions of outer space and reveal breathtaking phenomena. “Today, Hubble is producing more science than ever before in

  13. Monitoring and Detecting X-ray Transients with the Swift Observatory

    Science.gov (United States)

    Markwardt, Craig

    2002-01-01

    Swift is a multi-wavelength observatory specifically designed to detect transients sources in the gamma-ray energy band 15-200 keV. The primary goals of the mission involve gamma ray burst (GRB) astronomy, namely to determine the origin of GRBs and their afterglows, and use bursts to probe the early Universe. However, Swift will also discover new X-ray transient sources, and it will be possible to bring Swift's considerable multi-wavelength capabilities to bear on these sources, and those discovered by other means. The Burst Alert Telescope (BAT) is a coded mask instrument sensitive to 15-200 keV gamma rays, and has a field of view which covers approximately 1/8th of the sky in a single pointing. Over a typical observing day, the almost the entire sky will be observed and monitored for new transient sources. Sources will be detected within several hours of observation. The two narrow field instruments, the X-ray Telescope and Ultra-Violet Optical Telescope, can provide sensitive simultaneous imaging and spectroscopy observations in the optical through soft X-ray bands. The Swift science operations team will entertain requests for targets of opportunity for sources which are astrophysically significant. Swift will be ideally suited for the detection of transients which produce hard X-rays, such as black hole binaries and some neutron star systems.

  14. ARMAGH OBSERVATORY – HISTORIC BUILDING INFORMATION MODELLING FOR VIRTUAL LEARNING IN BUILDING CONSERVATION

    Directory of Open Access Journals (Sweden)

    M. Murphy

    2017-08-01

    Full Text Available In this paper the recording and design for a Virtual Reality Immersive Model of Armagh Observatory is presented, which will replicate the historic buildings and landscape with distant meridian markers and position of its principal historic instruments within a model of the night sky showing the position of bright stars. The virtual reality model can be used for educational purposes allowing the instruments within the historic building model to be manipulated within 3D space to demonstrate how the position measurements of stars were made in the 18th century. A description is given of current student and researchers activities concerning on-site recording and surveying and the virtual modelling of the buildings and landscape. This is followed by a design for a Virtual Reality Immersive Model of Armagh Observatory use game engine and virtual learning platforms and concepts.

  15. The Renovation and Future Capabilities of the Thacher Observatory

    Science.gov (United States)

    O'Neill, Katie; Osuna, Natalie; Edwards, Nick; Klink, Douglas; Swift, Jonathan; Vyhnal, Chris; Meyer, Kurt

    2016-01-01

    The Thacher School is in the process of renovating the campus observatory with a new meter class telescope and full automation capabilities for the purpose of scientific research and education. New equipment on site has provided a preliminary site characterization including seeing and V-band sky brightness measurements. These data, along with commissioning data from the MINERVA project (which uses comparable hardware) are used to estimate the capabilities of the observatory once renovation is complete. Our V-band limiting magnitude is expected to be better than 21.3 for a one minute integration time, and we estimate that milli-magnitude precision photometry will be possible for a V=14.5 point source over approximately 5 min timescales. The quick response, autonomous operation, and multi-band photometric capabilities of the renovated observatory will make it a powerful follow-up science facility for exoplanets, eclipsing binaries, near-Earth objects, stellar variability, and supernovae.

  16. The need for a European data platform for hydrological observatories

    Science.gov (United States)

    Blöschl, Günter; Bogena, Heye; Jensen, Karsten; Zacharias, Steffen; Kunstmann, Harald; Heinrich, Ingo; Kunkel, Ralf; Vereecken, Harry

    2017-04-01

    Experimental research in hydrology is amazingly fragmented and disperse. Typically, individual research groups establish and operate their own hydrological test sites and observatories with dedicated funding and specific research questions in mind. Once funding ceases, provisions for archiving and exchanging the data also soon run out and often data are lost or are no longer accessible to the research community. This has not only resulted in missed opportunities for exploring and mining hydrological data but also in a general difficulty in synthesizing research findings from different locations around the world. Many reasons for this fragmentation can be put forward, including the site-specific nature of hydrological processes, the particular types of research funding and the professional education in diverse departments. However, opportunities exist for making hydrological data more accessible and valuable to the research community, for example for designing cross-catchment experiments that build on a common data base and for the development and validation of hydrological models. A number of abundantly instrumented hydrological observatories, including the TERENO catchments in Germany, the HOBE catchment in Denmark and the HOAL catchment in Austria, have, in a first step, started to join forces to serve as a community-driven nucleus for a European data platform of hydrological observatories. The common data platform aims at making data of existing hydrological observatories accessible and available to the research community, thereby providing new opportunities for the design of cross-catchment experiments and model validation efforts. Tangible instruments for implementing this platform include a common data portal, for which the TEODOOR portal (http://www.tereno.net/) is currently used. Intangible instruments include a strong motivational basis. As with any community initiative, it is important to align expectations and to provide incentives to all involved. It is

  17. Instrument Correction and Dynamic Site Profile Validation at the Central United States Seismic Observatory, New Madrid Seismic Zone

    Science.gov (United States)

    Brengman, C.; Woolery, E. W.; Wang, Z.; Carpenter, S.

    2016-12-01

    The Central United States Seismic Observatory (CUSSO) is a vertical seismic array located in southwestern Kentucky within the New Madrid seismic zone. It is intended to describe the effects of local geology, including thick sediment overburden, on seismic-wave propagation, particularly strong-motion. The three-borehole array at CUSSO is composed of seismic sensors placed on the surface, and in the bedrock at various depths within the 585 m thick sediment overburden. The array's deep borehole provided a unique opportunity in the northern Mississippi embayment for the direct geological description and geophysical measurement of the complete late Cretaceous-Quaternary sediment column. A seven layer, intra-sediment velocity model is interpreted from the complex, inhomogeneous stratigraphy. The S- and P-wave sediment velocities range between 160 and 875 m/s and between 1000 and 2300 m/s, respectively, with bedrock velocities of 1452 and 3775 m/s, respectively. Cross-correlation and direct comparisons were used to filter out the instrument response and determine the instrument orientation, making CUSSO data ready for analysis, and making CUSSO a viable calibration site for other free-field sensors in the area. The corrected bedrock motions were numerically propagated through the CUSSO soil profile (transfer function) and compared, in terms of both peak acceleration and amplitude spectra, to the recorded surface observations. Initial observations reveal a complex spectral mix of amplification and de-amplification across the array, indicating the site effect in this deep sediment setting is not simply generated by the shallowest layers.

  18. Observatories and Telescopes of Modern Times

    Science.gov (United States)

    Leverington, David

    2016-11-01

    Preface; Part I. Optical Observatories: 1. Palomar Mountain Observatory; 2. The United States Optical Observatory; 3. From the Next Generation Telescope to Gemini and SOAR; 4. Competing primary mirror designs; 5. Active optics, adaptive optics and other technical innovations; 6. European Northern Observatory and Calar Alto; 7. European Southern Observatory; 8. Mauna Kea Observatory; 9. Australian optical observatories; 10. Mount Hopkins' Whipple Observatory and the MMT; 11. Apache Point Observatory; 12. Carnegie Southern Observatory (Las Campanas); 13. Mount Graham International Optical Observatory; 14. Modern optical interferometers; 15. Solar observatories; Part II. Radio Observatories: 16. Australian radio observatories; 17. Cambridge Mullard Radio Observatory; 18. Jodrell Bank; 19. Early radio observatories away from the Australian-British axis; 20. The American National Radio Astronomy Observatory; 21. Owens Valley and Mauna Kea; 22. Further North and Central American observatories; 23. Further European and Asian radio observatories; 24. ALMA and the South Pole; Name index; Optical observatory and telescope index; Radio observatory and telescope index; General index.

  19. The Use of Cronbach's Alpha When Developing and Reporting Research Instruments in Science Education

    Science.gov (United States)

    Taber, Keith S.

    2017-06-01

    Cronbach's alpha is a statistic commonly quoted by authors to demonstrate that tests and scales that have been constructed or adopted for research projects are fit for purpose. Cronbach's alpha is regularly adopted in studies in science education: it was referred to in 69 different papers published in 4 leading science education journals in a single year (2015)—usually as a measure of reliability. This article explores how this statistic is used in reporting science education research and what it represents. Authors often cite alpha values with little commentary to explain why they feel this statistic is relevant and seldom interpret the result for readers beyond citing an arbitrary threshold for an acceptable value. Those authors who do offer readers qualitative descriptors interpreting alpha values adopt a diverse and seemingly arbitrary terminology. More seriously, illustrative examples from the science education literature demonstrate that alpha may be acceptable even when there are recognised problems with the scales concerned. Alpha is also sometimes inappropriately used to claim an instrument is unidimensional. It is argued that a high value of alpha offers limited evidence of the reliability of a research instrument, and that indeed a very high value may actually be undesirable when developing a test of scientific knowledge or understanding. Guidance is offered to authors reporting, and readers evaluating, studies that present Cronbach's alpha statistic as evidence of instrument quality.

  20. Key issues in the thermal design of spaceborne cryogenic infrared instruments

    Science.gov (United States)

    Schember, Helene R.; Rapp, Donald

    1992-12-01

    Thermal design and analysis play an integral role in the development of spaceborne cryogenic infrared (IR) instruments. From conceptual sketches to final testing, both direct and derived thermal requirements place significant constraints on the instrument design. Although in practice these thermal requirements are interdependent, the sources of most thermal constraints may be grouped into six distinct categories. These are: (1) Detector temperatures, (2) Optics temperatures, (3) Pointing or alignment stability, (4) Mission lifetime, (5) Orbit, and (6) Test and Integration. In this paper, we discuss these six sources of thermal requirements with particular regard to development of instrument packages for low background infrared astronomical observatories. In the end, the thermal performance of these instruments must meet a set of thermal requirements. The development of these requirements is typically an ongoing and interactive process, however, and the thermal design must maintain flexibility and robustness throughout the process. The thermal (or cryogenic) engineer must understand the constraints imposed by the science requirements, the specific hardware, the observing environment, the mission design, and the testing program. By balancing these often competing factors, the system-oriented thermal engineer can work together with the experiment team to produce an effective overall design of the instrument.

  1. Maraghe Observatory and an Effort towards Retrieval of Architectural Design of Astronomical Units

    Directory of Open Access Journals (Sweden)

    Javad Shekari Niri

    2015-03-01

    Full Text Available Maraghe observatory was built by such engineers as Moayiededdin Orozi etc. under supervision of Khaje Nasireddin Tousi in 7th century AH. The most significant feature associated with Maraghe observatory is the fact that architecture is employed to achieve astronomical purposes in this site. The reason for preferring observatory by astronomers was the fact that these units are superior to wooden and metal instruments with respect to accuracy, no size limitations, etc. Architectural design and function of astronomical units of Maraghe observatory site after discovery of its foundation in the course of explorations before Islamic Revolution remained unclear until recent years. After conducting required studies and investigations, the author managed to find significant cues and after some precise comparisons, he succeeded to recover the main design and function of some astronomical units of this international center. Based on these findings these astronomical structures can reliably be rebuilt. This research showed that every circular or polygonal building cannot be considered as an observatory. For example form and function of cemetery structures are completely different with astronomical ones. Following this research also valuable results were obtained in relation to stone architectural structures present on Maraghe observatory hill. In addition, claims about invention of astronomical units of Maraghe observatory by non-Iranian scientists are rejected and rights of Iranian scientists are rationally defended in this regard.

  2. Metrology of the Solar Spectral Irradiance at the Top Of Atmosphere in the Near Infrared using Ground Based Instruments. Final results of the PYR-ILIOS campaign (Mauna Loa Observatory, June-July 2016).

    Science.gov (United States)

    Cessateur, G.; Bolsée, D.; Pereira, N.; Sperfeld, P.; Pape, S.

    2017-12-01

    The availability of reference spectra for the Solar Spectral Irradiance (SSI) is important for the solar physics, the studies of planetary atmospheres and climatology. The near infrared (NIR) part of these spectra is of great interest for its main role for example, in the Earth's radiative budget. Until recently, some large and unsolved discrepancies (up to 10 %) were observed in the 1.6 μm region between space instruments, models and ground-based measurements. We designed a ground-based instrumentation for SSI measurements at the Top Of Atmosphere (TOA) through atmospheric NIR windows using the Bouguer-Langley technique. The main instrument is a double NIR spectroradiometer designed by Bentham (UK), radiometrically characterized at the Royal Belgian Institute for Space Aeronomy. It was absolute calibrated against a high-temperature blackbody as primary standard for spectral irradiance at the Physikalisch-Technische Bundesanstalt (Germany). The PYR-ILIOS campaign was carried out in June to July 2016 at the Mauna Loa Observatory (Hawaii, USA, 3396 m a.s.l.) follows the four-month IRESPERAD campaign which was carried out in the summer 2011 at the Izaña Atmospheric Observatory (Canary Islands, 2367 m a.s.l.). We present here the results of the 3'week PYR-ILIOS campaign and compare them with the ATLAS 3 spectrum as well as from recently reprocessed NIR solar spectra obtained with SOLAR/SOLSPEC on ISS and SCIAMACHY on ENVISAT. The uncertainty budget of the PYR-ILIOS results will be discussed.

  3. BART: The Czech Autonomous Observatory

    Czech Academy of Sciences Publication Activity Database

    Nekola, Martin; Hudec, René; Jelínek, M.; Kubánek, P.; Štrobl, Jan; Polášek, Cyril

    2010-01-01

    Roč. 2010, Spec. Is. (2010), 103986/1-103986/5 ISSN 1687-7969. [Workshop on Robotic Autonomous Observatories. Málaga, 18.05.2009-21.05.2009] R&D Projects: GA ČR GA205/08/1207 Grant - others:ESA(XE) ESA-PECS project No. 98023; Spanish Ministry of Education and Science(ES) AP2003-1407 Institutional research plan: CEZ:AV0Z10030501 Keywords : robotic telescope * BART * gamma ray bursts Subject RIV: BN - Astronomy, Celestial Mechanics, Astrophysics http://www.hindawi.com/journals/aa/2010/103986.html

  4. The Astronomy and Space Science Concept Inventory: Assessment Instruments Aligned with the K-12 National Science Standards

    Science.gov (United States)

    Sadler, Philip M.

    2011-01-01

    We report on the development of an item test bank and associated instruments based on those K-12 national standards which involve astronomy and space science. Utilizing hundreds of studies in the science education research literature on student misconceptions, we have constructed 211 unique items that measure the degree to which students abandon such ideas for accepted scientific views. Piloted nationally with 7599 students and their 88 teachers spanning grades 5-12, the items reveal a range of interesting results, particularly student difficulties in mastering the NRC Standards and AAAS Benchmarks. Teachers generally perform well on items covering the standards of the grade level at which they teach, exhibiting few misconceptions of their own. Teachers dramatically overestimate their students’ performance, perhaps because they are unaware of their students’ misconceptions. Examples are given showing how the developed instruments can be used to assess the effectiveness of instruction and to evaluate the impact of professional development activities for teachers.

  5. Taurus Hill Observatory Scientific Observations for Pulkova Observatory during the 2016-2017 Season

    Science.gov (United States)

    Hentunen, V.-P.; Haukka, H.; Heikkinen, E.; Salmi, T.; Juutilainen, J.

    2017-09-01

    Taurus Hill Observatory (THO), observatory code A95, is an amateur observatory located in Varkaus, Finland. The observatory is maintained by the local astronomical association Warkauden Kassiopeia. THO research team has observed and measured various stellar objects and phenomena. Observatory has mainly focused on exoplanet light curve measurements, observing the gamma rays burst, supernova discoveries and monitoring. We also do long term monitoring projects.

  6. The Pulkovo Observatory in the last 50 years through the eyes of its Learned Secretary Yu. I. Vitinsky.

    Science.gov (United States)

    Zhukov, V. Yu.; Soboleva, T. V.

    A solar physicist, a Pulkovo astronomer, Yury Ivanovich Vitinsky (1926-2003) was the author of 210 scientific papers known in both Russia and abroad. He worked in the Observatory for about half a century (1953-2002) and held the office of the Learned Secretary of the Russian Academy of Sciences Main Astronomical Observatory for 35 years (1965-2000). In the last years of his life, Vitinsky brought his recollections that he titled "My Pulkovo" to the Main Astronomical Observatory Archive. His memoirs narrate about problems of the astronomical science, staff members and deeds of Pulkovo, things he thought of an events he was through. This is the half-a-century history of the Pulkovo Observatory in biographies of persons. The writer of the Recollections mentions the names of fifty persons most of whom are the Main Astronomical Observatory staff members that he worked with side by side. The memoirs provide accurate descriptions that are brief yet rather capacious of the author's Pulkovo colleagues, as well as other astronomers. The language of Vitinsky's recollection is good and clear. His memoirs contain moderate balanced views of people and events and provide objective and trustworthy data. "My Pulkovo" is an indispensable biographical source for the historian of the astronomical science, the Pulkovo Observatory and its scholarly staff members of the most recent decades. It is also just an interesting human document. In 2006, Yury Ivanovich would have been eighty.

  7. A future large-aperture UVOIR space observatory: reference designs

    Science.gov (United States)

    Rioux, Norman; Thronson, Harley; Feinberg, Lee; Stahl, H. Philip; Redding, Dave; Jones, Andrew; Sturm, James; Collins, Christine; Liu, Alice

    2015-09-01

    Our joint NASA GSFC/JPL/MSFC/STScI study team has used community-provided science goals to derive mission needs, requirements, and candidate mission architectures for a future large-aperture, non-cryogenic UVOIR space observatory. We describe the feasibility assessment of system thermal and dynamic stability for supporting coronagraphy. The observatory is in a Sun-Earth L2 orbit providing a stable thermal environment and excellent field of regard. Reference designs include a 36-segment 9.2 m aperture telescope that stows within a five meter diameter launch vehicle fairing. Performance needs developed under the study are traceable to a variety of reference designs including options for a monolithic primary mirror.

  8. Plan for a Sierra Nevada Hydrologic Observatory: Science Aims, Measurement Priorities, Research Opportunities and Expected Impacts

    Science.gov (United States)

    Bales, R.; Dozier, J.; Famiglietti, J.; Fogg, G.; Hopmans, J.; Kirchner, J.; Meixner, T.; Molotch, N.; Redmond, K.; Rice, R.; Sickman, J.; Warwick, J.

    2004-12-01

    In response to NSF's plans to establish a network of hydrologic observatories, a planning group is proposing a Sierra Nevada Hydrologic Observatory (SNHO). As argued in multiple consensus planning documents, the semi-arid mountain West is perhaps the highest priority for new hydrologic understanding. Based on input from over 100 individuals, it is proposed to initiate a mountain-range-scale study of the snow-dominated hydrology of the region, focusing on representative 1,000-5,000 km2 river basins originating in the Sierra Nevada and tributary to the Sacramento-San-Joaquin Delta. The SNHO objective is to provide the necessary infrastructure for improved understanding of surface-water and ground-water systems, their interactions and their linkages with ecosystems, biogeochemistry, agriculture, urban areas and water resources in semi-arid regions. The SNHO will include east-west transects of hydrological observations across the Sierra Nevada and into the basin and range system, in four distinct latitude bands that span much of the variability found in the semi-arid West. At least one transect will include agricultural and urban landscapes of the Great Central Valley. Investments in measurement systems will address scales from the mountain range down to the basin, headwater catchment and study plot. The intent is to provide representative measurements that will yield general knowledge as opposed to site-specific problem solving of a unique system. The broader, general science question posed by the planning group is: How do mountain hydrologic processes vary across landscapes, spanning a range of latitudes, elevations and thus climate, soils, geology and vegetation zones?\\" Embodied are additional broad questions for the hydrologic science community as a whole: (i) How do hydrologic systems that are subjected to multiple perturbations respond? (ii) How do pulses and changes propagate through the hydrologic system? (iii) What are the time lags and delays of stresses in

  9. Youth Science Ambassadors: Connecting Indigenous communities with Ocean Networks Canada tools to inspire future ocean scientists and marine resource managers

    Science.gov (United States)

    Pelz, M.; Hoeberechts, M.; Hale, C.; McLean, M. A.

    2017-12-01

    This presentation describes Ocean Networks Canada's (ONC) Youth Science Ambassador Program. The Youth Science Ambassadors are a growing network of youth in Canadian coastal communities whose role is to connect ocean science, ONC data, and Indigenous knowledge. By directly employing Indigenous youth in communities in which ONC operates monitoring equipment, ONC aims to encourage wider participation and interest in ocean science and exploration. Further, the Youth Science Ambassadors act as role models and mentors to other local youth by highlighting connections between Indigenous and local knowledge and current marine science efforts. Ocean Networks Canada, an initiative of the University of Victoria, develops, operates, and maintains cabled ocean observatory systems. These include technologies developed on the world-leading NEPTUNE and VENUS observatories as well as community observatories in the Arctic and coastal British Columbia. These observatories, large and small, enable communities, users, scientists, teachers, and students to monitor real-time and historical data from the local marine environment from anywhere on the globe. Youth Science Ambassadors are part of the Learning and Engagement team whose role includes engaging Indigenous communities and schools in ocean science through ONC's K-12 Ocean Sense education program. All of the data collected by ONC are freely available over the Internet for non-profit use, including disaster planning, community-based decision making, and education. The Youth Science Ambassadors support collaboration with Indigenous communities and schools by facilitating educational programming, encouraging participation in ocean data collection and analysis, and fostering interest in ocean science. In addition, the Youth Science Ambassadors support community collaboration in decision-making for instrument deployment locations and identify ways in which ONC can help to address any areas of concern raised by the community. This

  10. Community Observatories: Fostering Ideas that STEM From Ocean Sense: Local Observations. Global Connections.

    Science.gov (United States)

    Pelz, M. S.; Ewing, N.; Hoeberechts, M.; Riddell, D. J.; McLean, M. A.; Brown, J. C. K.

    2015-12-01

    Ocean Networks Canada (ONC) uses education and communication to inspire, engage and educate via innovative "meet them where they are, and take them where they need to go" programs. ONC data are accessible via the internet allowing for the promotion of programs wherever the learners are located. We use technologies such as web portals, mobile apps and citizen science to share ocean science data with many different audiences. Here we focus specifically on one of ONC's most innovative programs: community observatories and the accompanying Ocean Sense program. The approach is based on equipping communities with the same technology enabled on ONC's large cabled observatories. ONC operates the world-leading NEPTUNE and VENUS cabled ocean observatories and they collect data on physical, chemical, biological, and geological aspects of the ocean over long time periods, supporting research on complex Earth processes in ways not previously possible. Community observatories allow for similar monitoring on a smaller scale, and support STEM efforts via a teacher-led program: Ocean Sense. This program, based on local observations and global connections improves data-rich teaching and learning via visualization tools, interactive plotting interfaces and lesson plans for teachers that focus on student inquiry and exploration. For example, students use all aspects of STEM by accessing, selecting, and interpreting data in multiple dimensions, from their local community observatories to the larger VENUS and NEPTUNE networks. The students make local observations and global connections in all STEM areas. The first year of the program with teachers and students who use this innovative technology is described. Future community observatories and their technological applications in education, communication and STEM efforts are also described.

  11. A First Look at Target Mode Retrievals of CO2 from the Orbiting Carbon Observatory-2 (OCO-2)

    Science.gov (United States)

    Natraj, V.; Taylor, T.; Smyth, M.; Fisher, B.; O'Dell, C.; Pollock, H. R.; Crisp, D.

    2014-12-01

    The Orbiting Carbon Observatory-2 (OCO-2) is NASA's first dedicated Earth remote sensing satellite to study atmospheric carbon dioxide from space, and was launched successfully on July 2, 2014. OCO-2 is designed to quantify the sources and sinks of CO2by making highly precise measurements of its column abundance. OCO-2 has three science observation modes - nadir, glint and target. In the nadir mode, the satellite points the instrument to the local nadir, so that data can be collected along the ground track just below the spacecraft. In the glint mode, the spacecraft points the instrument toward the bright "glint" spot, where solar radiation is specularly reflected from the surface. In the target mode, the Observatory will lock its view onto a specific surface location, and will scan back and forth over that target while flying overhead. A target track pass can last for up to 9 minutes. Over that time period, the Observatory can acquire as many as 12,960 samples at local zenith angles that vary between 0° and 85°. Here, we analyze target track measurements over several of the OCO-2 validation sites where ground-based solar-looking Fourier Transform Spectrometers are located. The target scan serves two purposes. The first is to collect a large number of measurements over surface calibration and validation targets to assess the precision and accuracy of the retrieved column averaged CO2 dry air mole fraction (XCO2). The second is to look for spatial variations in column averaged CO2 dry air mole fraction (XCO2) in the vicinity of the target that could compromise the value of the measurements for calibration or validation. To meet both requirements, we compare XCO2 retrievals as a function of both observation angle and scan location, and investigate whether those variations are coming from instrument calibration, algorithmic deficiencies, aerosols/clouds or real CO2variations. Further, simulated retrievals indicate that target observations can show large sensitivity

  12. Beyond MOS and fibers: Optical Fourier-transform Imaging Unit for Cananea Observatory (OFIUCO)

    Science.gov (United States)

    Nieto-Suárez, M. A.; Rosales-Ortega, F. F.; Castillo, E.; García, P.; Escobedo, G.; Sánchez, S. F.; González, J.; Iglesias-Páramo, J.; Mollá, M.; Chávez, M.; Bertone, E.; et al.

    2017-11-01

    Many physical processes in astronomy are still hampered by the lack of spatial and spectral resolution, and also restricted to the field-of-view (FoV) of current 2D spectroscopy instruments available worldwide. It is due to that, many of the ongoing or proposed studies are based on large-scale imaging and/or spectroscopic surveys. Under this philosophy, large aperture telescopes are dedicated to the study of intrinsically faint and/or distance objects, covering small FoVs, with high spatial resolution, while smaller telescopes are devoted to wide-field explorations. However, future astronomical surveys, should be addressed by acquiring un-biases, spatially resolved, high-quality spectroscopic information for a wide FoV. Therefore, and in order to improve the current instrumental offer in the Observatorio Astrofísico Guillermo Haro (OAGH) in Cananea, Mexico (INAOE); and to explore a possible instrument for the future Telescopio San Pedro Mártir (6.5m), we are currently integrating at INAOE an instrument prototype that will provide us with un-biased wide-field (few arcmin) spectroscopic information, and with the flexibility of operating at different spectral resolutions (R 1-20000), with a spatial resolution limited by seeing, and therefore, to be used in a wide range of astronomical problems. This instrument called OFIUCO: Optical Fourier-transform Imaging Unit for Cananea Observatory, will make use of the Fourier Transform Spectroscopic technique, which has been proved to be feasible in the optical wavelength range (350-1000 nm) with designs such as SITELLE (CFHT). We describe here the basic technical description of a Fourier transform spectrograph with important modifications from previous astronomical versions, as well as the technical advantages and weakness, and the science cases in which this instrument can be implemented.

  13. ANALYZE THE KNOWLEDGE INQUIRY SCIENCE PHYSICS TEACHER CANDIDATES WITH ESSENCE INQUIRY SCIENCE TEST INSTRUMENT OPTIKA GEOMETRY

    Directory of Open Access Journals (Sweden)

    Wawan Bunawan

    2013-06-01

    Full Text Available The objective in this research to explore the relationship between ability of the knowledge essential features inquiry science and their reasons underlying sense of scientific inquiry for physics teacher candidates on content geometrical optics. The essential features of inquiry science are components that should arise during the learning process subject matter of geometrical optics reflectance of light on a flat mirror, the reflection of light on curved mirrors and refraction of light at the lens. Five of essential features inquiry science adopted from assessment system developed by the National Research Council. Content geometrical optics developed from an analysis of a college syllabus material. Based on the study of the essential features of inquiry and content develop the multiple choice diagnostic test three tier. Data were taken from the students who are taking courses in optics and wave from one the LPTK in North Sumatra totaled 38 students. Instruments showed Cronbach alpha reliability of 0.67 to test the essential features of inquiry science and 0.61 to there as on geometrical optics science inquiry.

  14. Exploring the Digital Universe with Europe's Astrophysical Virtual Observatory

    Science.gov (United States)

    2001-12-01

    need for virtual observatories has also been recognised by other astronomical communities. The National Science Foundation in the USA has awarded $10 million (EUR 11.4 m) for a National Virtual Observatory (NVO). The AVO project team has formed a close alliance with the NVO and both teams have representatives on each other's committees. It is clear to the NVO and AVO communities that there are no intrinsic boundaries to the virtual observatory concept and that all astronomers should be working towards a truly global virtual observatory that will enable new science to be carried out on the wealth of astronomical data held in the growing number of first-class international astronomical archives. AVO involves six partner organisations led by the European Southern Observatory (ESO) in Munich. The other partner organisations are the European Space Agency (ESA), the United Kingdom's ASTROGRID consortium, the CNRS-supported Centre de Données Astronomiques de Strasbourg (CDS) at the University Louis Pasteur in Strasbourg, the CNRS-supported TERAPIX astronomical data centre at the Institut d'Astrophysique in Paris and the Jodrell Bank Observatory at the University of Manchester. Note for editors A 13-minute background video (broadcast PAL) is available from ESO PR and the Hubble European Space Agency Information Centre (addresses below). It will also be transmitted via satellite on Wednesday 12 December 2001 from 12:00 to 12:15 CET on the ESA TV Service: http://television.esa.int

  15. Cryo-Vacuum Testing of the Integrated Science Instrument Module for the James Webb Space Telescope

    Science.gov (United States)

    Kimble, Randy A.; Davila, P. S.; Drury, M. P.; Glazer, S. D.; Krom, J. R.; Lundquist, R. A.; Mann, S. D.; McGuffey, D. B.; Perry, R. L.; Ramey, D. D.

    2011-01-01

    With delivery of the science instruments for the James Webb Space Telescope (JWST) to Goddard Space Flight Center (GSFC) expected in 2012, current plans call for the first cryo-vacuum test of the Integrated Science Instrument Module (ISIM) to be carried out at GSFC in early 2013. Plans are well underway for conducting this ambitious test, which will perform critical verifications of a number of optical, thermal, and operational requirements of the IS 1M hardware, at its deep cryogenic operating temperature. We describe here the facilities, goals, methods, and timeline for this important Integration & Test milestone in the JWST program.

  16. The brazilian indigenous planetary-observatory

    Science.gov (United States)

    Afonso, G. B.

    2003-08-01

    We have performed observations of the sky alongside with the Indians of all Brazilian regions that made it possible localize many indigenous constellations. Some of these constellations are the same as the other South American Indians and Australian aborigines constellations. The scientific community does not have much of this information, which may be lost in one or two generations. In this work, we present a planetary-observatory that we have made in the Park of Science Newton Freire-Maia of Paraná State, in order to popularize the astronomical knowledge of the Brazilian Indians. The planetary consists, essentially, of a sphere of six meters in diameter and a projection cylinder of indigenous constellations. In this planetary we can identify a lot of constellations that we have gotten from the Brazilian Indians; for instance, the four seasonal constellations: the Tapir (spring), the Old Man (summer), the Deer (autumn) and the Rhea (winter). A two-meter height wooden staff that is posted vertically on the horizontal ground similar to a Gnomon and stones aligned with the cardinal points and the soltices directions constitutes the observatory. A stone circle of ten meters in diameter surrounds the staff and the aligned stones. During the day we observe the Sun apparent motions and at night the indigenous constellations. Due to the great community interest in our work, we are designing an itinerant indigenous planetary-observatory to be used in other cities mainly by indigenous and primary schools teachers.

  17. The Virtual Solar Observatory at Eight and a Bit!

    Science.gov (United States)

    Davey, Alisdair R.; VSO Team

    2011-05-01

    The Virtual Solar Observatory (VSO) was the first virtual observatory in the solar and heliophysics data space. It first saw the light of day in 2003 with a mission to serve the solar physics community by enabling homogenous access to heterogeneous data, and hiding the gory details of doing so from the user. The VSO pioneered what was to become the "Small Box" methodology, setting out to provide only the services required to navigate the user to the data and then letting them directly transferred the data from the data providers. After eight and a bit years the VSO now serves data from 72 different instruments covering a multitude of space and ground based observatories, including data from SDO. Dealing with the volume of data from SDO has proved to be our most difficult challenge, forcing us from the small box approach to one where the various VSO sites not only serve SDO data, but are central to the distribution of the data within the US and to Europe and other parts of the world. With SDO data serving mostly in place we are now working on integration with the Heliophysics Event Knowledgebase (HEK) and including a number of new solar data sets in the VSO family. We have a complete VSO search interface in IDL now, enabling searching, downloading and processing solar data, all be done without leaving the IDL command line, and will be releasing a brand new web interface providing users and data providers, with the ability to create far more detailed and instrument specific searches. Eight years on and the VSO has plenty of work in front of it.

  18. Planetary Sciences practical experiences at the Master level with small telescopes

    Science.gov (United States)

    Sanchez-Lavega, A.; Perez-Hoyos, S.; del Rio-Gaztelurrutia, T.; Hueso, R.; Ordonez Etxeberria, I.; Rojas, J. F.

    2016-12-01

    The Master in Space Science and Technology of the Basque Country University UPV/EHU in Bilbao (Spain) has been taught during 7 years (A. Sanchez-Lavega et al., Eur. J. of Eng. Education. 2014). Along the different courses, a series of practical observations and studies of planetary sciences have been conducted with Master students, using telescopes with diameters in the range 28-50 cm pertaining to the Aula EspaZio Gela Observatory (http://www.ehu.eus/aula-espazio/presentacion.html). Simple instrumentation (cameras and a spectrograph) have been employed to study planetary atmospheres (dynamics and cloud structure) and orbital mechanics using the Galilean satellites. Here we present a sample of these studies, which have lead to publications in refereed journals and have been presented at different meetings with the coauthoring of the students. Plans for the future include involving the master students in high-resolution observations of Solar System planets using a remote controlled 36 cm telescope at the Calar Alto observatory in Southern Spain (separated 1000 km from the teaching facilities in Bilbao).

  19. SMAP Instrument Mechanical System Engineering

    Science.gov (United States)

    Slimko, Eric; French, Richard; Riggs, Benjamin

    2013-01-01

    The Soil Moisture Active Passive (SMAP) mission, scheduled for launch by the end of 2014, is being developed to measure the soil moisture and soil freeze/thaw state on a global scale over a three-year period. The accuracy, resolution, and global coverage of SMAP measurements are invaluable across many science and applications disciplines including hydrology, climate, carbon cycle, and the meteorological, environment, and ecology applications communities. The SMAP observatory is composed of a despun bus and a spinning instrument platform that includes both a deployable 6 meter aperture low structural frequency Astromesh reflector and a spin control system. The instrument section has engendered challenging mechanical system issues associated with the antenna deployment, flexible antenna pointing in the context of a multitude of disturbances, spun section mass properties, spin control system development, and overall integration with the flight system on both mechanical and control system levels. Moreover, the multitude of organizations involved, including two major vendors providing the spin subsystem and reflector boom assembly plus the flight system mechanical and guidance, navigation, and control teams, has led to several unique system engineering challenges. Capturing the key physics associated with the function of the flight system has been challenging due to the many different domains that are applicable. Key interfaces and operational concepts have led to complex negotiations because of the large number of organizations that integrate with the instrument mechanical system. Additionally, the verification and validation concerns associated with the mechanical system have had required far-reaching involvement from both the flight system and other subsystems. The SMAP instrument mechanical systems engineering issues and their solutions are described in this paper.

  20. NASA's Great Observatories Celebrate the International Year of Astronomy

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] Click on the image for larger version In 1609, Galileo improved the newly invented telescope, turned it toward the heavens, and revolutionized our view of the universe. In celebration of the 400th anniversary of this milestone, 2009 has been designated as the International Year of Astronomy. Today, NASA's Great Observatories are continuing Galileo's legacy with stunning images and breakthrough science from the Hubble Space Telescope, the Spitzer Space Telescope, and the Chandra X-ray Observatory. While Galileo observed the sky using visible light seen by the human eye, technology now allows us to observe in many wavelengths, including Spitzer's infrared view and Chandra's view in X-rays. Each wavelength region shows different aspects of celestial objects and often reveals new objects that could not otherwise be studied. This image of the spiral galaxy Messier 101 is a composite of views from Spitzer, Hubble, and Chandra. The red color shows Spitzer's view in infrared light. It highlights the heat emitted by dust lanes in the galaxy where stars can form. The yellow color is Hubble's view in visible light. Most of this light comes from stars, and they trace the same spiral structure as the dust lanes. The blue color shows Chandra's view in X-ray light. Sources of X-rays include million-degree gas, exploded stars, and material colliding around black holes. Such composite images allow astronomers to see how features seen in one wavelength match up with those seen in another wavelength. It's like seeing with a camera, night vision goggles, and X-ray vision all at once. In the four centuries since Galileo, astronomy has changed dramatically. Yet our curiosity and quest for knowledge remain the same. So, too, does our wonder at the splendor of the universe. The International Year of Astronomy Great Observatories Image Unveiling is supported by the NASA Science Mission Directorate Astrophysics Division. The project is a

  1. On the possibility of producing definitive magnetic observatory data within less than one year

    Science.gov (United States)

    Mandić, Igor; Korte, Monika

    2017-04-01

    Geomagnetic observatory data are fundamental in geomagnetic field studies and are widely used in other applications. Often they are combined with satellite and ground survey data. Unfortunately, the observatory definitive data are only available with a time lag ranging from several months up to more than a year. The reason for this lag is the annual production of the final calibration values, i.e. baselines that are used to correct preliminary data from continuously recording magnetometers. In this paper, we will show that the preparation of definitive geomagnetic data is possible within a calendar year and presents an original method for prompt and automatic estimation of the observatory baselines. The new baselines, obtained in a mostly automatic manner, are compared with the baselines reported on INTERMAGNET DVDs for the 2009-2011 period. The high quality of the baselines obtained by the proposed method indicates its suitability for data processing in fully automatic observatories when automated absolute instruments will be deployed at remote sites.

  2. Nuclear instrument engineering - the measuring and informative basis of nuclear science and technology

    International Nuclear Information System (INIS)

    Matveev, V.V.; Krasheninnikov, I.S.; Murin, I.D.; Stas', K.N.

    1977-01-01

    The cornerstones of developing nuclear instrument engineering in the USSR are shortly discussed. The industry is based on a well developed theory. A system approach is a characteristic feature of the present-day measuring and control systems engineering. Major functions of reactor instruments measuring different types of ionizing radiation are discussed at greater length. Nuclear measuring and control instruments and methods are widely used in different fields of science and technoloay and in different industries in the USSR. The efficient and safe operation of a nuclear facility is underlined to depend strongly upon a correlation between a technological process and the information and control system of the facility

  3. Geomagnetic Observatory Data for Real-Time Applications

    Science.gov (United States)

    Love, J. J.; Finn, C. A.; Rigler, E. J.; Kelbert, A.; Bedrosian, P.

    2015-12-01

    The global network of magnetic observatories represents a unique collective asset for the scientific community. Historically, magnetic observatories have supported global magnetic-field mapping projects and fundamental research of the Earth's interior and surrounding space environment. More recently, real-time data streams from magnetic observatories have become an important contributor to multi-sensor, operational monitoring of evolving space weather conditions, especially during magnetic storms. In this context, the U.S. Geological Survey (1) provides real-time observatory data to allied space weather monitoring projects, including those of NOAA, the U.S. Air Force, NASA, several international agencies, and private industry, (2) collaborates with Schlumberger to provide real-time geomagnetic data needed for directional drilling for oil and gas in Alaska, (3) develops products for real-time evaluation of hazards for the electric-power grid industry that are associated with the storm-time induction of geoelectric fields in the Earth's conducting lithosphere. In order to implement strategic priorities established by the USGS Natural Hazards Mission Area and the National Science and Technology Council, and with a focus on developing new real-time products, the USGS is (1) leveraging data management protocols already developed by the USGS Earthquake Program, (2) developing algorithms for mapping geomagnetic activity, a collaboration with NASA and NOAA, (3) supporting magnetotelluric surveys and developing Earth conductivity models, a collaboration with Oregon State University and the NSF's EarthScope Program, (4) studying the use of geomagnetic activity maps and Earth conductivity models for real-time estimation of geoelectric fields, (5) initiating geoelectric monitoring at several observatories, (6) validating real-time estimation algorithms against historical geomagnetic and geoelectric data. The success of these long-term projects is subject to funding constraints

  4. Second Chandra Instrument Activated August 28

    Science.gov (United States)

    1999-08-01

    Cambridge, MA--NASA's Chandra X-ray Observatory opened a new era in astronomy Saturday, August 28, by making the most precise measurements ever recorded of the energy output from the 10 million degree corona of a star. Last weekend's observations came after the successful activation of an instrument developed by MIT that will allow a one-thousand-fold improvement in the capability to measure X-ray spectra from space. The new measurements, made with the High Energy Transmission Grating Spectrometer, join spectacular images taken last week by Chandra of the aftermath of a gigantic stellar explosion. The spectrometer is one of four key instruments aboard Chandra, and the second to be activated. The others will be turned on over the next two weeks. The spectrometer activated yesterday spreads the X-rays from Chandra's mirrors into a spectrum, much as a prism spreads light into its colors. The spectrum then can be read by Chandra's imaging detectors like a kind of cosmic bar code from which scientists can deduce the chemical composition and temperature of the corona. A corona is a region of hot gas and magnetic loops that extend hundreds of thousands of miles above the star's visible surface and is best studied with X-rays. "The success of the new spectrometer is definitely a major milestone for modern astronomy," said MIT Professor Claude R. Canizares, principal investigator for the instrument and associate director of the Chandra X-ray Observatory Center (CXC). "Within the first hour we had obtained the best X-ray spectrum ever recorded for a celestial source. We can already see unexpected features that will teach us new things about stars and about matter at high temperatures." The spectrometer measured X-rays from the star Capella, which is 40 light years away in the constellation Auriga. Capella is actually two stars orbiting one another and possibly interacting in ways that pump extra heat into the corona, which appears more active than that of the Sun. How a star

  5. The Observatory as Laboratory: Spectral Analysis at Mount Wilson Observatory

    Science.gov (United States)

    Brashear, Ronald

    2018-01-01

    This paper will discuss the seminal changes in astronomical research practices made at the Mount Wilson Observatory in the early twentieth century by George Ellery Hale and his staff. Hale’s desire to set the agenda for solar and stellar astronomical research is often described in terms of his new telescopes, primarily the solar tower observatories and the 60- and 100-inch telescopes on Mount Wilson. This paper will focus more on the ancillary but no less critical parts of Hale’s research mission: the establishment of associated “physical” laboratories as part of the observatory complex where observational spectral data could be quickly compared with spectra obtained using specialized laboratory equipment. Hale built a spectroscopic laboratory on the mountain and a more elaborate physical laboratory in Pasadena and staffed it with highly trained physicists, not classically trained astronomers. The success of Hale’s vision for an astronomical observatory quickly made the Carnegie Institution’s Mount Wilson Observatory one of the most important astrophysical research centers in the world.

  6. First results from Orbiting Carbon Observatory-2 (OCO-2) and prospects for OCO-3

    Science.gov (United States)

    Eldering, Annmarie; Basilio, Ralph; Schimel, David; O'Dell, Chris

    2017-04-01

    Since September 6, 2014, NASA's Orbiting Carbon Observatory-2 (OCO-2) instrument has been routinely returning almost one million soundings of the column averaged CO2 dry air mole fraction, XCO2, over the sunlit hemisphere each day. On monthly time scales, 7 to 21% of these soundings are sufficiently cloud free to yield full-column estimates of XCO2 of the with single sounding random errors near 0.5 parts per million (ppm) at solar zenith angles as large as 70 degrees. These XCO2 estimates are being validated against results obtained from the Total Carbon Column Observing Network (TCCON) and other standards to assess their accuracy and correct regional scale biases. After correction, the median bias between OCO-2 and TCCON XCO2 estimates is less than 0.5 ppm, and root-mean-square (RMS) differences are typically less than 1.5 ppm. The OCO-2 data are now being used to investigate the impacts of the 2015/2016 El Nino on the carbon cycle, as well as examples of local emission enhancements and the seasonal patterns of solar induced fluorescence. Highlights of the latest science findings will be presented. The Orbiting Carbon Observatory-3 (OCO-3) instrument will explore, for the first time, daily variations in the release and uptake of carbon dioxide by plants and trees in the major tropical rainforests of South America, Africa, and Southeast Asia, the largest stores of aboveground carbon on our planet. NASA will develop and assemble the instrument using spare materials from OCO-2 and host the instrument on the International Space Station (ISS) (earliest launch readiness in early 2018.) The low-inclination ISS orbit lets OCO-3 sample the tropics and sub-tropics across the full range of daylight hours with dense observations at northern and southern mid-latitudes (+/- 52°). At the same time, OCO-3 will also collect measurements of solar-induced chlorophyll fluorescence (SIF) over these areas. The instrument utilizes an agile, 2-axis pointing mechanism (PMA), providing

  7. The Nature of Science Instrument-Elementary (NOSI-E): the end of the road?

    Science.gov (United States)

    Peoples, Shelagh M; O'Dwyer, Laura M

    2014-01-01

    This research continues prior work published in this journal (Peoples, O'Dwyer, Shields and Wang, 2013). The first paper described the scale development, psychometric analyses and part-validation of a theoretically-grounded Rasch-based instrument, the Nature of Science Instrument-Elementary (NOSI-E). The NOSI-E was designed to measure elementary students' understanding of the Nature of Science (NOS). In the first paper, evidence was provided for three of the six validity aspects (content, substantive and generalizability) needed to support the construct validity of the NOSI-E. The research described in this paper examines two additional validity aspects (structural and external). The purpose of this study was to determine which of three competing internal models provides reliable, interpretable, and responsive measures of students' understanding of NOS. One postulate is that the NOS construct is unidimensional;. alternatively, the NOS construct is composed of five independent unidimensional constructs (the consecutive approach). Lastly, the NOS construct is multidimensional and composed of five inter-related but separate dimensions. The vast body of evidence supported the claim that the NOS construct is multidimensional. Measures from the multidimensional model were positively related to student science achievement and students' perceptions of their classroom environment; this provided supporting evidence for the external validity aspect of the NOS construct. As US science education moves toward students learning science through engaging in authentic scientific practices and building learning progressions (NRC, 2012), it will be important to assess whether this new approach to teaching science is effective, and the NOSI-E may be used as a measure of the impact of this reform.

  8. The Student Actions Coding Sheet (SACS): An instrument for illuminating the shifts toward student-centered science classrooms

    Science.gov (United States)

    Erdogan, Ibrahim; Campbell, Todd; Hashidah Abd-Hamid, Nor

    2011-07-01

    This study describes the development of an instrument to investigate the extent to which student-centered actions are occurring in science classrooms. The instrument was developed through the following five stages: (1) student action identification, (2) use of both national and international content experts to establish content validity, (3) refinement of the item pool based on reviewer comments, (4) pilot testing of the instrument, and (5) statistical reliability and item analysis leading to additional refinement and finalization of the instrument. In the field test, the instrument consisted of 26 items separated into four categories originally derived from student-centered instruction literature and used by the authors to sort student actions in previous research. The SACS was administered across 22 Grade 6-8 classrooms by 22 groups of observers, with a total of 67 SACS ratings completed. The finalized instrument was found to be internally consistent, with acceptable estimates from inter-rater intraclass correlation reliability coefficients at the p Observation Protocol. Based on the analyses completed, the SACS appears to be a useful instrument for inclusion in comprehensive assessment packages for illuminating the extent to which student-centered actions are occurring in science classrooms.

  9. The SPICE concept - An approach to providing geometric and other ancillary information needed for interpretation of data returned from space science instruments

    Science.gov (United States)

    Acton, Charles H., Jr.

    1990-01-01

    The Navigation Ancillary Information Facility (NAIF), acting under the direction of NASA's Office of Space Science and Applications, and with substantial participation of the planetary science community, is designing and implementing an ancillary data system - called SPICE - to assist scientists in planning and interpreting scientific observations taken from spaceborne instruments. The principal objective of the implemented SPICE system is that it will hold the essential geometric and related ancillary information needed to recover the full value of science instrument data, and that it will facilitate correlations of individual instrument datasets with data obtained from other instruments on the same or other spacecraft.

  10. One year on VESPA, a community-driven Virtual Observatory in Planetary Science

    Science.gov (United States)

    Erard, S.; Cecconi, B.; Le Sidaner, P.; Rossi, A. P.; Capria, M. T.; Schmitt, B.; Andre, N.; Vandaele, A. C.; Scherf, M.; Hueso, R.; Maattanen, A. E.; Thuillot, W.; Achilleos, N.; Marmo, C.; Santolik, O.; Benson, K.

    2016-12-01

    The Europlanet H2020 program started on 1/9/2015 for 4 years. It includes an activity to adapt Virtual Observatory (VO) techniques to Planetary Science data called VESPA. The objective is to facilitate searches in big archives as well as sparse databases, to provide simple data access and on-line visualization, and to allow small data providers to make their data available in an interoperable environment with minimum effort. The VESPA system, based on a prototype developed in a previous program [1], has been hugely improved during the first year of Europlanet H2020: the infrastructure has been upgraded to describe data in many fields more accurately; the main user search interface (http://vespa.obspm.fr) has been redesigned to provide more flexibility; alternative ways to access Planetary Science data services from VO tools are being implemented in addition to receiving data from the main interface; VO tools are being improved to handle specificities of Solar System data, e.g. measurements in reflected light, coordinate systems, etc. Existing data services have been updated, and new ones have been designed. The global objective (50 data services) is already overstepped, with 54 services open or being finalized. A procedure to install data services has been documented, and hands-on sessions are organized twice a year at EGU and EPSC; this is intended to favour the installation of services by individual research teams, e.g. to distribute derived data related to a published study. In complement, regular discussions are held with big data providers, starting with space agencies (IPDA). Common projects with ESA and NASA's PDS have been engaged, which should lead to a connection between PDS4 and EPN-TAP. In parallel, a Solar System Interest Group has been decided in IVOA; the goal is here to adapt existing astronomy standards to Planetary Science.Future steps will include the development of a connection between the VO world and GIS tools, and integration of Heliophysics

  11. Indian moored observatory in the Arctic for long-term in situ data collection

    Directory of Open Access Journals (Sweden)

    R Venkatesan

    2016-08-01

    Full Text Available This article describes the first Indian arctic multi-sensor mooring (IndARC observatory in Kongsfjorden of Arctic waters. The Ministry of Earth Sciences evolved a unique moored observatory ‘IndARC’ with suite of sensors for physico-chemical and oceanographic in situ long-term data collection. The Arctic Ocean plays an important role in governing the earth’s climate and also faithfully records its past climatic history and represents a significant gap in ocean observations. This indigenously designed and installed observatory IndARC, for the first time, collected various parameters from July 2014 to July 2015. The uniqueness of this system, the challenges faced and results from data collected are presented in this article.

  12. NASA's Great Observatories Celebrate International Year of Astronomy

    Science.gov (United States)

    2009-11-01

    A never-before-seen view of the turbulent heart of our Milky Way galaxy is being unveiled by NASA on Nov. 10. This event will commemorate the 400 years since Galileo first turned his telescope to the heavens in 1609. In celebration of this International Year of Astronomy, NASA is releasing images of the galactic center region as seen by its Great Observatories to more than 150 planetariums, museums, nature centers, libraries, and schools across the country. The sites will unveil a giant, 6-foot-by-3-foot print of the bustling hub of our galaxy that combines a near-infrared view from the Hubble Space Telescope, an infrared view from the Spitzer Space Telescope, and an X-ray view from the Chandra X-ray Observatory into one multiwavelength picture. Experts from all three observatories carefully assembled the final image from large mosaic photo surveys taken by each telescope. This composite image provides one of the most detailed views ever of our galaxy's mysterious core. Participating institutions also will display a matched trio of Hubble, Spitzer, and Chandra images of the Milky Way's center on a second large panel measuring 3 feet by 4 feet. Each image shows the telescope's different wavelength view of the galactic center region, illustrating not only the unique science each observatory conducts, but also how far astronomy has come since Galileo. The composite image features the spectacle of stellar evolution: from vibrant regions of star birth, to young hot stars, to old cool stars, to seething remnants of stellar death called black holes. This activity occurs against a fiery backdrop in the crowded, hostile environment of the galaxy's core, the center of which is dominated by a supermassive black hole nearly four million times more massive than our Sun. Permeating the region is a diffuse blue haze of X-ray light from gas that has been heated to millions of degrees by outflows from the supermassive black hole as well as by winds from massive stars and by stellar

  13. Brazil to Join the European Southern Observatory

    Science.gov (United States)

    2010-12-01

    The Federative Republic of Brazil has yesterday signed the formal accession agreement paving the way for it to become a Member State of the European Southern Observatory (ESO). Following government ratification Brazil will become the fifteenth Member State and the first from outside Europe. On 29 December 2010, at a ceremony in Brasilia, the Brazilian Minister of Science and Technology, Sergio Machado Rezende and the ESO Director General, Tim de Zeeuw signed the formal accession agreement aiming to make Brazil a Member State of the European Southern Observatory. Brazil will become the fifteen Member State and the first from outside Europe. Since the agreement means accession to an international convention, the agreement must now be submitted to the Brazilian Parliament for ratification [1]. The signing of the agreement followed the unanimous approval by the ESO Council during an extraordinary meeting on 21 December 2010. "Joining ESO will give new impetus to the development of science, technology and innovation in Brazil as part of the considerable efforts our government is making to keep the country advancing in these strategic areas," says Rezende. The European Southern Observatory has a long history of successful involvement with South America, ever since Chile was selected as the best site for its observatories in 1963. Until now, however, no non-European country has joined ESO as a Member State. "The membership of Brazil will give the vibrant Brazilian astronomical community full access to the most productive observatory in the world and open up opportunities for Brazilian high-tech industry to contribute to the European Extremely Large Telescope project. It will also bring new resources and skills to the organisation at the right time for them to make a major contribution to this exciting project," adds ESO Director General, Tim de Zeeuw. The European Extremely Large Telescope (E-ELT) telescope design phase was recently completed and a major review was

  14. Development and validation of an instrument to evaluate science teachers' assessment beliefs and practices

    Science.gov (United States)

    Genc, Evrim

    The primary purpose of this study was to develop a valid and reliable instrument to examine science teachers' assessment beliefs and practices in science classrooms. The present study also investigated the relationship between teachers' beliefs and practices in terms of assessment issues in science, their perceptions of the factors that influenced their assessment practices and their feelings towards high-stakes testing. The participants of the study were 408 science teachers teaching at middle and high school levels in the State of Florida. Data were collected through two modes of administration of the instrument as a paper-and-pencil and a web-based form. The response rate for paper-and-pencil administration was estimated as 68% whereas the response for the web administration was found to be 27%. Results from the various dimensions of validity and reliability analyses revealed that the 24 item-four-factor belief and practice measures were psychometrically sound and conceptually anchored measures of science teachers' assessment beliefs and self-reported practices. Reliability estimates for the belief measure ranged from .83 to .91 whereas alpha values for the practice measure ranged from .56 to .90. Results from the multigroup analysis supported that the instrument has the same theoretical structure across both administration groups. Therefore, future researchers may use either a paper-and-pencil or web-based format of the instrument. This study underscored a discrepancy between what teachers believe and how they act in classroom settings. It was emphasized that certain factors were mediating the dynamics between the belief and the practice. The majority of teachers reported that instruction time, class size, professional development activities, availability of school funding, and state testing mandates impact their assessment routines. Teachers reported that both the preparation process and the results of the test created unbelievable tension both on students and

  15. Computing Infrastructure and Remote, Parallel Data Mining Engine for Virtual Observatories, Phase I

    Data.gov (United States)

    National Aeronautics and Space Administration — We propose to develop a state-of-the-art data mining engine that extends the functionality of Virtual Observatories (VO) from data portal to science analysis...

  16. Radioecological Observatories - Breeding Grounds for Innovative Research

    Energy Technology Data Exchange (ETDEWEB)

    Steiner, Martin; Urso, Laura; Wichterey, Karin; Willrodt, Christine [Bundesamt fuer Strahlenschutz - BfS, Willy-Brandt-Strasse 5, 38226 Salzgitter (Germany); Beresford, Nicholas A.; Howard, Brenda [NERC Centre for Ecology and Hydrology - CEH, Lancaster Environment Centre, Library Av., Bailrigg, Lancaster, LA1 4AP (United Kingdom); Bradshaw, Clare; Stark, Karolina [Stockholms Universitet - SU, Universitetsvaegen 10, SE-10691 Stockholm (Sweden); Dowdall, Mark; Liland, Astrid [Norwegian Radiation Protection Authority - NRPA, P.O. Box 55, NO-1332 Oesteraas (Norway); Eyrolle- Boyer, Frederique; Guillevic, Jerome; Hinton, Thomas [Institut de Radioprotection et de Surete Nucleaire - IRSN, 31, Avenue de la Division Leclerc, 92260 Fontenay-aux-Roses (France); Gashchak, Sergey [Chornobyl Center for Nuclear Safety, Radioactive Waste and Radioecology - Chornobyl Center, 77th Gvardiiska Dyviiya str.7/1, 07100 Slavutych (Ukraine); Hutri, Kaisa-Leena; Ikaeheimonen, Tarja; Muikku, Maarit; Outola, Iisa [Radiation and Nuclear Safety Authority - STUK, P.O. Box 14, 00881 Helsinki (Finland); Michalik, Boguslaw [Glowny Instytut Gornictwa - GIG, Plac Gwarkow 1, 40-166 Katowice (Poland); Mora, Juan Carlos; Real, Almudena; Robles, Beatriz [Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas - CIEMAT, Avenida complutense, 40, 28040 Madrid (Spain); Oughton, Deborah; Salbu, Brit [Norwegian University of Life Sciences - NMBU, P.O. Box 5003, NO-1432 Aas (Norway); Sweeck, Lieve [Studiecentrum voor Kernenergie/Centre d' Etude de l' Energie Nucleaire (SCK.CEN), Avenue Herrmann- Debroux 40, BE-1160 Brussels (Belgium); Yoschenko, Vasyl [National University of Life and Environmental Sciences of Ukraine (NUBiP of Ukraine), Herojiv Obrony st., 15, Kyiv-03041 (Ukraine)

    2014-07-01

    Within the EC-funded (FP7) Network of Excellence STAR (Strategy for Allied Radioecology, www.star-radioecology.org) the concept of Radioecological Observatories is currently being implemented on a European level for the first time. Radioecological Observatories are radioactively (and chemically) contaminated field sites that will provide a focus for joint long-term radioecological research. The benefit of this innovative approach is to create synergistic research collaborations by sharing expertise, ideas, data and resources. Research at the Radioecological Observatories will primarily focus on radioecological challenges outlined in the Strategic Research Agenda (SRA). Mechanisms to use these sites will be established under the EC-funded project COMET (Coordination and Implementation of a Pan-European Instrument for Radioecology, www.comet-radioecology.org). The European Radioecological Observatory sites were selected using a structured, progressive approach that was transparent, consistent and objective. A first screening of potential candidate sites was conducted based on the following exclusion criteria: long-term perspective for shared field work and suitability for addressing the radioecological challenges of the SRA. The proposed sites included former uranium mining and milling sites in France and Germany, the Chernobyl Exclusion Zone (CEZ) in Ukraine/Belarus and the Upper Silesian Coal Basin (USCB) in Poland. All candidate sites were prioritized based on evaluation criteria which comprised scientific issues, available infrastructure, administrative/legal constraints and financial considerations. Multi-criteria decision analysis, group discussions and recommendations provided by external experts were combined to obtain a preference order among the suggested sites. Using this approach, the Upper Silesian Coal Basin (USCB) in Poland and the Chernobyl Exclusion Zone (CEZ) were selected as Radioecological Observatories. The two sites have similar multi

  17. Integrated Instrument Simulator Suites for Earth Science

    Science.gov (United States)

    Tanelli, Simone; Tao, Wei-Kuo; Matsui, Toshihisa; Hostetler, Chris; Hair, John; Butler, Carolyn; Kuo, Kwo-Sen; Niamsuwan, Noppasin; Johnson, Michael P.; Jacob, Joseph C.; hide

    2012-01-01

    The NASA Earth Observing System Simulators Suite (NEOS3) is a modular framework of forward simulations tools for remote sensing of Earth's Atmosphere from space. It was initiated as the Instrument Simulator Suite for Atmospheric Remote Sensing (ISSARS) under the NASA Advanced Information Systems Technology (AIST) program of the Earth Science Technology Office (ESTO) to enable science users to perform simulations based on advanced atmospheric and simple land surface models, and to rapidly integrate in a broad framework any experimental or innovative tools that they may have developed in this context. The name was changed to NEOS3 when the project was expanded to include more advanced modeling tools for the surface contributions, accounting for scattering and emission properties of layered surface (e.g., soil moisture, vegetation, snow and ice, subsurface layers). NEOS3 relies on a web-based graphic user interface, and a three-stage processing strategy to generate simulated measurements. The user has full control over a wide range of customizations both in terms of a priori assumptions and in terms of specific solvers or models used to calculate the measured signals.This presentation will demonstrate the general architecture, the configuration procedures and illustrate some sample products and the fundamental interface requirements for modules candidate for integration.

  18. The SLICE, CHESS, and SISTINE Ultraviolet Spectrographs: Rocket-Borne Instrumentation Supporting Future Astrophysics Missions

    Science.gov (United States)

    France, Kevin; Hoadley, Keri; Fleming, Brian T.; Kane, Robert; Nell, Nicholas; Beasley, Matthew; Green, James C.

    2016-03-01

    NASA’s suborbital program provides an opportunity to conduct unique science experiments above Earth’s atmosphere and is a pipeline for the technology and personnel essential to future space astrophysics, heliophysics, and atmospheric science missions. In this paper, we describe three astronomy payloads developed (or in development) by the Ultraviolet Rocket Group at the University of Colorado. These far-ultraviolet (UV) (100-160nm) spectrographic instruments are used to study a range of scientific topics, from gas in the interstellar medium (accessing diagnostics of material spanning five orders of magnitude in temperature in a single observation) to the energetic radiation environment of nearby exoplanetary systems. The three instruments, Suborbital Local Interstellar Cloud Experiment (SLICE), Colorado High-resolution Echelle Stellar Spectrograph (CHESS), and Suborbital Imaging Spectrograph for Transition region Irradiance from Nearby Exoplanet host stars (SISTINE) form a progression of instrument designs and component-level technology maturation. SLICE is a pathfinder instrument for the development of new data handling, storage, and telemetry techniques. CHESS and SISTINE are testbeds for technology and instrument design enabling high-resolution (R>105) point source spectroscopy and high throughput imaging spectroscopy, respectively, in support of future Explorer, Probe, and Flagship-class missions. The CHESS and SISTINE payloads support the development and flight testing of large-format photon-counting detectors and advanced optical coatings: NASA’s top two technology priorities for enabling a future flagship observatory (e.g. the LUVOIR Surveyor concept) that offers factors of ˜50-100 gain in UV spectroscopy capability over the Hubble Space Telescope. We present the design, component level laboratory characterization, and flight results for these instruments.

  19. Grass Roots Design for the Ocean Science of Tomorrow

    Science.gov (United States)

    Jul, S.; Peach, C. L.; Kilb, D. L.; Schofield, O.; Fisher, C.; Quintana, C.; Keen, C. S.

    2010-12-01

    Current technologies offer the opportunity for ocean science to expand its traditional expeditionary base by embracing e-science methods of continuous interactive real-time research. The Ocean Observatories Initiative Cyberinfrastructure (OOI CI) is an NSF-funded effort to develop a national cyberinfrastructure that will allow researchers, educators and others to share in this new type of oceanography. The OOI is an environmental observatory spanning coastal waters to the deep ocean, enabled by the CI to offer scientists continuous interactive access to instruments in the ocean, and allow them to search, subscribe to and access real-time or archival data streams. It will also supply interactive analysis and visualization tools, and a virtual social environment for discovering and realizing collaborative opportunities. Most importantly, it provides an extensible open-access cyberinfrastructure that supports integration of new technologies and observatories, and which will allow adoption of its tools elsewhere, such as by the Integrated Ocean Observing System (IOOS). The eventual success of such a large and flexible system requires the input of a large number of people, and user-centered design has been a driving philosophy of the OOI CI from its beginning. Support for users’ real needs cannot be designed as an add-on or casual afterthought, but must be deeply embedded in all aspects of a project, from inception through architecture, implementation, and deployment. The OOI CI strategy is to employ the skills and knowledge of a small number of user experience professionals to channel and guide a very large collective effort to deliver tools, interfaces and interactions that are intellectually stimulating, scientifically productive, and conducive to innovation. Participation from all parts of the user community early in the design process is vital to meeting these goals. The OOI user experience team will be on hand to meet members of the Earth and ocean sciences

  20. Computing Infrastructure and Remote, Parallel Data Mining Engine for Virtual Observatories, Phase II

    Data.gov (United States)

    National Aeronautics and Space Administration — SciberQuest, Inc. proposes to develop a state-of-the-art data mining engine that extends the functionality of Virtual Observatories (VO) from data portal to science...

  1. Development and Validation of Nature of Science Instrument for Elementary School Students

    Science.gov (United States)

    Hacieminoglu, Esme; Yilmaz-Tüzün, Özgül; Ertepinar, Hamide

    2014-01-01

    The purposes of this study were to develop and validate an instrument for assessing elementary students' nature of science (NOS) views and to explain the elementary school students' NOS views, in terms of varying grade levels and gender. The sample included 782 students enrolled in sixth, seventh, and eighth grades. Exploratory factor analysis…

  2. Riccardo Giacconi to Receive National Medal of Science

    Science.gov (United States)

    2005-02-01

    Riccardo Giacconi, very recently retired President of Associated Universities, Inc. (AUI), will be awarded the National Medal of Science by President George W. Bush on March 14, according to the White House. Giacconi, who received the Nobel Prize in Physics in 2002, will be honored for his pioneering research in X-ray astronomy and for his visionary leadership of major astronomy facilities. Established by Congress in 1959, the National Medal of Science is the Nation's highest honor for American scientists and is awarded annually by the President of the United States to individuals "deserving of special recognition for their outstanding contributions to knowledge." "We are extremely proud that Riccardo Giacconi has been selected to receive the nation's highest award for scientific achievement," said current AUI President Ethan J. Schreier, a long-term colleague of Dr. Giacconi. "It is another fitting recognition for an outstanding scientific career that has enhanced our basic understanding of the universe," Schreier added. Giacconi, known as the father of X-ray astronomy, used X-ray detectors launched on rockets to discover the first cosmic X-ray source in 1962. Because X-ray radiation is absorbed in Earth's atmosphere, space-based instruments are necessary to study it. Giacconi outlined a methodical program to investigate this new X-ray universe and, working with his research group at American Science and Engineering, Inc. in Cambridge, Massachusetts, developed the first space satellite dedicated to the new field of X-ray astronomy. Named Uhuru, this X-ray satellite observatory was launched in 1970 and subsequently discovered hundreds of X-ray sources. The ground-breaking work of Giacconi and his group led to the discovery of black holes, which to that point had been hypothesized but never seen. Giacconi was also the first to prove that the universe contains background radiation of X-ray light. Riccardo Giacconi has played a key role in many other landmark

  3. Polychromatic X-ray Micro- and Nano-Beam Science and Instrumentation

    Science.gov (United States)

    Ice, G. E.; Larson, B. C.; Liu, W.; Barabash, R. I.; Specht, E. D.; Pang, J. W. L.; Budai, J. D.; Tischler, J. Z.; Khounsary, A.; Liu, C.; Macrander, A. T.; Assoufid, L.

    2007-01-01

    Polychromatic x-ray micro- and nano-beam diffraction is an emerging nondestructive tool for the study of local crystalline structure and defect distributions. Both long-standing fundamental materials science issues, and technologically important questions about specific materials systems can be uniquely addressed. Spatial resolution is determined by the beam size at the sample and by a knife-edge technique called differential aperture microscopy that decodes the origin of scattering from along the penetrating x-ray beam. First-generation instrumentation on station 34-ID-E at the Advanced Photon Source (APS) allows for nondestructive automated recovery of the three-dimensional (3D) local crystal phase and orientation. Also recovered are the local elastic-strain and the dislocation tensor distributions. New instrumentation now under development will further extend the applications of polychromatic microdiffraction and will revolutionize materials characterization.

  4. Polychromatic X-ray Micro- and Nano-Beam Science and Instrumentation

    International Nuclear Information System (INIS)

    Ice, G.E.; Larson, Ben C.; Liu, Wenjun; Barabash, Rozaliya; Specht, Eliot D; Pang, Judy; Budai, John D.; Tischler, Jonathan Zachary; Khounsary, Ali; Liu, Chian; Macrander, Albert T.; Assoufid, Lahsen

    2007-01-01

    Polychromatic x-ray micro- and nano-beam diffraction is an emerging nondestructive tool for the study of local crystalline structure and defect distributions. Both long-standing fundamental materials science issues, and technologically important questions about specific materials systems can be uniquely addressed. Spatial resolution is determined by the beam size at the sample and by a knife-edge technique called differential aperture microscopy that decodes the origin of scattering from along the penetrating x-ray beam. First-generation instrumentation on station 34-ID-E at the Advanced Photon Source (APS) allows for nondestructive automated recovery of the three-dimensional (3D) local crystal phase and orientation. Also recovered are the local elastic-strain and the dislocation tensor distributions. New instrumentation now under development will further extend the applications of polychromatic microdiffraction and will revolutionize materials characterization

  5. Orbiting Carbon Observatory-2 (OCO-2): Science Overview and A-Train Synergy

    Science.gov (United States)

    Crisp, David

    2011-01-01

    NASA's Orbiting Carbon Observatory (OCO) was designed to provide global estimates of atmospheric carbon dioxide (CO2) with the sensitivity, accuracy and sampling density needed to quantify regional scale carbon sources and sinks and characterize their behavior over the annual cycle.

  6. COVE: a visual environment for ocean observatory design

    International Nuclear Information System (INIS)

    Grochow, K; Lazowska, E; Stoermer, M; Kelley, D; Delaney, J

    2008-01-01

    Physical, chemical, and biological ocean processes play a crucial role in determining Earth's environment. Unfortunately, our knowledge of these processes is limited because oceanography is carried out today largely the way it was a century ago: as expeditionary science, going to sea in ships and measuring a relatively small number of parameters (e.g., temperature, salinity, and pressure) as time and budget allow. The NSF Ocean Observatories Initiative is a US$330 million project that will help transform oceanography from a data-poor to a data-rich science. A cornerstone of this project is the deep water Regional Scale Nodes (RSN) that will be installed off the coasts of Washington and Oregon. The RSN will include 1500 km of fiber optic cable providing power and bandwidth to the seafloor and throughout the water column. Thousands of sensors will be deployed to stream data and imagery to shore, where they will be available in real time for ocean scientists and the public at large. The design of the RSN is a complex undertaking, requiring a combination of many different interactive tools and areas of visualization: geographic visualization to see the available seafloor bathymetry, scientific visualization to examine existing geospatially located datasets, layout tools to place the sensors, and collaborative tools to communicate across the team during the design. COVE, the Common Observatory Visualization Environment, is a visualization environment designed to meet all these needs. COVE has been built by computer scientists working closely with the engineering and scientific teams who will build and use the RSN. This paper discusses the data and activities of cabled observatory design, the design of COVE, and results from its use across the team

  7. Using XML and Java Technologies for Astronomical Instrument Control

    Science.gov (United States)

    Ames, Troy; Case, Lynne; Powers, Edward I. (Technical Monitor)

    2001-01-01

    Traditionally, instrument command and control systems have been highly specialized, consisting mostly of custom code that is difficult to develop, maintain, and extend. Such solutions are initially very costly and are inflexible to subsequent engineering change requests, increasing software maintenance costs. Instrument description is too tightly coupled with details of implementation. NASA Goddard Space Flight Center, under the Instrument Remote Control (IRC) project, is developing a general and highly extensible framework that applies to any kind of instrument that can be controlled by a computer. The software architecture combines the platform independent processing capabilities of Java with the power of the Extensible Markup Language (XML), a human readable and machine understandable way to describe structured data. A key aspect of the object-oriented architecture is that the software is driven by an instrument description, written using the Instrument Markup Language (IML), a dialect of XML. IML is used to describe the command sets and command formats of the instrument, communication mechanisms, format of the data coming from the instrument, and characteristics of the graphical user interface to control and monitor the instrument. The IRC framework allows the users to define a data analysis pipeline which converts data coming out of the instrument. The data can be used in visualizations in order for the user to assess the data in real-time, if necessary. The data analysis pipeline algorithms can be supplied by the user in a variety of forms or programming languages. Although the current integration effort is targeted for the High-resolution Airborne Wideband Camera (HAWC) and the Submillimeter and Far Infrared Experiment (SAFIRE), first-light instruments of the Stratospheric Observatory for Infrared Astronomy (SOFIA), the framework is designed to be generic and extensible so that it can be applied to any instrument. Plans are underway to test the framework

  8. The EUV-observatory TESIS on board Coronas-Photon: scientific goals and initial plan of observations

    Science.gov (United States)

    Bogachev, Sergey

    The TESIS a EUV-observatory for solar research from space will be launched in 2008 September on board the satellite Coronas-Photon from cosmodrome Plesetsk. TESIS is a project of Lebedev Physical Institute of Russian Academy of Science with contribution from Space Research Center of Polish Academy of Science (the spectrometer SphinX). The experiment will focus on quasi-monochromatic imaging of the Sun and XUV spectroscopy of solar plasma. The scientific payload of TESIS contains five instruments: (1) Bragg crystal spectroheliometer for Sun monochromatic imaging in the line MgXII 8.42 A, (2) the normal-incidence Herschelian EUV telescopes with a resolution of 1.7 arc sec operated in lines FeXXII 133 A, FeIX 171 A and HeII 304 A, (3) the EUV imaging spectrometer, (4) the wide-field Ritchey-Chretien coronograph and (5) the X-ray spectrometer SphinX. The TESIS will focus on coordinated study of solar activity from the transition region to the outer corona up to 4 solar radii in wide temperature range from 5*104 to 2*107 K. We describe the scientific goals of the TESIS and its initial plan of observations.

  9. The Calibration Target for the Mars 2020 SHERLOC Instrument: Multiple Science Roles for Future Manned and Unmanned Mars Exploration

    Science.gov (United States)

    Fries, M.; Bhartia, R.; Beegle, L.; Burton, A.; Ross, A.; Shahar, A.

    2014-01-01

    The Scanning Habitable Environments with Raman & Luminescence for Organics & Chemicals (SHERLOC) instrument is a deep ultraviolet (UV) Raman/fluorescence instrument selected as part of the Mars 2020 rover instrument suite. SHERLOC will be mounted on the rover arm and its primary role is to identify carbonaceous species in martian samples, which may be selected for inclusion into a returnable sample cache. The SHERLOC instrument will require the use of a calibration target, and by design, multiple science roles will be addressed in the design of the target. Samples of materials used in NASA Extravehicular Mobility unit (EMU, or "space suit") manufacture have been included in the target to serve as both solid polymer calibration targets for SHERLOC instrument function, as well as for testing the resiliency of those materials under martian ambient conditions. A martian meteorite will also be included in the target to serve as a well-characterized example of a martian rock that contains trace carbonaceous material. This rock will be the first rock that we know of that has completed a round trip between planets and will therefore serve an EPO role to attract public attention to science and planetary exploration. The SHERLOC calibration target will address a wide range of NASA goals to include basic science of interest to both the Science Mission Directorate (SMD) and Human Exploration and Operations Mission Directorate (HEOMD).

  10. Construction Status and Early Science with the Daniel K. Inouye Solar Telescope

    Science.gov (United States)

    McMullin, Joseph P.; Rimmele, Thomas R.; Warner, Mark; Martinez Pillet, Valentin; Craig, Simon; Woeger, Friedrich; Tritschler, Alexandra; Berukoff, Steven J.; Casini, Roberto; Goode, Philip R.; Knoelker, Michael; Kuhn, Jeffrey Richard; Lin, Haosheng; Mathioudakis, Mihalis; Reardon, Kevin P.; Rosner, Robert; Schmidt, Wolfgang

    2016-05-01

    The 4-m Daniel K. Inouye Solar Telescope (DKIST) is in its seventh year of overall development and its fourth year of site construction on the summit of Haleakala, Maui. The Site Facilities (Utility Building and Support & Operations Building) are in place with ongoing construction of the Telescope Mount Assembly within. Off-site the fabrication of the component systems is completing with early integration testing and verification starting.Once complete this facility will provide the highest sensitivity and resolution for study of solar magnetism and the drivers of key processes impacting Earth (solar wind, flares, coronal mass ejections, and variability in solar output). The DKIST will be equipped initially with a battery of first light instruments which cover a spectral range from the UV (380 nm) to the near IR (5000 nm), and capable of providing both imaging and spectro-polarimetric measurements throughout the solar atmosphere (photosphere, chromosphere, and corona); these instruments are being developed by the National Solar Observatory (Visible Broadband Imager), High Altitude Observatory (Visible Spectro-Polarimeter), Kiepenheuer Institute (Visible Tunable Filter) and the University of Hawaii (Cryogenic Near-Infrared Spectro-Polarimeter and the Diffraction-Limited Near-Infrared Spectro-Polarimeter). Further, a United Kingdom consortium led by Queen's University Belfast is driving the development of high speed cameras essential for capturing the highly dynamic processes measured by these instruments. Finally, a state-of-the-art adaptive optics system will support diffraction limited imaging capable of resolving features approximately 20 km in scale on the Sun.We present the overall status of the construction phase along with the current challenges as well as a review of the planned science testing and the transition into early science operations.

  11. Gender, culture, and astrophysical fieldwork: Elizabeth Campbell and the Lick Observatory-Crocker eclipse expeditions.

    Science.gov (United States)

    Pang, A. S.-K.

    The article is organized as follows. It begins with an overview of women in nineteenth-century American science. It then describes the culture of mountaintop observatories and life on Mount Hamilton. Elizabeth Campbell's unique role in the Crocker-Lick expeditions drew upon her equally unique role in the observatory, and also on the meaning given to women's work in general on the mountain. The bulk of the article focuses on the Campbells and their expeditions to India in 1898, Spain in 1905, and the South Pacific in 1908. The third section compares the Lick Observatory expeditions to those conducted by David Todd of Amherst College. Todd's wife, Mabel Loomis Todd, went into the field several times with her husband, but her place in the field was radically different from Elizabeth Campbell's, a difference that can be ascribed to a combination of local culture and personality. Finally, it compares American expeditions to British expeditions of the period, to see what the absence of British women on expeditions can tell us about the way national scientific styles and cultures affected gender roles in science.

  12. Preliminary systems engineering evaluations for the National Ecological Observatory Network.

    Energy Technology Data Exchange (ETDEWEB)

    Robertson, Perry J.; Kottenstette, Richard Joseph; Crouch, Shannon M.; Brocato, Robert Wesley; Zak, Bernard Daniel; Osborn, Thor D.; Ivey, Mark D.; Gass, Karl Leslie; Heller, Edwin J.; Dishman, James Larry; Schubert, William Kent; Zirzow, Jeffrey A.

    2008-11-01

    The National Ecological Observatory Network (NEON) is an ambitious National Science Foundation sponsored project intended to accumulate and disseminate ecologically informative sensor data from sites among 20 distinct biomes found within the United States and Puerto Rico over a period of at least 30 years. These data are expected to provide valuable insights into the ecological impacts of climate change, land-use change, and invasive species in these various biomes, and thereby provide a scientific foundation for the decisions of future national, regional, and local policy makers. NEON's objectives are of substantial national and international importance, yet they must be achieved with limited resources. Sandia National Laboratories was therefore contracted to examine four areas of significant systems engineering concern; specifically, alternatives to commercial electrical utility power for remote operations, approaches to data acquisition and local data handling, protocols for secure long-distance data transmission, and processes and procedures for the introduction of new instruments and continuous improvement of the sensor network. The results of these preliminary systems engineering evaluations are presented, with a series of recommendations intended to optimize the efficiency and probability of long-term success for the NEON enterprise.

  13. Distributed Framework for Dynamic Telescope and Instrument Control

    Science.gov (United States)

    Ames, Troy J.; Case, Lynne

    2002-01-01

    Traditionally, instrument command and control systems have been developed specifically for a single instrument. Such solutions are frequently expensive and are inflexible to support the next instrument development effort. NASA Goddard Space Flight Center is developing an extensible framework, known as Instrument Remote Control (IRC) that applies to any kind of instrument that can be controlled by a computer. IRC combines the platform independent processing capabilities of Java with the power of the Extensible Markup Language (XML). A key aspect of the architecture is software that is driven by an instrument description, written using the Instrument Markup Language (IML). IML is an XML dialect used to describe graphical user interfaces to control and monitor the instrument, command sets and command formats, data streams, communication mechanisms, and data processing algorithms. The IRC framework provides the ability to communicate to components anywhere on a network using the JXTA protocol for dynamic discovery of distributed components. JXTA (see httD://www.jxta.org,) is a generalized protocol that allows any devices connected by a network to communicate in a peer-to-peer manner. IRC uses JXTA to advertise a device's IML and discover devices of interest on the network. Devices can join or leave the network and thus join or leave the instrument control environment of IRC. Currently, several astronomical instruments are working with the IRC development team to develop custom components for IRC to control their instruments. These instruments include: High resolution Airborne Wideband Camera (HAWC), a first light instrument for the Stratospheric Observatory for Infrared Astronomy (SOFIA); Submillimeter And Far Infrared Experiment (SAFIRE), a Principal Investigator instrument for SOFIA; and Fabry-Perot Interferometer Bolometer Research Experiment (FIBRE), a prototype of the SAFIRE instrument, used at the Caltech Submillimeter Observatory (CSO). Most recently, we have

  14. An Observatory to Enhance the Preparation of Future California Teachers

    Science.gov (United States)

    Connolly, L.; Lederer, S.

    2004-12-01

    With a major grant from the W. M. Keck Foundation, California State University, San Bernardino is establishing a state-of-the-art teaching astronomical observatory. The Observatory will be fundamental to an innovative undergraduate physics and astronomy curriculum for Physics and Liberal Studies majors and will be integrated into our General Education program. The critical need for a research and educational observatory is linked to changes in California's Science Competencies for teacher certification. Development of the Observatory will also complement a new infusion of NASA funding and equipment support for our growing astronomy education programs and the University's established Strategic Plan for excellence in education and teacher preparation. The Observatory will consist of two domed towers. One tower will house a 20" Ritchey-Chretien telescope equipped with a CCD camera in conjunction with either UBVRI broadband filters or a spectrometer for evening laboratories and student research projects. The second tower will house the university's existing 12" Schmidt-Cassegrain optical telescope coupled with a CCD camera and an array of filters. A small aperture solar telescope will be attached to the 12" for observing solar prominences while a milar filter can be attached to the 12" for sunspot viewing. We have been very fortunate to receive a challenge grant of \\600,000 from the W. M. Keck Foundation to equip the two domed towers; we continue to seek a further \\800,000 to meet our construction needs. Funding also provided by the California State University, San Bernardino.

  15. Code Sharing and Collaboration: Experiences From the Scientist's Expert Assistant Project and Their Relevance to the Virtual Observatory

    Science.gov (United States)

    Korathkar, Anuradha; Grosvenor, Sandy; Jones, Jeremy; Li, Connie; Mackey, Jennifer; Neher, Ken; Obenschain, Arthur F. (Technical Monitor)

    2001-01-01

    In the Virtual Observatory (VO), software tools will perform the functions that have traditionally been performed by physical observatories and their instruments. These tools will not be adjuncts to VO functionality but will make up the very core of the VO. Consequently, the tradition of observatory and system independent tools serving a small user base is not valid for the VO. For the VO to succeed, we must improve software collaboration and code sharing between projects and groups. A significant goal of the Scientist's Expert Assistant (SEA) project has been promoting effective collaboration and code sharing among groups. During the past three years, the SEA project has been developing prototypes for new observation planning software tools and strategies. Initially funded by the Next Generation Space Telescope, parts of the SEA code have since been adopted by the Space Telescope Science Institute. SEA has also supplied code for the SIRTF (Space Infrared Telescope Facility) planning tools, and the JSky Open Source Java library. The potential benefits of sharing code are clear. The recipient gains functionality for considerably less cost. The provider gains additional developers working with their code. If enough users groups adopt a set of common code and tools, de facto standards can emerge (as demonstrated by the success of the FITS standard). Code sharing also raises a number of challenges related to the management of the code. In this talk, we will review our experiences with SEA--both successes and failures, and offer some lessons learned that might promote further successes in collaboration and re-use.

  16. IceCube Gen2. The next-generation neutrino observatory for the South Pole

    Energy Technology Data Exchange (ETDEWEB)

    Santen, Jakob van [DESY, Zeuthen (Germany); Collaboration: IceCube-Collaboration

    2016-07-01

    The IceCube Neutrino Observatory is a cubic-kilometer Cherenkov telescope buried in the ice sheet at the South Pole that detects neutrinos of all flavors with energies from tens of GeV to several PeV. The instrument provided the first measurement of the flux of high-energy astrophysical neutrinos, opening a new window to the TeV universe. At the other end of its sensitivity range, IceCube has provided precision measurements of neutrino oscillation parameters that are competitive with dedicated accelerator-based experiments. Here we present design studies for IceCube Gen2, the next-generation neutrino observatory for the South Pole. Instrumenting a volume of more that 5 km{sup 3} with over 100 new strings, IceCube Gen2 will have substantially greater sensitivity to high-energy neutrinos than current-generation instruments. PINGU, a dense infill array, will lower the energy threshold of the inner detector region to 4 GeV, allowing a determination of the neutrino mass hierarchy. On the surface, a large air shower detector will veto high-energy atmospheric muons and neutrinos from the southern hemisphere, enhancing the reach of astrophysical neutrino searches. With its versatile instrumentation, the IceCube Gen2 facility will allow us to explore the neutrino sky with unprecedented sensitivity, providing new constraints on the sources of the highest-energy cosmic rays, and yield precision data on the mixing and mass ordering of neutrinos.

  17. End-to-end operations at the National Radio Astronomy Observatory

    Science.gov (United States)

    Radziwill, Nicole M.

    2008-07-01

    In 2006 NRAO launched a formal organization, the Office of End to End Operations (OEO), to broaden access to its instruments (VLA/EVLA, VLBA, GBT and ALMA) in the most cost-effective ways possible. The VLA, VLBA and GBT are mature instruments, and the EVLA and ALMA are currently under construction, which presents unique challenges for integrating software across the Observatory. This article 1) provides a survey of the new developments over the past year, and those planned for the next year, 2) describes the business model used to deliver many of these services, and 3) discusses the management models being applied to ensure continuous innovation in operations, while preserving the flexibility and autonomy of telescope software development groups.

  18. The NASA Earth Science Program and Small Satellites

    Science.gov (United States)

    Neeck, Steven P.

    2015-01-01

    Earth's changing environment impacts every aspect of life on our planet and climate change has profound implications on society. Studying Earth as a single complex system is essential to understanding the causes and consequences of climate change and other global environmental concerns. NASA's Earth Science Division (ESD) shapes an interdisciplinary view of Earth, exploring interactions among the atmosphere, oceans, ice sheets, land surface interior, and life itself. This enables scientists to measure global and climate changes and to inform decisions by Government, other organizations, and people in the United States and around the world. The data collected and results generated are accessible to other agencies and organizations to improve the products and services they provide, including air quality indices, disaster prediction and response, agricultural yield projections, and aviation safety. ESD's Flight Program provides the spacebased observing systems and supporting infrastructure for mission operations and scientific data processing and distribution that support NASA's Earth science research and modeling activities. The Flight Program currently has 21 operating Earth observing space missions, including the recently launched Global Precipitation Measurement (GPM) mission, the Orbiting Carbon Observatory-2 (OCO-2), the Soil Moisture Active Passive (SMAP) mission, and the International Space Station (ISS) RapidSCAT and Cloud-Aerosol Transport System (CATS) instruments. The ESD has 22 more missions and instruments planned for launch over the next decade. These include first and second tier missions from the 2007 Earth Science Decadal Survey, Climate Continuity missions to assure availability of key climate data sets, and small-sized competitively selected orbital missions and instrument missions of opportunity belonging to the Earth Venture (EV) Program. Small satellites (500 kg or less) are critical contributors to these current and future satellite missions

  19. European Southern Observatory

    CERN Multimedia

    CERN PhotoLab

    1970-01-01

    Professor A. Blaauw, Director general of the European Southern Observatory, with George Hampton on his right, signs the Agreement covering collaboration with CERN in the construction of the large telescope to be installed at the ESO Observatory in Chile.

  20. New Observatory at the University of Tennessee at Martin

    Science.gov (United States)

    Crews, Lionel J.; Chrysler, R.; Turner, K.

    2010-01-01

    A new observatory has been completed at the University of Tennessee at Martin and is now open for student research, local teacher training, and public outreach. The telescope is a 16" Meade RCT on a Software Bisque Paramount ME mount, 10' HomeDome, and SBIG CCD camera. The project endured many delays from a necessary change in housing from roll-top roof to dome, to the shutter blowing off in a heavy windstorm. This project was funded primarily by a Tennessee Math-Science Partnership grant (PI: Dr. Michael Gibson, UT Martin) directed at secondary teacher training in sciences.

  1. The Evolution of Inquiry Activities in the Akamai Observatory Short Course, 2004-2009

    Science.gov (United States)

    Rice, E. L.; McElwain, M.; Sonnett, S.; Rafelski, M.

    2010-12-01

    The Akamai Observatory Short Course (AOSC) is a five-day course of activities designed to prepare college students majoring in science, technology, engineering, and mathematics (STEM) fields for internships at observatories on the Big Island of Hawai'i. The design and implementation of inquiry-based activities in the AOSC have evolved considerably over the six years of the course. The content goals have always focused on the basic understanding of light and optics necessary to understand telescopes, but the scientific process goals gradually evolved to reflect the increasingly recognized importance of engineering design skills for successful observatory internships. In 2004 the inquiry-based activities were limited to one well-established Color, Light, and Spectra activity. In subsequent years more activities were customized and expanded upon to reflect the learners' diverse academic backgrounds, the developing goals of the short course, and feedback from internship hosts. The most recent inquiry, the Design and Build a Telescope activity, engaged students in designing and building a simple telescope, emphasizing science and engineering process skills in addition to science content. This activity was influenced by the Mission Design activity, added in 2006, that incorporated the application of inquiry-based learning to the engineering design process and allowed students to draw upon their diverse prior knowledge and experience. In this paper we describe the inquiry-based activities in the AOSC in the context of its year-to-year evolution, including the conceptual and pragmatic changes to the short course that influenced the evolution.

  2. US earthquake observatories: recommendations for a new national network

    Energy Technology Data Exchange (ETDEWEB)

    1980-01-01

    This report is the first attempt by the seismological community to rationalize and optimize the distribution of earthquake observatories across the United States. The main aim is to increase significantly our knowledge of earthquakes and the earth's dynamics by providing access to scientifically more valuable data. Other objectives are to provide a more efficient and cost-effective system of recording and distributing earthquake data and to make as uniform as possible the recording of earthquakes in all states. The central recommendation of the Panel is that the guiding concept be established of a rationalized and integrated seismograph system consisting of regional seismograph networks run for crucial regional research and monitoring purposes in tandem with a carefully designed, but sparser, nationwide network of technologically advanced observatories. Such a national system must be thought of not only in terms of instrumentation but equally in terms of data storage, computer processing, and record availability.

  3. The Student Actions Coding Sheet (SACS): An Instrument for Illuminating the Shifts toward Student-Centered Science Classrooms

    Science.gov (United States)

    Erdogan, Ibrahim; Campbell, Todd; Abd-Hamid, Nor Hashidah

    2011-01-01

    This study describes the development of an instrument to investigate the extent to which student-centered actions are occurring in science classrooms. The instrument was developed through the following five stages: (1) student action identification, (2) use of both national and international content experts to establish content validity, (3)…

  4. Progress Report on the US Critical Zone Observatory Program

    Science.gov (United States)

    Barrera, E. C.

    2014-12-01

    The Critical Zone Observatory (CZO) program supported by the National Science Foundation originated from the recommendation of the Earth Science community published in the National Research Council report "Basic Research Opportunities in Earth Sciences" (2001) to establish natural laboratories to study processes and systems of the Critical Zone - the surface and near-surface environment sustaining nearly all terrestrial life. After a number of critical zone community workshops to develop a science plan, the CZO program was initiated in 2007 with three sites and has now grown to 10 sites and a National Office, which coordinates research, education and outreach activities of the network. Several of the CZO sites are collocated with sites supported by the US Long Term Ecological Research (LTER) and the Long Term Agricultural Research (LTAR) programs, and the National Ecological Observatory Network (NEON). Future collaboration with additional sites of these networks will add to the potential to answer questions in a more comprehensive manner and in a larger regional scale about the critical zone form and function. At the international level, CZOs have been established in many countries and strong collaborations with the US program have been in place for many years. The next step is the development of a coordinated international program of critical zone research. The success of the CZO network of sites can be measured in transformative results that elucidate properties and processes controlling the critical zone and how the critical zone structure, stores and fluxes respond to climate and land use change. This understanding of the critical zone can be used to enhance resilience and sustainability, and restore ecosystem function. Thus, CZO science can address major societal challenges. The US CZO network is a facility open to research of the critical zone community at large. Scientific data and information about the US program are available at www.criticalzone.org.

  5. Connecting an Ocean-Bottom Broadband Seismometer to a Seafloor Cabled Observatory: A Prototype System in Monterey Bay

    Science.gov (United States)

    McGill, P.; Neuhauser, D.; Romanowicz, B.

    2008-12-01

    The Monterey Ocean-Bottom Broadband (MOBB) seismic station was installed in April 2003, 40 km offshore from the central coast of California at a seafloor depth of 1000 m. It comprises a three-component broadband seismometer system (Guralp CMG-1T), installed in a hollow PVC caisson and buried under the seafloor; a current meter; and a differential pressure gauge. The station has been operating continuously since installation with no connection to the shore. Three times each year, the station is serviced with the aid of a Remotely Operated Vehicle (ROV) to change the batteries and retrieve the seismic data. In February 2009, the MOBB system will be connected to the Monterey Accelerated Research System (MARS) seafloor cabled observatory. The NSF-funded MARS observatory comprises a 52 km electro-optical cable that extends from a shore facility in Moss Landing out to a seafloor node in Monterey Bay. Once installation is completed in November 2008, the node will provide power and data to as many as eight science experiments through underwater electrical connectors. The MOBB system is located 3 km from the MARS node, and the two will be connected with an extension cable installed by an ROV with the aid of a cable-laying toolsled. The electronics module in the MOBB system is being refurbished to support the connection to the MARS observatory. The low-power autonomous data logger has been replaced with a PC/104 computer stack running embedded Linux. This new computer will run an Object Ring Buffer (ORB), which will collect data from the various MOBB sensors and forward it to another ORB running on a computer at the MARS shore station. There, the data will be archived and then forwarded to a third ORB running at the UC Berkeley Seismological Laboratory. Timing will be synchronized among MOBB's multiple acquisition systems using NTP, GPS clock emulation, and a precise timing signal from the MARS cable. The connection to the MARS observatory will provide real-time access to

  6. Journal of Earth System Science | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    Home; Journals; Journal of Earth System Science. V B Sumithranand. Articles written in Journal of Earth System Science. Volume 119 Issue 4 August 2010 pp 507-517. Variability of soil moisture and its relationship with surface albedo and soil thermal diffusivity at Astronomical Observatory, Thiruvananthapuram, south ...

  7. Project Solaris, a Global Network of Autonomous Observatories: Design, Commissioning, and First Science Results

    Science.gov (United States)

    Kozłowski, S. K.; Sybilski, P. W.; Konacki, M.; Pawłaszek, R. K.; Ratajczak, M.; Hełminiak, K. G.; Litwicki, M.

    2017-10-01

    We present the design and commissioning of Project Solaris, a global network of autonomous observatories. Solaris is a Polish scientific undertaking aimed at the detection and characterization of circumbinary exoplanets and eclipsing binary stars. To accomplish this, a network of four fully autonomous observatories has been deployed in the Southern Hemisphere: Solaris-1 and Solaris-2 in the South African Astronomical Observatory in South Africa; Solaris-3 in Siding Spring Observatory in Australia; and Solaris-4 in Complejo Astronomico El Leoncito in Argentina. The four stations are nearly identical and are equipped with 0.5-m Ritchey-Crétien (f/15) or Cassegrain (f/9, Solaris-3) optics and high-grade 2 K × 2 K CCD cameras with Johnson and Sloan filter sets. We present the design and implementation of low-level security; data logging and notification systems; weather monitoring components; all-sky vision system, surveillance system; and distributed temperature and humidity sensors. We describe dedicated grounding and lighting protection system design and robust fiber data transfer interfaces in electrically demanding conditions. We discuss the outcomes of our design, as well as the resulting software engineering requirements. We describe our system’s engineering approach to achieve the required level of autonomy, the architecture of the custom high-level industry-grade software that has been designed and implemented specifically for the use of the network. We present the actual status of the project and first photometric results; these include data and models of already studied systems for benchmarking purposes (Wasp-4b, Wasp-64b, and Wasp-98b transits, PG 1663-018, an eclipsing binary with a pulsator) as well J024946-3825.6, an interesting low-mass binary system for which a complete model is provided for the first time.

  8. The Ocean Observatories Initiative: Unprecedented access to real-time data streaming from the Cabled Array through OOI Cyberinfrastructure

    Science.gov (United States)

    Knuth, F.; Vardaro, M.; Belabbassi, L.; Smith, M. J.; Garzio, L. M.; Crowley, M. F.; Kerfoot, J.; Kawka, O. E.

    2016-02-01

    The National Science Foundation's Ocean Observatories Initiative (OOI), is a broad-scale, multidisciplinary facility that will transform oceanographic research by providing users with unprecedented access to long-term datasets from a variety of deployed physical, chemical, biological, and geological sensors. The Cabled Array component of the OOI, installed and operated by the University of Washington, is located on the Juan de Fuca tectonic plate off the coast of Oregon. It is a unique network of >100 cabled instruments and instrumented moorings transmitting data to shore in real-time via fiber optic technology. Instruments now installed include HD video and digital still cameras, mass spectrometers, a resistivity-temperature probe inside the orifice of a high-temperature hydrothermal vent, upward-looking ADCP's, pH and pC02 sensors, Horizontal Electrometer Pressure Inverted Echosounders and many others. Here, we present the technical aspects of data streaming from the Cabled Array through the OOI Cyberinfrastructure. We illustrate the types of instruments and data products available, data volume and density, processing levels and algorithms used, data delivery methods, file formats and access methods through the graphical user interface. Our goal is to facilitate the use and access to these unprecedented, co-registered oceanographic datasets. We encourage researchers to collaborate through the use of these simultaneous, interdisciplinary measurements, in the exploration of short-lived events (tectonic, volcanic, biological, severe storms), as well as long-term trends in ocean systems (circulation patterns, climate change, ocean acidity, ecosystem shifts).

  9. Decision Analysis Tools for Volcano Observatories

    Science.gov (United States)

    Hincks, T. H.; Aspinall, W.; Woo, G.

    2005-12-01

    Staff at volcano observatories are predominantly engaged in scientific activities related to volcano monitoring and instrumentation, data acquisition and analysis. Accordingly, the academic education and professional training of observatory staff tend to focus on these scientific functions. From time to time, however, staff may be called upon to provide decision support to government officials responsible for civil protection. Recognizing that Earth scientists may have limited technical familiarity with formal decision analysis methods, specialist software tools that assist decision support in a crisis should be welcome. A review is given of two software tools that have been under development recently. The first is for probabilistic risk assessment of human and economic loss from volcanic eruptions, and is of practical use in short and medium-term risk-informed planning of exclusion zones, post-disaster response, etc. A multiple branch event-tree architecture for the software, together with a formalism for ascribing probabilities to branches, have been developed within the context of the European Community EXPLORIS project. The second software tool utilizes the principles of the Bayesian Belief Network (BBN) for evidence-based assessment of volcanic state and probabilistic threat evaluation. This is of practical application in short-term volcano hazard forecasting and real-time crisis management, including the difficult challenge of deciding when an eruption is over. An open-source BBN library is the software foundation for this tool, which is capable of combining synoptically different strands of observational data from diverse monitoring sources. A conceptual vision is presented of the practical deployment of these decision analysis tools in a future volcano observatory environment. Summary retrospective analyses are given of previous volcanic crises to illustrate the hazard and risk insights gained from use of these tools.

  10. NASA's Earth Science Flight Program overview

    Science.gov (United States)

    Neeck, Steven P.; Volz, Stephen M.

    2011-11-01

    NASA's Earth Science Division (ESD) conducts pioneering work in Earth system science, the interdisciplinary view of Earth that explores the interaction among the atmosphere, oceans, ice sheets, land surface interior, and life itself that has enabled scientists to measure global and climate changes and to inform decisions by governments, organizations, and people in the United States and around the world. The ESD makes the data collected and results generated by its missions accessible to other agencies and organizations to improve the products and services they provide, including air quality indices, disaster management, agricultural yield projections, and aviation safety. In addition to four missions now in development and 14 currently operating on-orbit, the ESD is now developing the first tier of missions recommended by the 2007 Earth Science Decadal Survey and is conducting engineering studies and technology development for the second tier. Furthermore, NASA's ESD is planning implementation of a set of climate continuity missions to assure availability of key data sets needed for climate science and applications. These include a replacement for the Orbiting Carbon Observatory (OCO), OCO-2, planned for launch in 2013; refurbishment of the SAGE III atmospheric chemistry instrument to be hosted by the International Space Station (ISS) as early as 2014; and the Gravity Recovery and Climate Experiment Follow-On (GRACE FO) mission scheduled for launch in 2016. The new Earth Venture (EV) class of missions is a series of uncoupled, low to moderate cost, small to medium-sized, competitively selected, full orbital missions, instruments for orbital missions of opportunity, and sub-orbital projects.

  11. Detection and Implications of Laser-Induced Raman Scattering at Astronomical Observatories

    Directory of Open Access Journals (Sweden)

    Frédéric P. A. Vogt

    2017-06-01

    Full Text Available Laser guide stars employed at astronomical observatories provide artificial wavefront reference sources to help correct (in part the impact of atmospheric turbulence on astrophysical observations. Following the recent commissioning of the 4 Laser Guide Star Facility (4LGSF on Unit Telescope 4 (UT4 of the Very Large Telescope (VLT, we characterize the spectral signature of the uplink beams from the 22-W lasers to assess the impact of laser scattering from the 4LGSF on science observations. We use the Multi-Unit Spectroscopic Explorer (MUSE optical integral field spectrograph mounted on the Nasmyth B focus of UT4 to acquire spectra at a resolution of R≅3000 of the uplink laser beams over the wavelength range of 4750 Å–9350 Å. We report the first detection of laser-induced Raman scattering by N_{2}, O_{2}, CO_{2}, H_{2}O, and (tentatively CH_{4} molecules in the atmosphere above the astronomical observatory of Cerro Paranal. In particular, our observations reveal the characteristic spectral signature of laser photons—but 480 Å to 2210 Å redder than the original laser wavelength of 5889.959 Å—landing on the 8.2-m primary mirror of UT4 after being Raman-scattered on their way up to the sodium layer. Laser-induced Raman scattering, a phenomenon not usually discussed in the astronomical context, is not unique to the observatory of Cerro Paranal, but it is common to any astronomical telescope employing a laser guide star (LGS system. It is thus essential for any optical spectrograph coupled to a LGS system to thoroughly handle the possibility of a Raman spectral contamination via a proper baffling of the instrument and suitable calibrations procedures. These considerations are particularly applicable for the HARMONI optical spectrograph on the upcoming Extremely Large Telescope (ELT. At sites hosting multiple telescopes, laser-collision-prediction tools should also account for the presence of Raman emission from the uplink laser beam

  12. The Virtual Solar Observatory and the Heliophysics Meta-Virtual Observatory

    Science.gov (United States)

    Gurman, Joseph B.

    2007-01-01

    The Virtual Solar Observatory (VSO) is now able to search for solar data ranging from the radio to gamma rays, obtained from space and groundbased observatories, from 26 sources at 12 data providers, and from 1915 to the present. The solar physics community can use a Web interface or an Application Programming Interface (API) that allows integrating VSO searches into other software, including other Web services. Over the next few years, this integration will be especially obvious as the NASA Heliophysics division sponsors the development of a heliophysics-wide virtual observatory (VO), based on existing VO's in heliospheric, magnetospheric, and ionospheric physics as well as the VSO. We examine some of the challenges and potential of such a "meta-VO."

  13. Academic Research Equipment in the Physical and Computer Sciences and Engineering. An Analysis of Findings from Phase I of the National Science Foundation's National Survey of Academic Research Instruments and Instrumentation Needs.

    Science.gov (United States)

    Burgdorf, Kenneth; White, Kristine

    This report presents information from phase I of a survey designed to develop quantitative indicators of the current national stock, cost/investment, condition, obsolescence, utilization, and need for major research instruments in academic settings. Data for phase I (which focused on the physical and computer sciences and engineering) were…

  14. The French Jesuit Mission to Thailand in the 1680s and the Establishment of a Major Astronomical Observatory

    Science.gov (United States)

    Soonthornthum, Boonrucksar; Orchiston, Wayne; Komonjinda, Siramas

    2012-09-01

    The first great Thai ruler to encourage the adoption of Western culture and technology was King Narai, and his enlightened attitude led to the rapid development of Thailand. King Narai also had a passion for astronomy, and he pursued this interest by allowing French Jesuit missionaries to set up a large modern well-equipped astronomical observatory in Lopburi Province between AD 1685 and 1687. This was known as the Wat San Paolo Observatory, and King Narai and the missionaries observed a total lunar eclipse on 10 December 1685 and a partial solar eclipse on 30 April 1688. These observations and others made at Wat San Paolo Observatory during the 1680s marked the start of modern scientific astronomy in Thailand. In this paper we discuss King Narai's scientific and other interests, the founding of the Wat San Paolo Observatory, the missionaries who conducted the astronomical programs, their instruments and their observations. We also describe the surviving ruins of the Observatory and their interpretation as a site of national scientific importance in Thailand.

  15. Thermal Testing and Model Correlation of the Magnetospheric Multiscale (MMS) Observatories

    Science.gov (United States)

    Kim, Jong S.; Teti, Nicholas M.

    2015-01-01

    The Magnetospheric Multiscale (MMS) mission is a Solar Terrestrial Probes mission comprising four identically instrumented spacecraft that will use Earth's magnetosphere as a laboratory to study the microphysics of three fundamental plasma processes: magnetic reconnection, energetic particle acceleration, and turbulence. This paper presents the complete thermal balance (TB) test performed on the first of four observatories to go through thermal vacuum (TV) and the minibalance testing that was performed on the subsequent observatories to provide a comparison of all four. The TV and TB tests were conducted in a thermal vacuum chamber at the Naval Research Laboratory (NRL) in Washington, D.C. with the vacuum level higher than 1.3 x 10 (sup -4) pascals (10 (sup -6) torr) and the surrounding temperature achieving -180 degrees Centigrade. Three TB test cases were performed that included hot operational science, cold operational science and a cold survival case. In addition to the three balance cases a two hour eclipse and a four hour eclipse simulation was performed during the TV test to provide additional transient data points that represent the orbit in eclipse (or Earth's shadow) The goal was to perform testing such that the flight orbital environments could be simulated as closely as possible. A thermal model correlation between the thermal analysis and the test results was completed. Over 400 1-Wire temperature sensors, 200 thermocouples and 125 flight thermistor temperature sensors recorded data during TV and TB testing. These temperature versus time profiles and their agreements with the analytical results obtained using Thermal Desktop and SINDA/FLUINT are discussed. The model correlation for the thermal mathematical model (TMM) is conducted based on the numerical analysis results and the test data. The philosophy of model correlation was to correlate the model to within 3 degrees Centigrade of the test data using the standard deviation and mean deviation error

  16. National Astronomical Observatory of Japan

    CERN Document Server

    Haubold, Hans J; UN/ESA/NASA Workshop on the International Heliophysical Year 2007 and Basic Space Science, hosted by the National Astronomical Observatory of Japan

    2010-01-01

    This book represents Volume II of the Proceedings of the UN/ESA/NASA Workshop on the International Heliophysical Year 2007 and Basic Space Science, hosted by the National Astronomical Observatory of Japan, Tokyo, 18 - 22 June, 2007. It covers two programme topics explored in this and past workshops of this nature: (i) non-extensive statistical mechanics as applicable to astrophysics, addressing q-distribution, fractional reaction and diffusion, and the reaction coefficient, as well as the Mittag-Leffler function and (ii) the TRIPOD concept, developed for astronomical telescope facilities. The companion publication, Volume I of the proceedings of this workshop, is a special issue in the journal Earth, Moon, and Planets, Volume 104, Numbers 1-4, April 2009.

  17. Preliminary Analysis of Assessment Instrument Design to Reveal Science Generic Skill and Chemistry Literacy

    Science.gov (United States)

    Sumarni, Woro; Sudarmin; Supartono, Wiyanto

    2016-01-01

    The purpose of this research is to design assessment instrument to evaluate science generic skill (SGS) achievement and chemistry literacy in ethnoscience-integrated chemistry learning. The steps of tool designing refers to Plomp models including 1) Investigation Phase (Prelimenary Investigation); 2) Designing Phase (Design); 3)…

  18. MLRS - A lunar/artificial satellite laser ranging facility at the McDonald Observatory

    Science.gov (United States)

    Shelus, P. J.

    1985-01-01

    Experience from lunar and satellite laser ranging experiments carried out at McDonald Observatory has been used to design the McDonald Laser Ranging Station (MLRS). The MLRS is a dual-purpose installation designed to obtain observations from the LAGEOS satellite and lunar targets. The instruments used at the station include a telescope assembly 0.76 meters in diameter; a Q-switched doubled neodymium YAG laser with a pulse rate of three nanoseconds; and a GaAs photodetector with Fabry-Perot interferometric filter. A functional diagram of the system is provided. The operating parameters of the instruments are summarized in a table.

  19. Virtual Observatory: From Concept to Implementation

    Science.gov (United States)

    Djorgovski, S. G.; Williams, R.

    2005-12-01

    We review the origins of the Virtual Observatory (VO) concept, and the current status of the efforts in this field. VO is the response of the astronomical community to the challenges posed by the modern massive and complex data sets. It is a framework in which information technology is harnessed to organize, maintain, and explore the rich information content of the exponentially growing data sets, and to enable a qualitatively new science to be done with them. VO will become a complete, open, distributed, web-based framework for astronomy of the early 21st century. A number of significant efforts worldwide are now striving to convert this vision into reality. The technological and methodological challenges posed by the information-rich astronomy are also common to many other fields. We see a fundamental change in the way all science is done, driven by the information technology revolution.

  20. James Webb Space Telescope Core 2 Test - Cryogenic Thermal Balance Test of the Observatorys Core Area Thermal Control Hardware

    Science.gov (United States)

    Cleveland, Paul; Parrish, Keith; Thomson, Shaun; Marsh, James; Comber, Brian

    2016-01-01

    The James Webb Space Telescope (JWST), successor to the Hubble Space Telescope, will be the largest astronomical telescope ever sent into space. To observe the very first light of the early universe, JWST requires a large deployed 6.5-meter primary mirror cryogenically cooled to less than 50 Kelvin. Three scientific instruments are further cooled via a large radiator system to less than 40 Kelvin. A fourth scientific instrument is cooled to less than 7 Kelvin using a combination pulse-tube Joule-Thomson mechanical cooler. Passive cryogenic cooling enables the large scale of the telescope which must be highly folded for launch on an Ariane 5 launch vehicle and deployed once on orbit during its journey to the second Earth-Sun Lagrange point. Passive cooling of the observatory is enabled by the deployment of a large tennis court sized five layer Sunshield combined with the use of a network of high efficiency radiators. A high purity aluminum heat strap system connects the three instrument's detector systems to the radiator systems to dissipate less than a single watt of parasitic and instrument dissipated heat. JWST's large scale features, while enabling passive cooling, also prevent the typical flight configuration fully-deployed thermal balance test that is the keystone of most space missions' thermal verification plans. This paper describes the JWST Core 2 Test, which is a cryogenic thermal balance test of a full size, high fidelity engineering model of the Observatory's 'Core' area thermal control hardware. The 'Core' area is the key mechanical and cryogenic interface area between all Observatory elements. The 'Core' area thermal control hardware allows for temperature transition of 300K to approximately 50 K by attenuating heat from the room temperature IEC (instrument electronics) and the Spacecraft Bus. Since the flight hardware is not available for test, the Core 2 test uses high fidelity and flight-like reproductions.

  1. A pilot Virtual Observatory (pVO) for integrated catchment science - Demonstration of national scale modelling of hydrology and biogeochemistry (Invited)

    Science.gov (United States)

    Freer, J. E.; Bloomfield, J. P.; Johnes, P. J.; MacLeod, C.; Reaney, S.

    2010-12-01

    There are many challenges in developing effective and integrated catchment management solutions for hydrology and water quality issues. Such solutions should ideally build on current scientific evidence to inform policy makers and regulators and additionally allow stakeholders to take ownership of local and/or national issues, in effect bringing together ‘communities of practice’. A strategy being piloted in the UK as the Pilot Virtual Observatory (pVO), funded by NERC, is to demonstrate the use of cyber-infrastructure and cloud computing resources to investigate better methods of linking data and models and to demonstrate scenario analysis for research, policy and operational needs. The research will provide new ways the scientific and stakeholder communities come together to exploit current environmental information, knowledge and experience in an open framework. This poster presents the project scope and methodologies for the pVO work dealing with national modelling of hydrology and macro-nutrient biogeochemistry. We evaluate the strategies needed to robustly benchmark our current predictive capability of these resources through ensemble modelling. We explore the use of catchment similarity concepts to understand if national monitoring programs can inform us about the behaviour of catchments. We discuss the challenges to applying these strategies in an open access and integrated framework and finally we consider the future for such virtual observatory platforms for improving the way we iteratively improve our understanding of catchment science.

  2. Reusing Joint Polar Satellite System (jpss) Ground System Components to Process AURA Ozone Monitoring Instrument (omi) Science Products

    Science.gov (United States)

    Moses, J. F.; Jain, P.; Johnson, J.; Doiron, J. A.

    2017-12-01

    New Earth observation instruments are planned to enable advancements in Earth science research over the next decade. Diversity of Earth observing instruments and their observing platforms will continue to increase as new instrument technologies emerge and are deployed as part of National programs such as Joint Polar Satellite System (JPSS), Geostationary Operational Environmental Satellite system (GOES), Landsat as well as the potential for many CubeSat and aircraft missions. The practical use and value of these observational data often extends well beyond their original purpose. The practicing community needs intuitive and standardized tools to enable quick unfettered development of tailored products for specific applications and decision support systems. However, the associated data processing system can take years to develop and requires inherent knowledge and the ability to integrate increasingly diverse data types from multiple sources. This paper describes the adaptation of a large-scale data processing system built for supporting JPSS algorithm calibration and validation (Cal/Val) node to a simplified science data system for rapid application. The new configurable data system reuses scalable JAVA technologies built for the JPSS Government Resource for Algorithm Verification, Independent Test, and Evaluation (GRAVITE) system to run within a laptop environment and support product generation and data processing of AURA Ozone Monitoring Instrument (OMI) science products. Of particular interest are the root requirements necessary for integrating experimental algorithms and Hierarchical Data Format (HDF) data access libraries into a science data production system. This study demonstrates the ability to reuse existing Ground System technologies to support future missions with minimal changes.

  3. Remote Observing: Equipment, Methods and Experiences at the Dark Sky Observatory

    Science.gov (United States)

    Caton, Daniel B.; Hawkins, L.

    2009-01-01

    Over the last few years we have experimented with remote observing with the 32-inch telescope at our Dark Sky Observatory. We have used relatively inexpensive X10 control modules and software to control many electrical and electronic circuits and devices. User access is via a combination of Microsoft Remote Desktop and RealVNC. X10's ActiveHome Pro software provides the interface for device control. Data acquisition has been with a Photometrics CH250 CCD camera under control of PMIS. Our new imaging camera is an Apogee U42 controlled by MaximDL. In both cases the control over the Internet is by the RD/VNC interface. All of this goes through an ordinary DSL connection at the observatory and provides surprisingly good performance even with the user having only DSL access at home as well. Field acquisition for cases of telescope misalignment with the sky after an instrument changeover are provided by an ImagingSource DMK 41AU02-USB camera on a Vixen 80mm f/5 auxiliary telescope. In some cases, to prevent crashing PMIS due to buffer overrun/interrupt issues, the field alignment is monitored using a streaming Linksys webcam that looks at the data-acquisition PC's monitor. Autoguiding uses an SBIG ST-402 camera and either CCDOPS or MaximDL. While we have only done imaging via remote use, we are working to develop control of the spectrograph as well. Weather conditions are monitored with a combination of a Davis Vantage Pro weather station, a Boltwood cloud/precipitation detector, daytime webcams and an infrared-sensitive SBIG Meteor camera for night views of the sky. We are grateful for support for this work from National Science Foundation grants AST-0520812 and AST-0722491.

  4. STEREO-IMPACT Education and Public Outreach: Sharing STEREO Science

    Science.gov (United States)

    Craig, N.; Peticolas, L. M.; Mendez, B. J.

    2005-12-01

    The Solar TErrestrial RElations Observatory (STEREO) is scheduled for launch in Spring 2006. STEREO will study the Sun with two spacecrafts in orbit around it and on either side of Earth. The primary science goal is to understand the nature and consequences of Coronal Mass Ejections (CMEs). Despite their importance, scientists don't fully understand the origin and evolution of CMEs, nor their structure or extent in interplanetary space. STEREO's unique 3-D images of the structure of CMEs will enable scientists to determine their fundamental nature and origin. We will discuss the Education and Public Outreach (E/PO) program for the In-situ Measurement of Particles And CME Transients (IMPACT) suite of instruments aboard the two crafts and give examples of upcoming activities, including NASA's Sun-Earth day events, which are scheduled to coincide with a total solar eclipse in March. This event offers a good opportunity to engage the public in STEREO science, because an eclipse allows one to see the solar corona from where CMEs erupt. STEREO's connection to space weather lends itself to close partnerships with the Sun-Earth Connection Education Forum (SECEF), The Exploratorium, and UC Berkeley's Center for New Music and Audio Technologies to develop informal science programs for science centers, museum visitors, and the public in general. We will also discuss our teacher workshops locally in California and also at annual conferences such as those of the National Science Teachers Association. Such workshops often focus on magnetism and its connection to CMEs and Earth's magnetic field, leading to the questions STEREO scientists hope to answer. The importance of partnerships and coordination in working in an instrument E/PO program that is part of a bigger NASA mission with many instrument suites and many PIs will be emphasized. The Education and Outreach Porgram is funded by NASA's SMD.

  5. Footprint Database and web services for the Herschel space observatory

    Science.gov (United States)

    Verebélyi, Erika; Dobos, László; Kiss, Csaba

    2015-08-01

    Using all telemetry and observational meta-data, we created a searchable database of Herschel observation footprints. Data from the Herschel space observatory is freely available for everyone but no uniformly processed catalog of all observations has been published yet. As a first step, we unified the data model for all three Herschel instruments in all observation modes and compiled a database of sky coverage information. As opposed to methods using a pixellation of the sphere, in our database, sky coverage is stored in exact geometric form allowing for precise area calculations. Indexing of the footprints allows for very fast search among observations based on pointing, time, sky coverage overlap and meta-data. This enables us, for example, to find moving objects easily in Herschel fields. The database is accessible via a web site and also as a set of REST web service functions which makes it usable from program clients like Python or IDL scripts. Data is available in various formats including Virtual Observatory standards.

  6. Materials and Life Science Experimental Facility (MLF at the Japan Proton Accelerator Research Complex II: Neutron Scattering Instruments

    Directory of Open Access Journals (Sweden)

    Kenji Nakajima

    2017-11-01

    Full Text Available The neutron instruments suite, installed at the spallation neutron source of the Materials and Life Science Experimental Facility (MLF at the Japan Proton Accelerator Research Complex (J-PARC, is reviewed. MLF has 23 neutron beam ports and 21 instruments are in operation for user programs or are under commissioning. A unique and challenging instrumental suite in MLF has been realized via combination of a high-performance neutron source, optimized for neutron scattering, and unique instruments using cutting-edge technologies. All instruments are/will serve in world-leading investigations in a broad range of fields, from fundamental physics to industrial applications. In this review, overviews, characteristic features, and typical applications of the individual instruments are mentioned.

  7. Global TIE Observatories: Real Time Observational Astronomy Through a Robotic Telescope Network

    Science.gov (United States)

    Clark, G.; Mayo, L. A.

    2001-12-01

    Astronomy in grades K-12 is traditionally taught (if at all) using textbooks and a few simple hands-on activities. Teachers are generally not trained in observational astronomy techniques and are unfamiliar with the most basic astronomical concepts. In addition, most students, by High School graduation, will never have even looked through the eyepiece of a telescope. The problem becomes even more challenging in inner cities, remote rural areas and low socioeconomic communities where educational emphasis on topics in astronomy as well as access to observing facilities is limited or non existent. Access to most optical telescope facilities is limited to monthly observing nights that cater to a small percentage of the general public living near the observatory. Even here, the observing experience is a one-time event detached from the process of scientific enquiry and sustained educational application. Additionally, a number of large, "research grade" observatory facilities are largely unused, partially due to the slow creep of light pollution around the facilities as well as the development of newer, more capable telescopes. Though cutting edge science is often no longer possible at these sights, real research opportunities in astronomy remain numerous for these facilities as educational tools. The possibility now exists to establish a network of research grade telescopes, no longer useful to the professional astronomical community, that can be made accessible through classrooms, after school, and community based programs all across the country through existing IT technologies and applications. These telescopes could provide unparalleled research and educational opportunities for a broad spectrum of students and turns underutilized observatory facilities into valuable, state-of-the-art teaching centers. The NASA sponsored Telescopes In Education project has been wildly successful in engaging the K-12 education community in real-time, hands-on, interactive astronomy

  8. The scientific use of technological instruments

    NARCIS (Netherlands)

    Boon, Mieke; Hansson, Sven Ove

    2015-01-01

    One of the most obvious ways in which the natural sciences depend on technology is through the use of instruments. This chapter presents a philosophical analysis of the role of technological instruments in science. Two roles of technological instruments in scientific practices are distinguished:

  9. Archives at the U.S. Naval Observatory - Recent Projects

    Science.gov (United States)

    Corbin, B. G.

    2004-12-01

    In 1874, like many other astronomical institutions, the U.S. Naval Observatory sent eight expeditions to different parts of the globe to observe the Transit of Venus. After all results were in, William Harkness was placed in charge of preparing the results and observations for publication. Page proofs of these observations appeared in 1881, but due to lack of funds and other reasons, these volumes were never published. Recently funds became available to have photocopies made on acid-free paper. The Astrophysics Data System (ADS) agreed to scan the photocopied pages and has made this publication available via the ADS so it now may be seen by anyone with access to the web. The compilation of a historical photograph archive at the USNO is continuing. Photographs and glass plates are being scanned by students and placed on the web. As the Naval Observatory has many thousands of plates and photographs, this project will take quite some time to complete. The images are of instruments, buildings, and staff members. The URL for this collection is http://www.usno.navy.mil/library/search.shtml

  10. Computer Vision for the Solar Dynamics Observatory (SDO)

    Science.gov (United States)

    Martens, P. C. H.; Attrill, G. D. R.; Davey, A. R.; Engell, A.; Farid, S.; Grigis, P. C.; Kasper, J.; Korreck, K.; Saar, S. H.; Savcheva, A.; Su, Y.; Testa, P.; Wills-Davey, M.; Bernasconi, P. N.; Raouafi, N.-E.; Delouille, V. A.; Hochedez, J. F.; Cirtain, J. W.; Deforest, C. E.; Angryk, R. A.; de Moortel, I.; Wiegelmann, T.; Georgoulis, M. K.; McAteer, R. T. J.; Timmons, R. P.

    2012-01-01

    In Fall 2008 NASA selected a large international consortium to produce a comprehensive automated feature-recognition system for the Solar Dynamics Observatory (SDO). The SDO data that we consider are all of the Atmospheric Imaging Assembly (AIA) images plus surface magnetic-field images from the Helioseismic and Magnetic Imager (HMI). We produce robust, very efficient, professionally coded software modules that can keep up with the SDO data stream and detect, trace, and analyze numerous phenomena, including flares, sigmoids, filaments, coronal dimmings, polarity inversion lines, sunspots, X-ray bright points, active regions, coronal holes, EIT waves, coronal mass ejections (CMEs), coronal oscillations, and jets. We also track the emergence and evolution of magnetic elements down to the smallest detectable features and will provide at least four full-disk, nonlinear, force-free magnetic field extrapolations per day. The detection of CMEs and filaments is accomplished with Solar and Heliospheric Observatory (SOHO)/ Large Angle and Spectrometric Coronagraph (LASCO) and ground-based Hα data, respectively. A completely new software element is a trainable feature-detection module based on a generalized image-classification algorithm. Such a trainable module can be used to find features that have not yet been discovered (as, for example, sigmoids were in the pre- Yohkoh era). Our codes will produce entries in the Heliophysics Events Knowledgebase (HEK) as well as produce complete catalogs for results that are too numerous for inclusion in the HEK, such as the X-ray bright-point metadata. This will permit users to locate data on individual events as well as carry out statistical studies on large numbers of events, using the interface provided by the Virtual Solar Observatory. The operations concept for our computer vision system is that the data will be analyzed in near real time as soon as they arrive at the SDO Joint Science Operations Center and have undergone basic

  11. INSTRUMENTS OF SUPPORT FOR RESEARCH AND DEVELOPMENT FUNDED BY LEADING DOMESTIC AND INTERNATIONAL SCIENCE FOUNDATIONS

    Directory of Open Access Journals (Sweden)

    Irina E. Ilina

    2017-06-01

    Full Text Available Introduction: one of the key aspects of the knowledge economy development is the growing significance of the results of research and development. The education and basic research play a key role in this process. Funding for education and fundamental science is carried out mainly at the expense of the state resources, including a system of foundations for scientific, engineering and innovation activities in Russia. The purpose of this article is to present recommendations for improving the tools of domestic foundations in funding fundamental research and development, including education and training. The propositions are made with a comparative analysis of the domestic and foreign science foun dations’ activities. Materials and Methods: the authors used analysis, comparison, induction, deduction, graphical analysis, generalisation and other scientific methods during the study. Results: the lack of comparability between domestic and foreign scientific funds in the volume of funding allocated for basic research and development is revealed. This situation affects the scientific research. The foreign foundations have a wide range of instruments to support research projects at all stages of the life cycle of grants for education and training prior to release of an innovative product to market (the use of “innovation elevator” system. The Russian national scientific foundations have no such possibilities. The authors guess that the Russian organisations ignore some of the instruments for supporting research and development. Use of these tools could enhance the effectiveness of research projects. According to the study of domestic and foreign experience in supporting research and development, the authors proposed a matrix composed of instruments for support in the fields of basic scientific researches and education with such phases of the project life cycle as “research” and “development”. Discussion and Conclusions: the foreign science

  12. Solar activity monitoring and forecasting capabilities at Big Bear Solar Observatory

    Directory of Open Access Journals (Sweden)

    P. T. Gallagher

    2002-07-01

    Full Text Available The availability of full-disk, high-resolution Ha images from Big Bear Solar Observatory (USA, Kanzelhöhe Solar Observatory (Austria, and Yunnan Astronomical Observatory (China allows for the continual monitoring of solar activity with unprecedented spatial and temporal resolution. Typically, this Global Ha Network (GHN provides almost uninterrupted Ha images with a cadence of 1 min and an image scale of 1'' per pixel.  Every hour, GHN images are transferred to the web-based BBSO Active Region Monitor (ARM; www.bbso.njit.edu/arm, which includes the most recent EUV, continuum, and magnetogram data from the Solar and Heliospheric Observatory, together with magnetograms from the Global Oscillation Network Group. ARM also includes a variety of active region properties from the National Oceanic and Atmospheric Administration’s Space Environment Center, such as up-to-date active region positions, GOES 5-min X-ray data, and flare identification. Stokes I, V, Q, and U images are available from the recently operational BBSO Digital Vector Magnetograph and the Vector Magnetograph at the Huairou Solar Observing Station of Beijing Observatory. Vector magnetograms provide complete information on the photospheric magnetic field, and allow for magnetic flux gradients, electric currents, and shear forces to be calculated: these measurements are extremely sensitive to conditions resulting in flaring activity. Furthermore, we have developed a Flare Prediction System which estimates the probability for each region to produce C-, M-, or X-class flares based on nearly eight years of NOAA data from cycle 22. This, in addition to BBSO’s daily solar activity reports, has proven a useful resource for activity forecasting.Key words. Solar physics, astronomy and astrophysics (flares and mass ejections; instruments and techniques; photosphere and chromosphere

  13. Experimental innovations in surface science a guide to practical laboratory methods and instruments

    CERN Document Server

    Yates, John T

    2015-01-01

    This book is a new edition of a classic text on experimental methods and instruments in surface science. It offers practical insight useful to chemists, physicists, and materials scientists working in experimental surface science. This enlarged second edition contains almost 300 descriptions of experimental methods. The more than 50 active areas with individual scientific and measurement concepts and activities relevant to each area are presented in this book. The key areas covered are: Vacuum System Technology, Mechanical Fabrication Techniques, Measurement Methods, Thermal Control, Delivery of Adsorbates to Surfaces, UHV Windows, Surface Preparation Methods, High Area Solids, Safety. The book is written for researchers and graduate students.

  14. PoSSUM: Polar Suborbital Science in the Upper Mesosphere

    Science.gov (United States)

    Reimuller, J. D.; Fritts, D. C.; Thomas, G. E.; Taylor, M. J.; Mitchell, S.; Lehmacher, G. A.; Watchorn, S. R.; Baumgarten, G.; Plane, J. M.

    2013-12-01

    Project PoSSUM (www.projectpossum.org) is a suborbital research project leveraging imaging and remote sensing techniques from Reusable Suborbital Launch Vehicles (rSLVs) to gather critical climate data through use of the PoSSUM Observatory and the PoSSUM Aeronomy Laboratory. An acronym for Polar Suborbital Science in the Upper Mesosphere, PoSSUM grew from the opportunity created by the Noctilucent Cloud Imagery and Tomography Experiment, selected by the NASA Flight Opportunities Program as Experiment 46-S in March 2012. This experiment will employ an rSLV (e.g. the XCOR Lynx Mark II) launched from a high-latitude spaceport (e.g. Eielson AFB, Alaska or Kiruna, Sweden) during a week-long deployment scheduled for July 2015 to address critical questions concerning noctilucent clouds (NLCs) through flights that transition the cloud layer where the clouds will be under direct illumination from the sun. The 2015 Project PoSSUM NLC campaign will use the unique capability of rSLVs to address key under-answered questions pertaining to NLCs. Specifically, PoSSUM will answer: 1) What are the small-scale dynamics of NLCs and what does this tell us about the energy and momentum deposition from the lower atmosphere? 2) What is the seasonal variability of NLCs, mesospheric dynamics, and temperatures? 3) Are structures observed in the OH layer coupled with NLC structures? 4) How do NLCs nucleate? and 5) What is the geometry of NLC particles and how do they stratify? Instrumentation will include video and still-frame visible cameras (PoSSUMCam), infrared cameras, a mesospheric temperatures experiment, a depolarization LiDAR, a mesospheric density and temperatures experiment (MCAT), a mesospheric winds experiment, and a meteoric smoke detector (MASS). The instrument suite used on PoSSUM will mature through subsequent campaigns to develop an integrated, modular laboratory (the ';PoSSUM Observatory') that will provide repeatable, low cost, in-situ NLC and aeronomy observations as well

  15. The National Astronomical Observatory of Japan and Post-war Japanese Optical Astronomy

    Science.gov (United States)

    Tajima, Toshiyuki

    This paper depicts some aspects of the formative process of the Japanese optical and infrared astronomical community in the post-war period, featuring the transition of the National Astronomical Observatory of Japan(NAOJ). We take up three cases of telescope construction, examining their background and their contribution to the Japanese astronomical community. Through these cases, the characteristics of traditions and cultures of optical and infrared astronomy in Japan are considered. Although the Tokyo Astronomical Observatory (TAO) of the University of Tokyo, the predecessor of NAOJ, was originally founded as an agency for practical astronomical observation such as time and almanac service, it has become an international centre for all types of astrophysical research. Research and development of telescopes and observational instruments have become an important part of the astronomers' practice. Now, however, a number of Japanese universities are planning to have their own large to middle-sized telescopes, and a new style of astronomical research is emerging involving astrophysical studies utilising data acquired from the Virtual Observatory, so there is a distinct possibility that the status of the NAOJ will change even further in the future.

  16. The Contributions of the WIYN Observatory to Undergraduate Education

    Science.gov (United States)

    Hooper, Eric; Consortium, WIYN

    2014-01-01

    Over its nearly 20 year history the WIYN Observatory has provided crucial data for numerous undergraduate research projects at the partner institutions (University of Wisconsin-Madison, Indiana University, and Yale University) plus others who access the telescope via national time from NOAO. WIYN and its instruments have served both undergraduates who are local to each institution, as well as those who have a temporary tenure as Research Experience for Undergraduates (REU) students. The topics of this work range widely, and only a few examples are listed here. Numerous studies of stars have been undertaken by undergraduates, from rotation velocities of pre-main sequence stars (Rhode et al.) to dynamical heating mechanisms in open clusters (Friel et al.). Extragalactic investigations range from a study of cold ISM in galaxies near the centers of rich clusters (Gallagher & Hooper, et al.) to the stellar populations of post-starburst galaxies hosting low-level AGN (Wolf & Hooper, et al.). Students have made wide use of WIYN's long established suite of facility instruments, which currently includes the Hydra multi-object fiber spectrograph, the SparsePak integral field unit fiber spectrograph, and the WHIRC near-infrared imager. A current undergraduate is a key player in final laboratory testing of two new integral field units that will come to WIYN soon. Finally, the new large format imager pODI currently is in science operation, soon to be followed by an upgrade to nearly four times the current imaging area, a powerful tool that will join the others in contributing to undergraduate research and education. This presentation is a continuation of the overview of WIYN contributions to education that began with a discussion of graduate education at the Indianapolis AAS (Hooper, AAS Meeting #222, #214.23).

  17. Global Precipitation Measurement (GPM) Core Observatory Falling Snow Estimates

    Science.gov (United States)

    Skofronick Jackson, G.; Kulie, M.; Milani, L.; Munchak, S. J.; Wood, N.; Levizzani, V.

    2017-12-01

    Retrievals of falling snow from space represent an important data set for understanding and linking the Earth's atmospheric, hydrological, and energy cycles. Estimates of falling snow must be captured to obtain the true global precipitation water cycle, snowfall accumulations are required for hydrological studies, and without knowledge of the frozen particles in clouds one cannot adequately understand the energy and radiation budgets. This work focuses on comparing the first stable falling snow retrieval products (released May 2017) for the Global Precipitation Measurement (GPM) Core Observatory (GPM-CO), which was launched February 2014, and carries both an active dual frequency (Ku- and Ka-band) precipitation radar (DPR) and a passive microwave radiometer (GPM Microwave Imager-GMI). Five separate GPM-CO falling snow retrieval algorithm products are analyzed including those from DPR Matched (Ka+Ku) Scan, DPR Normal Scan (Ku), DPR High Sensitivity Scan (Ka), combined DPR+GMI, and GMI. While satellite-based remote sensing provides global coverage of falling snow events, the science is relatively new, the different on-orbit instruments don't capture all snow rates equally, and retrieval algorithms differ. Thus a detailed comparison among the GPM-CO products elucidates advantages and disadvantages of the retrievals. GPM and CloudSat global snowfall evaluation exercises are natural investigative pathways to explore, but caution must be undertaken when analyzing these datasets for comparative purposes. This work includes outlining the challenges associated with comparing GPM-CO to CloudSat satellite snow estimates due to the different sampling, algorithms, and instrument capabilities. We will highlight some factors and assumptions that can be altered or statistically normalized and applied in an effort to make comparisons between GPM and CloudSat global satellite falling snow products as equitable as possible.

  18. Automating OSIRIS Data Reduction for the Keck Observatory Archive

    Science.gov (United States)

    Holt, J.; Tran, H. D.; Goodrich, R.; Berriman, G. B.; Gelino, C. R.; KOA Team

    2014-05-01

    By the end of 2013, the Keck Observatory Archive (KOA) will serve data from all active instruments on the Keck Telescopes. OSIRIS (OH-Suppressing Infra-Red Imaging Spectrograph), the last active instrument to be archived in KOA, has been in use behind the (AO) system at Keck since February 2005. It uses an array of tiny lenslets to simultaneously produce spectra at up to 4096 locations. Due to the complicated nature of the OSIRIS raw data, the OSIRIS team developed a comprehensive data reduction program. This data reduction system has an online mode for quick real-time reductions, which are used primarily for basic data visualization and quality assessment done at the telescope while observing. The offline version of the data reduction system includes an expanded reduction method list, does more iterations for a better construction of the data cubes, and is used to produce publication-quality products. It can also use reconstruction matrices that are developed after the observations were taken, and are more refined. The KOA team is currently utilizing the standard offline reduction mode to produce quick-look browse products for the raw data. Users of the offline data reduction system generally use a graphical user interface to manually setup the reduction parameters. However, in order to reduce and serve the 200,000 science files on disk, all of the reduction parameters and steps need to be fully automated. This pipeline will also be used to automatically produce quick-look browse products for future OSIRIS data after each night's observations. Here we discuss the complexities of OSIRIS data, the reduction system in place, methods for automating the system, performance using virtualization, and progress made to date in generating the KOA products.

  19. The Instrument Implementation of Two-tier Multiple Choice to Analyze Students’ Science Process Skill Profile

    Directory of Open Access Journals (Sweden)

    Sukarmin Sukarmin

    2018-01-01

    Full Text Available This research is aimed to analyze the profile of students’ science process skill (SPS by using instrument two-tier multiple choice. This is a descriptive research that describes the profile of students’ SPS. Subjects of the research were 10th-grade students from high, medium and low categorized school. Instrument two-tier multiple choice consists of 30 question that contains an indicator of SPS. The indicator of SPS namely formulating a hypothesis, designing experiment, analyzing data, applying the concept, communicating, making a conclusion. Based on the result of the research and analysis, it shows that: 1 the average of indicator achievement of science process skill at high categorized school on formulating hypothesis is 74,55%, designing experiment is 74,89%, analyzing data is 67,89%, applying concept is 52,89%, communicating is 80,22%, making conclusion is 76%, 2. the average of indicator achievement of science process skill at medium categorized school on formulating hypothesis is 53,47%, designing experiment is 59,86%, analyzing data is 42,22%, applying concept is 33,19%, communicating is 76,25%, making conclusion is 61,53%, 3 the average of indicator achievement of science process skill at low categorized school on formulating hypothesis is 51%, designing experiment is 55,17%, analyzing data is 39,17%, applying concept is 35,83%, communicating is 58,83%, making conclusion is 58%.

  20. With hiccups and bumps: the development of a Rasch-based instrument to measure elementary students' understanding of the nature of science.

    Science.gov (United States)

    Peoples, Shelagh M; O'Dwyer, Laura M; Shields, Katherine A; Wang, Yang

    2013-01-01

    This research describes the development process, psychometric analyses and part validation study of a theoretically-grounded Rasch-based instrument, the Nature of Science Instrument-Elementary (NOSI-E). The NOSI-E was designed to measure elementary students' understanding of the Nature of Science (NOS). Evidence is provided for three of the six validity aspects (content, substantive and generalizability) needed to support the construct validity of the NOSI-E. A future article will examine the structural and external validity aspects. Rasch modeling proved especially productive in scale improvement efforts. The instrument, designed for large-scale assessment use, is conceptualized using five construct domains. Data from 741 elementary students were used to pilot the Rasch scale, with continuous improvements made over three successive administrations. The psychometric properties of the NOSI-E instrument are consistent with the basic assumptions of Rasch measurement, namely that the items are well-fitting and invariant. Items from each of the five domains (Empirical, Theory-Laden, Certainty, Inventive, and Socially and Culturally Embedded) are spread along the scale's continuum and appear to overlap well. Most importantly, the scale seems appropriately calibrated and responsive for elementary school-aged children, the target age group. As a result, the NOSI-E should prove beneficial for science education research. As the United States' science education reform efforts move toward students' learning science through engaging in authentic scientific practices (NRC, 2011), it will be important to assess whether this new approach to teaching science is effective. The NOSI-E can be used as one measure of whether this reform effort has an impact.

  1. Heliophysics: The New Science of the Sun-Solar System Connection. Recommended Roadmap for Science and Technology 2005-2035

    Science.gov (United States)

    2005-01-01

    This is a Roadmap to understanding the environment of our Earth, from its life-sustaining Sun out past the frontiers of the solar system. A collection of spacecraft now patrols this space, revealing not a placid star and isolated planets, but an immense, dynamic, interconnected system within which our home planet is embedded and through which space explorers must journey. These spacecraft already form a great observatory with which the Heliophysics program can study the Sun, the heliosphere, the Earth, and other planetary environments as elements of a system--one that contains dynamic space weather and evolves in response to solar, planetary, and interstellar variability. NASA continually evolves the Heliophysics Great Observatory by adding new missions and instruments in order to answer the challenging questions confronting us now and in the future as humans explore the solar system. The three heliophysics science objectives: opening the frontier to space environment prediction; understanding the nature of our home in space, and safeguarding the journey of exploration, require sustained research programs that depend on combining new data, theory, analysis, simulation, and modeling. Our program pursues a deeper understanding of the fundamental physical processes that underlie the exotic phenomena of space.

  2. The development and validation of the Self-Efficacy Beliefs about Equitable Science Teaching and learning instrument for prospective elementary teachers

    Science.gov (United States)

    Ritter, Jennifer M.

    1999-12-01

    The purpose of this study was to develop, validate and establish the reliability of an instrument to assess the self-efficacy beliefs of prospective elementary teachers with regards to science teaching and learning for diverse learners. The study used Bandura's theoretical framework, in that the instrument would use the self-efficacy construct to explore the beliefs of prospective elementary science teachers with regards to science teaching and learning to diverse learners: specifically the two dimensions of self-efficacy beliefs defined by Bandura (1977): personal self-efficacy and outcome expectancy. A seven step plan was designed and followed in the process of developing the instrument, which was titled the Self-Efficacy Beliefs about Equitable Science Teaching or SEBEST. Diverse learners as recognized by Science for All Americans (1989) are "those who in the past who have largely been bypassed in science and mathematics education: ethnic and language minorities and girls" (p. xviii). That definition was extended by this researcher to include children from low socioeconomic backgrounds based on the research by Gomez and Tabachnick (1992). The SEBEST was administered to 226 prospective elementary teachers at The Pennsylvania State University. Using the results from factor analyses, Coefficient Alpha, and Chi-Square a 34 item instrument was found to achieve the greatest balance across the construct validity, reliability and item balance with the content matrix. The 34 item SEBEST was found to load purely on four factors across the content matrix thus providing evidence construct validity. The Coefficient Alpha reliability for the 34 item SEBEST was .90 and .82 for the PSE sub-scale and .78 for the OE sub-scale. A Chi-Square test (X2 = 2.7 1, df = 7, p > .05) was used to confirm that the 34 items were balanced across the Personal Self-Efficacy/Outcome Expectancy and Ethnicity/LanguageMinority/Gender Socioeconomic Status/dimensions of the content matrix. Based on

  3. An automatic DI-flux at the Livingston Island geomagnetic observatory, Antarctica: requirements and lessons learned

    Science.gov (United States)

    Marsal, Santiago; José Curto, Juan; Torta, Joan Miquel; Gonsette, Alexandre; Favà, Vicent; Rasson, Jean; Ibañez, Miquel; Cid, Òscar

    2017-07-01

    The DI-flux, consisting of a fluxgate magnetometer coupled with a theodolite, is used for the absolute manual measurement of the magnetic field angles in most ground-based observatories worldwide. Commercial solutions for an automated DI-flux have recently been developed by the Royal Meteorological Institute of Belgium (RMI), and are practically restricted to the AutoDIF and its variant, the GyroDIF. In this article, we analyze the pros and cons of both instruments in terms of its suitability for installation at the partially manned geomagnetic observatory of Livingston Island (LIV), Antarctica. We conclude that the GyroDIF, even if it is less accurate and more power demanding, is more suitable than the AutoDIF for harsh conditions due to the simpler infrastructure that is necessary. Power constraints in the Spanish Antarctic Station Juan Carlos I (ASJI) during the unmanned season require an energy-efficient design of the thermally regulated box housing the instrument as well as thorough power management. Our experiences can benefit the geomagnetic community, which often faces similar challenges.

  4. An automatic DI-flux at the Livingston Island geomagnetic observatory, Antarctica: requirements and lessons learned

    Directory of Open Access Journals (Sweden)

    S. Marsal

    2017-07-01

    Full Text Available The DI-flux, consisting of a fluxgate magnetometer coupled with a theodolite, is used for the absolute manual measurement of the magnetic field angles in most ground-based observatories worldwide. Commercial solutions for an automated DI-flux have recently been developed by the Royal Meteorological Institute of Belgium (RMI, and are practically restricted to the AutoDIF and its variant, the GyroDIF. In this article, we analyze the pros and cons of both instruments in terms of its suitability for installation at the partially manned geomagnetic observatory of Livingston Island (LIV, Antarctica. We conclude that the GyroDIF, even if it is less accurate and more power demanding, is more suitable than the AutoDIF for harsh conditions due to the simpler infrastructure that is necessary. Power constraints in the Spanish Antarctic Station Juan Carlos I (ASJI during the unmanned season require an energy-efficient design of the thermally regulated box housing the instrument as well as thorough power management. Our experiences can benefit the geomagnetic community, which often faces similar challenges.

  5. Six Years of Science with the TAROT Telescope at La Silla

    Science.gov (United States)

    Klotz, A.; Boer, M.; Atteia, J.-L.; Gendre, B.; Le Borgne, J.-F.; Frappa, E.; Vachier, F.; Berthier, J.

    2013-03-01

    The TAROT telescopes are a pair of robotic autonomous observatories with identical suites of instrumentation, with one located in each hemisphere. The southern TAROT telescope, which was installed in 2006 at the La Silla Observatory, uses more than 90% of the clear night-time, and has become a very reliable and productive instrument. The primary objective of TAROT is the detection and study of the optical counter-parts of cosmic gamma-ray bursts, and many results have been obtained in this area. But several other topics, ranging from stellar physics to supernovae, have also been addressed successfully thanks to the telescope's flexibility. We present the main scientific results obtained by the TAROT robotic observatory at La Silla.

  6. NASA Unveils First Images From Chandra X-Ray Observatory

    Science.gov (United States)

    1999-08-01

    Extraordinary first images from NASA's Chandra X-ray Observatory trace the aftermath of a gigantic stellar explosion in such stunning detail that scientists can see evidence of what may be a neutron star or black hole near the center. Another image shows a powerful X-ray jet blasting 200,000 light years into intergalactic space from a distant quasar. Released today, both images confirm that NASA's newest Great Observatory is in excellent health and its instruments and optics are performing up to expectations. Chandra, the world's largest and most sensitive X-ray telescope, is still in its orbital check-out and calibration phase. "When I saw the first image, I knew that the dream had been realized," said Dr. Martin Weisskopf, Chandra Project Scientist, NASA's Marshall Space Flight Center, Huntsville, AL. "This observatory is ready to take its place in the history of spectacular scientific achievements." "We were astounded by these images," said Harvey Tananbaum, Director of the Smithsonian Astrophysical Observatory's Chandra X- ray Center, Cambridge, MA. "We see the collision of the debris from the exploded star with the matter around it, we see shock waves rushing into interstellar space at millions of miles per hour, and, as a real bonus, we see for the first time a tantalizing bright point near the center of the remnant that could possibly be a collapsed star associated with the outburst." Chandra's PKS 0637-752 PKS 0637-752 After the telescope's sunshade door was opened last week, one of the first images taken was of the 320-year-old supernova remnant Cassiopeia A, which astronomers believe was produced by the explosion of a massive star. Material blasted into space from the explosion crashed into surrounding material at 10 million miles per hour. This collision caused violent shock waves, like massive sonic booms, creating a vast 50-million degree bubble of X-ray emitting gas. Heavy elements in the hot gas produce X-rays of specific energies. Chandra's ability

  7. ESA's X-ray space observatory XMM takes first pictures

    Science.gov (United States)

    2000-02-01

    functioning of the observatory. The Optical Monitor also simultaneously viewed the same regions. One RGS spectrometer obtained its first spectra on 25 January; the other will be commissioned at the start of February. This initial series of short and long duration exposures have delighted the Project management team and the scientists even more. First analyses confirm that the spacecraft is extremely stable, the XMM telescopes are focusing perfectly, and the EPIC cameras, Optical Monitor and RGS spectrometers are working exactly as expected. The Science Operations Centre infrastructure, processing and archiving the science data telemetry from the spacecraft, is also performing well. Initial inspection of the first commissioning images immediately showed some unique X-ray views of several celestial objects, to be presented on 9 February. The occasion will give Principal Investigators and Project management the opportunity to comment on the pictures and the excellent start of the XMM mission. The Calibration and Performance Verification phase for XMM's science instruments is to begin on 3 March, with routine science operations starting in June. Press is invited to attend to the press conference that will be held at the Villafranca/ Madrid- Vilspa facility (ESA's Satellite Tracking Station) Apartado 50727, E-2 080 MADRID, Spain. The press event will be broadcast to the other ESA establishments: ESA Headquarters, Paris; ESA/ ESTEC (Space Expo), Noordwijk, the Netherlands; ESA/ESOC, Darmstadt, Germany and ESA/ESRIN, Frascati, Italy. Media representatives wishing to attend the event are kindly requested to fill out the attached reply from and fax it back to the establishment of their choice.

  8. Taking Charge: Walter Sydney Adams and the Mount Wilson Observatory

    Science.gov (United States)

    Brashear, R.

    2004-12-01

    The growing preeminence of American observational astronomy in the first half of the 20th century is a well-known story and much credit is given to George Ellery Hale and his skill as an observatory-building entrepreneur. But a key figure who has yet to be discussed in great detail is Walter Sydney Adams (1876-1956), Hale's Assistant Director at Mount Wilson Observatory. Due to Hale's illnesses, Adams was Acting Director for much of Hale's tenure, and he became the second Director of Mount Wilson from 1923 to 1946. Behind his New England reserve Adams was instrumental in the growth of Mount Wilson and thus American astronomy in general. Adams was hand-picked by Hale to take charge of stellar spectroscopy work at Yerkes and Mount Wilson and the younger astronomer showed tremendous loyalty to Hale and Hale's vision throughout his career. As Adams assumed the leadership role at Mount Wilson he concentrated on making the observatory a place where researchers worked with great freedom but maintain a high level of cooperation. This paper will concentrate on Adams's early years and look at his growing relationship with Hale and how he came to be the central figure in the early history of Mount Wilson as both a solar and stellar observatory. His education, his years at Dartmouth and Yerkes (including his unfortunate encounter with epsilon Leonis), and his formative years on Mount Wilson are all important in learning how he shaped the direction of Mount Wilson and the development of American astronomy in the first half of the 20th century. This latter history cannot be complete until we bring Adams into better focus.

  9. Autonomous Infrastructure for Observatory Operations

    Science.gov (United States)

    Seaman, R.

    This is an era of rapid change from ancient human-mediated modes of astronomical practice to a vision of ever larger time domain surveys, ever bigger "big data", to increasing numbers of robotic telescopes and astronomical automation on every mountaintop. Over the past decades, facets of a new autonomous astronomical toolkit have been prototyped and deployed in support of numerous space missions. Remote and queue observing modes have gained significant market share on the ground. Archives and data-mining are becoming ubiquitous; astroinformatic techniques and virtual observatory standards and protocols are areas of active development. Astronomers and engineers, planetary and solar scientists, and researchers from communities as diverse as particle physics and exobiology are collaborating on a vast range of "multi-messenger" science. What then is missing?

  10. Optical Spectroscopy with the Technology of Virtual Observatory

    Science.gov (United States)

    Škoda, P.

    The contemporary astronomy is flooded with an exponentially growing petabyte-scaled data volumes produced by powerful ground and space-based instrumentation as well as a product of extensive computer simulations and computations of complex numerical models. The efficient organization and seamless handling of this information avalanche stored in a world-wide spread heterogeneous databases and the facilitation of extraction of new physical knowledge about the Universe is a primary goal of the rapidly evolving astronomical Virtual Observatory (VO). We give an overview of current spectroscopic capabilities of VO and identify the future requirements indispensable for detailed multi-wavelength analysis of huge amounts of spectra in a semi-automatic manner.

  11. An Engineering Design Reference Mission for a Future Large-Aperture UVOIR Space Observatory

    Science.gov (United States)

    Thronson, Harley A.; Bolcar, Matthew R.; Clampin, Mark; Crooke, Julie A.; Redding, David; Rioux, Norman; Stahl, H. Philip

    2016-01-01

    From the 2010 NRC Decadal Survey and the NASA Thirty-Year Roadmap, Enduring Quests, Daring Visions, to the recent AURA report, From Cosmic Birth to Living Earths, multiple community assessments have recommended development of a large-aperture UVOIR space observatory capable of achieving a broad range of compelling scientific goals. Of these priority science goals, the most technically challenging is the search for spectroscopic biomarkers in the atmospheres of exoplanets in the solar neighborhood. Here we present an engineering design reference mission (EDRM) for the Advanced Technology Large-Aperture Space Telescope (ATLAST), which was conceived from the start as capable of breakthrough science paired with an emphasis on cost control and cost effectiveness. An EDRM allows the engineering design trade space to be explored in depth to determine what are the most demanding requirements and where there are opportunities for margin against requirements. Our joint NASA GSFC/JPL/MSFC/STScI study team has used community-provided science goals to derive mission needs, requirements, and candidate mission architectures for a future large-aperture, non-cryogenic UVOIR space observatory. The ATLAST observatory is designed to operate at a Sun-Earth L2 orbit, which provides a stable thermal environment and excellent field of regard. Our reference designs have emphasized a serviceable 36-segment 9.2 m aperture telescope that stows within a five-meter diameter launch vehicle fairing. As part of our cost-management effort, this particular reference mission builds upon the engineering design for JWST. Moreover, it is scalable to a variety of launch vehicle fairings. Performance needs developed under the study are traceable to a variety of additional reference designs, including options for a monolithic primary mirror.

  12. The Organization and Management of the Virtual Astronomical Observatory

    Science.gov (United States)

    Berriman, G. Bruce; Hanisch, Robert J.; Lazio, T. Joseph W.; Szalay, Alexander; Fabbiano, Giussepina

    2012-01-01

    The U.S. Virtual Astronomical Observatory (VAO; http://www.us-vao.org/) has been in operation since May 2010. Its goal is to enable new science through efficient integration of distributed multi-wavelength data. This paper describes the management and organization of the VAO, and emphasizes the techniques used to ensure efficiency in a distributed organization. Management methods include using an annual program plan as the basis for establishing contracts with member organizations, regular communication, and monitoring of processes.

  13. Cascadia, an ultracompact seismic instrument with over 200dB of dynamic range

    Science.gov (United States)

    Parker, Tim; Devanney, Peter; Bainbridge, Geoff; Townsend, Bruce

    2017-04-01

    Integration of geophysical instrumentation is clearly a way to lower overall station cost, make installations less complex, reduce installation time, increase station utility and value to a wider group of researchers, data miners and monitoring groups. Initiatives to expand early earthquake warning networks and observatories can use these savings for increasing station density. Integration of mature instrument systems such as broadband sensors and accelerometers used in strong motion studies has to be done with care to preserve the low noise and low frequency performance while providing over 200dB of dynamic range. Understanding the instrument complexities and deployment challenges allows the engineering teams to optimize the packaging to make installation and servicing cost effective, simple, routine and ultimately more reliable. We discuss early results from testing both in the lab and in the field of a newly released instrument called the Cascadia that integrates a broadband seismometer with a class A (USGS rating) accelerometer in a small stainless steel sonde suited for dense arrays in either ad hoc direct bury field deployments or in observatory quality shallow boreholes.

  14. Instrumental traditions and theories of light the uses of instruments in the optical revolution

    CERN Document Server

    Chen, Xiang

    2000-01-01

    An analysis of the optical revolution in the context of early 19th century Britain. Far from merely involving the replacement of one optical theory by another, the revolution also involved substantial changes in instruments and the practices that surrounded them. People's judgements about classification, explanation and evaluation were affected by the way they used such optical instruments as spectroscopes, telescopes, polarisers, photometers, gratings, prisms and apertures. There were two instrumental traditions in this historical period, each of which nurtured a body of practice that exemplified how optical instruments should be operated, and especially how the eye should be used. These traditions functioned just like paradigms, shaping perspectives and even world views. Readership: Scholars and graduate students in the history of science, history of instrument, philosophy of science and science studies. Can also be used as a textbook in graduate courses on 19th century physics.

  15. Evolution and validation of a personal form of an instrument for assessing science laboratory classroom environments

    Science.gov (United States)

    Fraser, Barry J.; Giddings, Geoffrey J.; McRobbie, Campbell J.

    The research reported in this article makes two distinctive contributions to the field of classroom environment research. First, because existing instruments are unsuitable for science laboratory classes, the Science Laboratory Environment Inventory (SLEI) was developed and validated. Second, a new Personal form of the SLEI (involving a student's perceptions of his or her own role within the class) was developed and validated in conjunction with the conventional Class form (involving a student's perceptions of the class as a whole), and its usefulness was investigated. The instrument was cross-nationally fieldtested with 5,447 students in 269 senior high school and university classes in six countries, and cross-validated with 1,594 senior high school students in 92 classes in Australia. Each SLEI scale exhibited satisfactory internal consistency reliability, discriminant validity, and factorial validity, and differentiated between the perceptions of students in different classes. A variety of applications with the new instrument furnished evidence about its usefulness and revealed that science laboratory classes are dominated by closed-ended activities; mean scores obtained on the Class form were consistently somewhat more favorable than on the corresponding Personal form; females generally held more favorable perceptions than males, but these differences were somewhat larger for the Personal form than the Class form; associations existed between attitudinal outcomes and laboratory environment dimensions; and the Class and Personal forms of the SLEI each accounted for unique variance in student outcomes which was independent of that accounted for by the other form.

  16. The LCOGT Science Archive and Data Pipeline

    Science.gov (United States)

    Lister, Tim; Walker, Z.; Ciardi, D.; Gelino, C. R.; Good, J.; Laity, A.; Swain, M.

    2013-01-01

    Las Cumbres Observatory Global Telescope (LCOGT) is building and deploying a world-wide network of optical telescopes dedicated to time-domain astronomy. In the past year, we have deployed and commissioned four new 1m telescopes at McDonald Observatory, Texas and at CTIO, Chile, with more to come at SAAO, South Africa and Siding Spring Observatory, Australia. To handle these new data sources coming from the growing LCOGT network, and to serve them to end users, we have constructed a new data pipeline and Science Archive. We describe the new LCOGT pipeline, currently under development and testing, which makes use of the ORAC-DR automated recipe-based data reduction pipeline and illustrate some of the new data products. We also present the new Science Archive, which is being developed in partnership with the Infrared Processing and Analysis Center (IPAC) and show some of the new features the Science Archive provides.

  17. Telemetry and Science Data Software System

    Science.gov (United States)

    Bates, Lakesha; Hong, Liang

    2011-01-01

    The Telemetry and Science Data Software System (TSDSS) was designed to validate the operational health of a spacecraft, ease test verification, assist in debugging system anomalies, and provide trending data and advanced science analysis. In doing so, the system parses, processes, and organizes raw data from the Aquarius instrument both on the ground and while in space. In addition, it provides a user-friendly telemetry viewer, and an instant pushbutton test report generator. Existing ground data systems can parse and provide simple data processing, but have limitations in advanced science analysis and instant report generation. The TSDSS functions as an offline data analysis system during I&T (integration and test) and mission operations phases. After raw data are downloaded from an instrument, TSDSS ingests the data files, parses, converts telemetry to engineering units, and applies advanced algorithms to produce science level 0, 1, and 2 data products. Meanwhile, it automatically schedules upload of the raw data to a remote server and archives all intermediate and final values in a MySQL database in time order. All data saved in the system can be straightforwardly retrieved, exported, and migrated. Using TSDSS s interactive data visualization tool, a user can conveniently choose any combination and mathematical computation of interesting telemetry points from a large range of time periods (life cycle of mission ground data and mission operations testing), and display a graphical and statistical view of the data. With this graphical user interface (GUI), the data queried graphs can be exported and saved in multiple formats. This GUI is especially useful in trending data analysis, debugging anomalies, and advanced data analysis. At the request of the user, mission-specific instrument performance assessment reports can be generated with a simple click of a button on the GUI. From instrument level to observatory level, the TSDSS has been operating supporting

  18. Operating a wide-area high-availability collaborative remote observing system for classically-scheduled observations at the W. M. Keck Observatory

    Science.gov (United States)

    Kibrick, Robert I.; Wirth, Gregory D.; Allen, Steven L.; Deich, William T. S.; Goodrich, Robert W.; Lanclos, Kyle; Lyke, James E.

    2011-03-01

    For over a decade, the W. M. Keck Observatory's two 10-meter telescopes have been operated remotely from its Waimea headquarters. Over the last 9 years, WMKO remote observing has expanded to allow observing teams at dedicated sites located across California to observe via the Internet either in collaboration with colleagues in Waimea or entirely from California; this capability was extended to Swinburne University in Melbourne, Australia in 2010 and to Yale University in New Haven, Connecticut in early 2011. All Keck facility science instruments are currently supported. Observers distributed between as many as four sites can collaborate in the interactive operation of each instrument by means of shared VNC desktops and multipoint video and/or telephone conferencing. Automated routers at primary remote observing sites ensure continued connectivity during Internet outages. Each Keck remote observing facility is similarly equipped and configured so observers have the same operating environment. This architecture provides observers the flexibility to conduct observations from the location best suited to their needs and to adapt to last-minute changes. It also enhances the ability of off-site technical staff to provide remote support.

  19. Development of perceived instrumentality for mathematics, reading and science curricula

    Science.gov (United States)

    Garcia, Steve L.

    Perceptions of instrumentality (PI) are the connections one sees between a current activity and a future goal. With high PI, one is motivated to persist with quality effort because the current activity, even when difficult, is perceived as aligned with, and progress toward, the goal. Conversely, with low PI, one is motivated to relinquish effort in pursuit of other, more meaningful goals. In view of the alarming dropout rates in this country, it appears that PI research has much to offer in understanding students' motivations to stay in school and hence to become employed in their field of choice. Because academic achievement motivation can be affected by gender and ethnicity, particularly for specific components of the curriculum, and because curricular content varies across grade levels and school settings, this line of research offers significant potential for understanding and improving student outcomes. This research examined the development of PI among suburban 6th, 8th, 10th and 12th graders from a school district in the southwestern United States. Twelve hundred students completed a one-time paper and pencil survey measuring the perceived instrumentality of mathematics, literacy and science courses in terms of the students' occupational choices. MANOVA was used to determine factors that may affect students' overall PI and individual subject PI. Grade, gender, ethnicity, occupational choice, expectancy and value were the independent variables. A school setting variable was examined for effects on 12th graders. For the 8th through 12th grade sample, significant main effects were observed for grade, gender, minority status, occupational choice and expectancy on PI. Results show that PI is highest in the 6 th grade. Males reported higher Math PI than females. Females reported higher Reading PI and Science PI than males. Minority students reported lower overall PI and Science PI than non-minority students. Students who aspire to professional careers report the

  20. Jovian seismology: preliminary results of the SYMPA instrument

    Science.gov (United States)

    Gaulme, P.; Schmider, F. X.; Gay, J.; Jacob, C.; Jeanneaux, F.; Alvarez, M.; Reyes, M.; Valtier, J. C.; Fossat, E.; Palle, P. L.; Belmonte, J. C.; Gelly, B.

    2006-06-01

    Jupiter's internal structure is poorly known (Guillot et al. 2004). Seismology is a powerful tool to investigate the internal structure of planets and stars, by analyzing how acoustic waves propagate. Mosser (1997) and Gudkova & Zarkhov (1999) showed that the detection and the identification of non-radial modes up to degree ℓ=25 can constrain strongly the internal structure. SYMPA is a ground-based network project dedicated to the Jovian oscillations (Schmider et al. 2002). The instrument is composed of a Mach-Zehnder interferometer producing four interferograms of the planetary spectrum. The combination of the four images in phase quadrature allows the reconstruction of the incident light phase, which is related to the Doppler shift generated by the oscillations. Two SYMPA instruments were built at the Nice university and were used simultaneously during two observation campaigns, in 2004 and 2005, at the San Pedro Martir observatory (Mexico) and the Teide observatory (Las Canarias). We will present for the first time the data processing and the preliminary results of the experiment.

  1. Measurement Instrument for Scientific Teaching (MIST): A Tool to Measure the Frequencies of Research-Based Teaching Practices in Undergraduate Science Courses.

    Science.gov (United States)

    Durham, Mary F; Knight, Jennifer K; Couch, Brian A

    2017-01-01

    The Scientific Teaching (ST) pedagogical framework provides various approaches for science instructors to teach in a way that more closely emulates how science is practiced by actively and inclusively engaging students in their own learning and by making instructional decisions based on student performance data. Fully understanding the impact of ST requires having mechanisms to quantify its implementation. While many useful instruments exist to document teaching practices, these instruments only partially align with the range of practices specified by ST, as described in a recently published taxonomy. Here, we describe the development, validation, and implementation of the Measurement Instrument for Scientific Teaching (MIST), a survey derived from the ST taxonomy and designed to gauge the frequencies of ST practices in undergraduate science courses. MIST showed acceptable validity and reliability based on results from 7767 students in 87 courses at nine institutions. We used factor analyses to identify eight subcategories of ST practices and used these categories to develop a short version of the instrument amenable to joint administration with other research instruments. We further discuss how MIST can be used by instructors, departments, researchers, and professional development programs to quantify and track changes in ST practices. © 2017 M. F. Durham et al. CBE—Life Sciences Education © 2017 The American Society for Cell Biology. This article is distributed by The American Society for Cell Biology under license from the author(s). It is available to the public under an Attribution–Noncommercial–Share Alike 3.0 Unported Creative Commons License (http://creativecommons.org/licenses/by-nc-sa/3.0).

  2. In situ vector calibration of magnetic observatories

    Directory of Open Access Journals (Sweden)

    A. Gonsette

    2017-09-01

    Full Text Available The goal of magnetic observatories is to measure and provide a vector magnetic field in a geodetic coordinate system. For that purpose, instrument set-up and calibration are crucial. In particular, the scale factor and orientation of a vector magnetometer may affect the magnetic field measurement. Here, we highlight the baseline concept and demonstrate that it is essential for data quality control. We show how the baselines can highlight a possible calibration error. We also provide a calibration method based on high-frequency absolute measurements. This method determines a transformation matrix for correcting variometer data suffering from scale factor and orientation errors. We finally present a practical case where recovered data have been successfully compared to those coming from a reference magnetometer.

  3. Look to the Stars - The APUS Observatory: An Innovative Robotic Telescope for Online Astronomical Education and Research

    Science.gov (United States)

    Albin, Edward

    2018-01-01

    We report on the American Public University System’s new robotic telescope, located in Charles Town, WV -- an innovative observatory deployed in an online institution of higher education. The instrument is operated by the Department of Space Studies and is situated atop the university’s new Information Technology building. At the heart of the observatory is a Planewave CDK24 telescope, equipped with a SBIG STX-16803 CCD camera. The telescope is a key technological component in the Department's new undergraduate / graduate astronomy concentration. Since the university is a dedicated online educational institution, the acquisition of a fully remote controlled telescope ties closely into the program's philosophy of quality online instruction. Our robotic observatory is intimately integrated into our astronomy curriculum, with the telescope being utilized for original astronomical education and research purposes. For instance, not only is imagery used in the classroom and for laboratory instruction, graduate students in our MS degree program have an opportunity to collect original telescopic data for research / thesis projects. Examples of ongoing investigations with the telescope include observations of exoplanet transits and variable star photometry. When not in use for specific observing projects, the telescope is scripted to conduct autonomous supernova searches by patrolling dozens of galaxies throughout the night. Our goal is to have the instrument scheduled for continuous observing of the heavens throughout the year on all clear evenings.

  4. TMT approach to observatory software development process

    Science.gov (United States)

    Buur, Hanne; Subramaniam, Annapurni; Gillies, Kim; Dumas, Christophe; Bhatia, Ravinder

    2016-07-01

    The purpose of the Observatory Software System (OSW) is to integrate all software and hardware components of the Thirty Meter Telescope (TMT) to enable observations and data capture; thus it is a complex software system that is defined by four principal software subsystems: Common Software (CSW), Executive Software (ESW), Data Management System (DMS) and Science Operations Support System (SOSS), all of which have interdependencies with the observatory control systems and data acquisition systems. Therefore, the software development process and plan must consider dependencies to other subsystems, manage architecture, interfaces and design, manage software scope and complexity, and standardize and optimize use of resources and tools. Additionally, the TMT Observatory Software will largely be developed in India through TMT's workshare relationship with the India TMT Coordination Centre (ITCC) and use of Indian software industry vendors, which adds complexity and challenges to the software development process, communication and coordination of activities and priorities as well as measuring performance and managing quality and risk. The software project management challenge for the TMT OSW is thus a multi-faceted technical, managerial, communications and interpersonal relations challenge. The approach TMT is using to manage this multifaceted challenge is a combination of establishing an effective geographically distributed software team (Integrated Product Team) with strong project management and technical leadership provided by the TMT Project Office (PO) and the ITCC partner to manage plans, process, performance, risk and quality, and to facilitate effective communications; establishing an effective cross-functional software management team composed of stakeholders, OSW leadership and ITCC leadership to manage dependencies and software release plans, technical complexities and change to approved interfaces, architecture, design and tool set, and to facilitate

  5. Inventing a space mission the story of the Herschel space observatory

    CERN Document Server

    Minier, Vincent; Bontems, Vincent; de Graauw, Thijs; Griffin, Matt; Helmich, Frank; Pilbratt, Göran; Volonte, Sergio

    2017-01-01

    This book describes prominent technological achievements within a very successful space science mission: the Herschel space observatory. Focusing on the various processes of innovation it offers an analysis and discussion of the social, technological and scientific context of the mission that paved the way to its development. It addresses the key question raised by these processes in our modern society, i.e.: how knowledge management of innovation set the conditions for inventing the future? In that respect the book is based on a transdisciplinary analysis of the programmatic complexity of Herschel, with inputs from space scientists, managers, philosophers, and engineers. This book is addressed to decision makers, not only in space science, but also in other industries and sciences using or building large machines. It is also addressed to space engineers and scientists as well as students in science and management.

  6. From EXOSAT to the High Energy Astrophysics Science Archive (HEASARC): X-ray Astronomy Comes of Age

    Science.gov (United States)

    White, Nicholas E.

    2012-01-01

    In May 1983 the European Space Agency launched EXOSAT, its first X-ray astronomy observatory. Even though it lasted only 3 short years, this mission brought not only new capabilities that resulted in unexpected discoveries, but also a pioneering approach to operations and archiving that changed X-ray astronomy from observations led by small instrument teams, to an observatory approach open to the entire community through a guest observer program. The community use of the observatory was supported by a small dedicated team of scientists, the precursor to the data center activities created to support e.g. Chandra and XMM-Newton. The new science capabilities of EX OS AT included a 90 hr highly eccentric high earth orbit that allow unprecedented continuous coverage of sources as well as direct communication with the satellite that allowed real time decisions to respond to unexpected events through targets of opportunity. The advantages of this orbit demonstrated by EXOSAT resulted in Chandra and XMM-Newton selecting similar orbits. The three instruments on board the EXOSAT observatory were complementary, designed to give complete coverage over a wide energy band pass of 0.05-50 keY. An onboard processor could be programmed to give multiple data modes that could be optimized in response to science discoveries: These new capabilities resulted in many new discoveries including the first comprehensive study of AGN variability, new orbital periods in X-ray binaries and cataclysmic variables, new black holes, quasi-periodic oscillations from neutron stars and black holes and broad band X-ray spectroscopy. The EXOSAT team generated a well-organized database accessible worldwide over the nascent internet, allowing remote selection of data products, making samples and undertaking surveys from the data. The HEASARC was established by NASA at Goddard Space Flight Center in 1990 as the repository of NASA X-ray and Gamma-ray data. The proven EXOSAT database system became the core

  7. CALIPSO Borehole Instrumentation Project at Soufriere Hills Volcano, Montserrat, BWI: Data Acquisition, Telemetry, Integration, and Archival Systems

    Science.gov (United States)

    Mattioli, G. S.; Linde, A. T.; Sacks, I. S.; Malin, P. E.; Shalev, E.; Elsworth, D.; Hidayat, D.; Voight, B.; Young, S. R.; Dunkley, P. N.; Herd, R.; Norton, G.

    2003-12-01

    The CALIPSO Project (Caribbean Andesite Lava Island-volcano Precision Seismo-geodetic Observatory) has greatly enhanced the monitoring and scientific infrastructure at the Soufriere Hills Volcano, Montserrat with the recent installation of an integrated array of borehole and surface geophysical instrumentation at four sites. Each site was designed to be sufficiently hardened to withstand extreme meteorological events (e.g. hurricanes) and only require minimum routine maintenance over an expected observatory lifespan of >30 y. The sensor package at each site includes: a single-component, very broad band, Sacks-Evertson strainmeter, a three-component seismometer ( ˜Hz to 1 kHz), a Pinnacle Technologies series 5000 tiltmeter, and a surface Ashtech u-Z CGPS station with choke ring antenna, SCIGN mount and radome. This instrument package is similar to that envisioned by the Plate Boundary Observatory for deployment on EarthScope target volcanoes in western North America and thus the CALIPSO Project may be considered a prototype PBO installation with real field testing on a very active and dangerous volcano. Borehole sites were installed in series and data acquisition began immediately after the sensors were grouted into position at 200 m depth, with the first completed at Trants (5.8 km from dome) in 12-02, then Air Studios (5.2 km), Geralds (9.4 km), and Olveston (7.0 km) in 3-03. Analog data from the strainmeter (50 Hz sync) and seismometer (200 Hz) were initially digitized and locally archived using RefTek 72A-07 data acquisition systems (DAS) on loan from the PASSCAL instrument pool. Data were downloaded manually to a laptop approximately every month from initial installation until August 2003, when new systems were installed. Approximately 0.2 Tb of raw data in SEGY format have already been acquired and are currently archived at UARK for analysis by the CALIPSO science team. The July 12th dome collapse and vulcanian explosion events were recorded at 3 of the 4

  8. Teachers' conceptions of the nature of science: Analyzing the impact of a teacher enhancement program in changing attitudes and perceptions of science and scientific research

    Science.gov (United States)

    Govett, Aimee Lee

    The purpose of this study was to determine the efficacy of a residential science research experience in changing participants' attitudes and understanding of the nature of science and their view of themselves as science researchers. Data from interviews, journal writings, classroom observations and two pre-post instruments were used in the evaluation plan. As participants of this study, 16 inservice teachers (K--16) attended a two-week residential institute at the National Radio Astronomy Observatory (NRAO) in Green Bank, West Virginia. The format of the institute featured a scientific research experience designed to arm its participants with the skills needed to model their classroom teaching after scientific research. The program included lessons on the fundamentals of radio astronomy, science talks and interactions with practicing scientists, in-depth tours of the NRAO facilities, and pedagogical instruction for implementing research in the classroom. The WVU College of Education staff and the NRAO staff stressed the importance of the nature of the research experience offered to these teachers. In the Education Sessions the WVU science education staff guided participants through the steps required to turn their experience around, in order to develop student research projects for their classrooms. The results from the Research Self Assessment instrument show significant gains for all participants in being more comfortable doing research. For the Nature of Science and Science Teaching instrument there were only three items that showed significant gains for all participants both in understanding the nature of science and in their views on implementing the Green Bank constructivist learning philosophy. The women, especially the elementary teacher group, showed the greatest change in their understanding of the nature of science as reflected in the interviews as well as in their personal journals. The seven men, who were all in the secondary field, made no significant

  9. Stellar Radial Velocities with IGRINS at McDonald Observatory

    Science.gov (United States)

    Mace, Gregory; Jaffe, Daniel; Park, Chan; Lee, Jae-Joon

    2016-06-01

    Exoplanet searches with dedicated instrumentation have made 1 m/s radial velocity (RV) precision routine.Yet, RVs for large samples of stars generally remain at the 1km/s level.TheImmersion Grating Infrared Spectrometer (IGRINS) is a revolutionary instrument that exploits broad spectral coverage at high-resolution in the near-infrared.IGRINS on the 2.7 meter Harlan J. Smith Telescope at McDonald Observatory is nearly as sensitive as CRIRES at the 8 meter Very Large Telescope. However, IGRINS at R=45,000 has more than 30 times the spectral grasp of CRIRES.The use of a silicon immersion grating facilitates a compact cryostat while providing simultaneous wavelength coverage from 1.45 - 2.45 microns. Wehave developed a pipeline to cross-correlate the more than 20,000 resolution elements in two IGRINS exposures and provide relative RVs with uncertainties of 50m/s (product for multi-epoch studies of low-mass, stellar and substellar multiplicity.

  10. US Naval Observatory Hourly Observations

    Data.gov (United States)

    National Oceanic and Atmospheric Administration, Department of Commerce — Hourly observations journal from the National Observatory in Washington DC. The observatory is the first station in the United States to produce hourly observations...

  11. Optical Spectroscopy with the Technology of Virtual Observatory

    Directory of Open Access Journals (Sweden)

    Škoda P.

    2011-12-01

    Full Text Available The contemporary astronomy is flooded with an exponentially growing petabyte-scaled data volumes produced by powerful ground and space-based instrumentation as well as a product of extensive computer simulations and computations of complex numerical models. The efficient organization and seamless handling of this information avalanche stored in a world-wide spread heterogeneous databases and the facilitation of extraction of new physical knowledge about the Universe is a primary goal of the rapidly evolving astronomical Virtual Observatory (VO. We give an overview of current spectroscopic capabilities of VO and identify the future requirements indispensable for detailed multi-wavelength analysis of huge amounts of spectra in a semi-automatic manner.

  12. Core Facility of the Juelich Observatory for Cloud Evolution (JOYCE - CF)

    Science.gov (United States)

    Beer, J.; Troemel, S.

    2017-12-01

    A multiple and holistic multi-sensor monitoring of clouds and precipitation processes is a challenging but promising task in the meteorological community. Instrument synergies offer detailed views in microphysical and dynamical developments of clouds. Since 2017 The the Juelich Observatory for Cloud Evolution (JOYCE) is transformed into a Core Facility (JOYCE - CF). JOYCE - CF offers multiple long-term remote sensing observations of the atmosphere, develops an easy access to all observations and invites scientists word wide to exploit the existing data base for their research but also to complement JOYCE-CF with additional long-term or campaign instrumentation. The major instrumentation contains a twin set of two polarimetric X-band radars, a microwave profiler, two cloud radars, an infrared spectrometer, a Doppler lidar and two ceilometers. JOYCE - CF offers easy and open access to database and high quality calibrated observations of all instruments. E.g. the two polarimetric X-band radars which are located in 50 km distance are calibrated using the self-consistency method, frequently repeated vertical pointing measurements as well as instrument synergy with co-located micro-rain radar and distrometer measurements. The presentation gives insights into calibration procedures, the standardized operation procedures and recent synergistic research exploiting our radars operating at three different frequencies.

  13. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... School of Physics and Telecommunication Engineering, Shaanxi University of Technology, Shaanxi 723001, China. Yunnan Astronomical Observatory, National Astronomical Observatory, Chinese Academy of Sciences, Kunming, Yunnan 650011, China. College of Physics and Electronics, Yunnan ...

  14. Synchrotron light sources and free-electron lasers accelerator physics, instrumentation and science applications

    CERN Document Server

    Khan, Shaukat; Schneider, Jochen; Hastings, Jerome

    2016-01-01

    Hardly any other discovery of the nineteenth century did have such an impact on science and technology as Wilhelm Conrad Röntgen’s seminal find of the X-rays. X-ray tubes soon made their way as excellent instruments for numerous applications in medicine, biology, materials science and testing, chemistry and public security. Developing new radiation sources with higher brilliance and much extended spectral range resulted in stunning developments like the electron synchrotron and electron storage ring and the freeelectron laser. This handbook highlights these developments in fifty chapters. The reader is given not only an inside view of exciting science areas but also of design concepts for the most advanced light sources. The theory of synchrotron radiation and of the freeelectron laser, design examples and the technology basis are presented. The handbook presents advanced concepts like seeding and harmonic generation, the booming field of Terahertz radiation sources and upcoming brilliant light sources dri...

  15. Network analysis to support research management: evidence from the Fiocruz Observatory in Science, Technology and Innovation in Health

    Energy Technology Data Exchange (ETDEWEB)

    Fonseca, B.; Sampaio, R.B.; Silva, M.V.; Dos Santos, P.X.

    2016-07-01

    Brazil has been encouraging the establishment of research networks to address strategic health issues in response to social demands, creating an urgent need to develop indicators for their evaluation. The Oswaldo Cruz Foundation (Fiocruz), a national research, training and production institution, has initiated the development of an “Observatory in Science, Technology and Innovation in Health” to monitor and evaluate research and technological development for the formulation of institutional policies. In this context, we are proposing the use of social network analysis to map cooperation in strategic areas of research, identify prominent researchers and support internal research networks. In this preliminary study, coauthorship analysis was used to map the cooperative relations of Fiocruz in tuberculosis (TB) research, an important public health issue for which diagnosis and adequate treatment are still challenging. Our findings suggest that Brazilian research organizations acting in TB research are embedded in highly connected networks. The large number of international organizations present in the Brazilian network reflects the global increase in scientific collaboration and Brazil’s engagement in international collaborative research efforts. Fiocruz frequent cooperation with high-income countries demonstrates its concern in benefiting from the access to facilities, funding, equipment and networks that are often limited in its research setting. Collaboration with high burden countries has to be strengthened, as it could improve access to local knowledge and better understanding of the disease in different endemic contexts. Centrality analysis consolidated information on the importance of Fiocruz in connecting TB research institutions in Brazil. Fiocruz Observatory intends to advance this analysis by looking into the mechanisms of collaboration, identifying priority themes and assessing comparative advantages of the network members, an important contribution

  16. New sources and instrumentation for neutron science

    International Nuclear Information System (INIS)

    Gil, Alina

    2011-01-01

    Neutron-scattering research has a lot to do with our everyday lives. Things like medicine, food, electronics, cars and airplanes have all been improved by neutron-scattering research. Neutron research also helps scientists improve materials used in a multitude of different products, such as high-temperature superconductors, powerful lightweight magnets, stronger, lighter plastic products etc. Neutron scattering is one of the most effective ways to obtain information on both, the structure and the dynamics of condensed matter. Most of the world's neutron sources were built decades ago, and although the uses and demand for neutrons have increased throughout the years, few new sources have been built. The new construction, accelerator-based neutron source, the spallation source will provide the most intense pulsed neutron beams in the world for scientific research and industrial development. In this paper it will be described what neutrons are and what unique properties make them useful for science, how spallation source is designed to produce neutron beams and the experimental instruments that will use those beams. Finally, it will be described how past neutron research has affected our everyday lives and what we might expect from the most exciting future applications.

  17. New sources and instrumentation for neutron science

    Energy Technology Data Exchange (ETDEWEB)

    Gil, Alina, E-mail: a.gil@ajd.czest.pl [Faculty of Mathematical and Natural Sciences, JD University, Al. Armii Krajowej 13/15, 42-200 Czestochowa (Poland)

    2011-04-01

    Neutron-scattering research has a lot to do with our everyday lives. Things like medicine, food, electronics, cars and airplanes have all been improved by neutron-scattering research. Neutron research also helps scientists improve materials used in a multitude of different products, such as high-temperature superconductors, powerful lightweight magnets, stronger, lighter plastic products etc. Neutron scattering is one of the most effective ways to obtain information on both, the structure and the dynamics of condensed matter. Most of the world's neutron sources were built decades ago, and although the uses and demand for neutrons have increased throughout the years, few new sources have been built. The new construction, accelerator-based neutron source, the spallation source will provide the most intense pulsed neutron beams in the world for scientific research and industrial development. In this paper it will be described what neutrons are and what unique properties make them useful for science, how spallation source is designed to produce neutron beams and the experimental instruments that will use those beams. Finally, it will be described how past neutron research has affected our everyday lives and what we might expect from the most exciting future applications.

  18. Aquarius: The Instrument and Initial Results

    Science.gov (United States)

    Vine, David M Le; Lagerloef, G.S.E.; Ruf, C.; Wentz, F.; Yueh, S.; Piepmeier, J.; Lindstrom, E.; Dinnat, E.

    2012-01-01

    Aquarius was launched on June 10, 2011 aboard the Aquarius/SAC-D observatory and the instrument has been operating continuously since the initial turned-on was completed on August 25. The initial observed antenna temperatures were close to predicted and the first salinity map was released in September. In order to map the ocean salinity field, Aquarius includes several special features such as the inclusion of a scatterometer to provide a roughness correction, measurement of the third Stokes parameter to correct for Faraday rotation, and fast sampling to mitigate the effects of RFI. This paper provides an overview of the instrument and an example of initial results. Details are covered in subsequent papers in the session on Aquarius

  19. Observatory data and the Swarm mission

    DEFF Research Database (Denmark)

    Macmillan, S.; Olsen, Nils

    2013-01-01

    products. We describe here the preparation of the data set of ground observatory hourly mean values, including procedures to check and select observatory data spanning the modern magnetic survey satellite era. We discuss other possible combined uses of satellite and observatory data, in particular those......The ESA Swarm mission to identify and measure very accurately the different magnetic signals that arise in the Earth’s core, mantle, crust, oceans, ionosphere and magnetosphere, which together form the magnetic field around the Earth, has increased interest in magnetic data collected on the surface...... of the Earth at observatories. The scientific use of Swarm data and Swarm-derived products is greatly enhanced by combination with observatory data and indices. As part of the Swarm Level-2 data activities plans are in place to distribute such ground-based data along with the Swarm data as auxiliary data...

  20. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Yunnan Astronomical Observatory, National Astronomical Observatory, Chinese Academy of Science, Kunming, Yunnan 650011, China. College of Physics and Electronics, Yunnan Normal University, Kunming, Yunnan 650092, China. Department of Physics, Yuxi Teachers' College, Yuxi, Yunnan 653100, ...

  1. The Impact of Crosstalk in the X-IFU Instrument on Athena Science Cases

    Science.gov (United States)

    Hartog, R. Den; Peille, P.; Dauser, T.; Jackson, B.; Bandler, S.; Barret, D.; Brand, T.; Herder, J-W Den; Kiviranta, M.; Kuur, J. Van Der; hide

    2016-01-01

    In this paper we present a first assessment of the impact of various forms of instrumental crosstalk on the science performance of the X-ray Integral Field Unit (X-IFU) on the Athena X-ray mission. This assessment is made using the SIXTE end-to-end simulator in the context of one of the more technically challenging science cases for the XIFU instrument. Crosstalk considerations may influence or drive various aspects of the design of the array of high-count-rate Transition Edge Sensor (TES) detectors and its Frequency Domain Multiplexed (FDM) readout architecture. The Athena X-ray mission was selected as the second L-class mission in ESA's Cosmic Vision 2015–25 plan, with alaunch foreseen in 2028, to address the theme ''Hot and Energetic Universe"1. One of the two instruments on boardAthena is the X-ray Integral Field Unit2 (X-IFU) which is based on an array of 3800 Transition Edge Sensors (TES's)operated at a temperature of 90 mK. The science cases pose an interesting challenge for this instrument, as they requirea combination of high energy resolution (2.5 eV FWHM or better), high spatial resolution (5 arcsec or better) and highcount rate capability (several tens of counts per second per detector for point sources as bright as 10 mCrab).The performance at the single sensor level has been demonstrated3, but the operation of such detectors in an array, usingmultiplexed readout, brings additional challenges, both for the design of the array in which the sensors are placed and forthe readout of the sensors. The readout of the detector array will be based on Frequency Domain Multiplexing (FDM)4.In this system of detectors and readout, crosstalk can arise through various mechanisms: on the TES array, neighboringsensors can couple through thermal crosstalk. Detectors adjacent in carrier frequency may suffer from electrical crosstalkdue to the finite width of the bandpass filters, and shared sources of impedance in their signal lines. The signals from theindividual

  2. An astronomical observatory for Peru

    Science.gov (United States)

    del Mar, Juan Quintanilla; Sicardy, Bruno; Giraldo, Víctor Ayma; Callo, Víctor Raúl Aguilar

    2011-06-01

    Peru and France are to conclude an agreement to provide Peru with an astronomical observatory equipped with a 60-cm diameter telescope. The principal aims of this project are to establish and develop research and teaching in astronomy. Since 2004, a team of researchers from Paris Observatory has been working with the University of Cusco (UNSAAC) on the educational, technical and financial aspects of implementing this venture. During an international astronomy conference in Cusco in July 2009, the foundation stone of the future Peruvian Observatory was laid at the top of Pachatusan Mountain. UNSAAC, represented by its Rector, together with the town of Oropesa and the Cusco regional authority, undertook to make the sum of 300,000€ available to the project. An agreement between Paris Observatory and UNSAAC now enables Peruvian students to study astronomy through online teaching.

  3. Creating a global observatory for health R&D.

    Science.gov (United States)

    Terry, Robert F; Salm, José F; Nannei, Claudia; Dye, Christopher

    2014-09-12

    A global map of health R&D activity would improve the coordination of research and help to match limited resources with public health priorities, such as combating antimicrobial resistance. The challenges of R&D mapping are large because there are few standards for research classification and governance and limited capacity to report on R&D data, especially in low-income countries. Nevertheless, based on developments in semantic classification, and with better reporting of funded research though the Internet, it is now becoming feasible to create a global observatory for health R&D. Copyright © 2014, American Association for the Advancement of Science.

  4. Contamination control requirements implementation for the James Webb Space Telescope (JWST), part 2: spacecraft, sunshield, observatory, and launch

    Science.gov (United States)

    Wooldridge, Eve M.; Schweiss, Andrea; Henderson-Nelson, Kelly; Woronowicz, Michael; Patel, Jignasha; Macias, Matthew; McGregor, R. Daniel; Farmer, Greg; Schmeitzky, Olivier; Jensen, Peter; Rumler, Peter; Romero, Beatriz; Breton, Jacques

    2014-09-01

    This paper will continue from Part 1 of JWST contamination control implementation. In addition to optics, instruments, and thermal vacuum testing, JWST also requires contamination control for a spacecraft that must be vented carefully in order to maintain solar array and thermal radiator thermal properties; a tennis court-sized sunshield made with 1-2 mil Kapton™ layers that must be manufactured and maintained clean; an observatory that must be integrated, stowed and transported to South America; and a rocket that typically launches commercial payloads without contamination sensitivity. An overview of plans developed to implement contamination control for the JWST spacecraft, sunshield, observatory and launch vehicle will be presented.

  5. Changes of liquid Water content in fog at Milešovka Observatory (Czech Republic)

    Czech Academy of Sciences Publication Activity Database

    Fišák, Jaroslav

    2008-01-01

    Roč. 11, - (2008), s. 5-8 ISSN 1335-339X R&D Projects: GA AV ČR IAA3042301; GA AV ČR 1QS200420562 Institutional research plan: CEZ:AV0Z30420517 Keywords : fog * liquid water content * month changes * Observatory Milešovka * visibility Subject RIV: DG - Athmosphere Sciences, Meteorology

  6. Daily variation characteristics at polar geomagnetic observatories

    Science.gov (United States)

    Lepidi, S.; Cafarella, L.; Pietrolungo, M.; Di Mauro, D.

    2011-08-01

    This paper is based on the statistical analysis of the diurnal variation as observed at six polar geomagnetic observatories, three in the Northern and three in the Southern hemisphere. Data are for 2006, a year of low geomagnetic activity. We compared the Italian observatory Mario Zucchelli Station (TNB; corrected geomagnetic latitude: 80.0°S), the French-Italian observatory Dome C (DMC; 88.9°S), the French observatory Dumont D'Urville (DRV; 80.4°S) and the three Canadian observatories, Resolute Bay (RES; 83.0°N), Cambridge Bay (CBB; 77.0°N) and Alert (ALE, 87.2°N). The aim of this work was to highlight analogies and differences in daily variation as observed at the different observatories during low geomagnetic activity year, also considering Interplanetary Magnetic Field conditions and geomagnetic indices.

  7. Byurakan Astrophysical Observatory as Cultural Centre

    Science.gov (United States)

    Mickaelian, A. M.; Farmanyan, S. V.

    2017-07-01

    NAS RA V. Ambartsumian Byurakan Astrophysical Observatory is presented as a cultural centre for Armenia and the Armenian nation in general. Besides being scientific and educational centre, the Observatory is famous for its unique architectural ensemble, rich botanical garden and world of birds, as well as it is one of the most frequently visited sightseeing of Armenia. In recent years, the Observatory has also taken the initiative of the coordination of the Cultural Astronomy in Armenia and in this field, unites the astronomers, historians, archaeologists, ethnographers, culturologists, literary critics, linguists, art historians and other experts. Keywords: Byurakan Astrophysical Observatory, architecture, botanic garden, tourism, Cultural Astronomy.

  8. The statistics of low frequency radio interference at the Murchison Radio-astronomy Observatory

    OpenAIRE

    Sokolowski, Marcin; Wayth, Randall B.; Lewis, Morgan

    2016-01-01

    We characterize the low frequency radio-frequency interference (RFI) environment at the Murchison Radio-astronomy Observatory (MRO), the location selected for the low-frequency component of the Square Kilometre Array. Data were collected from the BIGHORNS instrument, located at the MRO, which records a contiguous bandwidth between 70 and 300 MHz, between November 2014 to March 2015 inclusive. The data were processed to identify RFI, and we describe a series of statistics in both the time and ...

  9. SEL2 servicing: increased science return via on-orbit propellant replenishment

    Science.gov (United States)

    Reed, Benjamin B.; DeWeese, Keith; Kienlen, Michael; Aranyos, Thomas; Pellegrino, Joseph; Bacon, Charles; Qureshi, Atif

    2016-07-01

    Spacecraft designers are driving observatories to the distant Sun-Earth Lagrange Point 2 (SEL2) to meet ever-increasing science requirements. The mass fraction dedicated to propellant for these observatories to reach and operate at SEL2 will be allocated with the upmost care, as it comes at the expense of optics and instrument masses. As such, these observatories could benefit from on-orbit refueling, allowing greater dry-to-wet mass ratio at launch and/or longer mission life. NASA is developing technologies, capabilities and integrated mission designs for multiple servicing applications in low Earth orbit (LEO), geosynchronous Earth orbit (GEO) and cisluner locations. Restore-L, a mission officially in formulation, will launch a free-flying robotic servicer to refuel a government-owned satellite in LEO by mid 2020. This paper will detail the results of a point design mission study to extend Restore-L servicing technologies from LEO to SEL2. This SEL2 mission would launch an autonomous, robotic servicer spacecraft equipped to extend the life of two space assets through refueling. Two space platforms were chosen to 1) drive the requirements for achieving SEL2 orbit and rendezvous with a spacecraft, and 2) to drive the requirements to translate within SEL2 to conduct a follow-on servicing mission. Two fuels, xenon and hydrazine, were selected to assess a multiple delivery system. This paper will address key mission drivers, such as servicer autonomy (necessitated due to communications latency at L2). Also discussed will be the value of adding cooperative servicing elements to the client observatories to reduce mission risk.

  10. Undergraduate Research and Education at MIT Haystack Observatory

    Science.gov (United States)

    Pratap, P.; Salah, J.

    2000-05-01

    The MIT Haystack Observatory Undergraduate Research Initiative is an NSF- funded program aimed at involving undergraduate students in active radio astronomical research. The project has two major thrusts - students get hands-on experience using a small radio telescope that has been developed at Haystack and which will be provided as a low cost kit early next year. Beta versions of this telescope are being built for a select group of institutions. The second component is a research experience with the Haystack 37-m telescope. Use of the 37-m telescope has ranged from classroom demonstrations to original research projects. The Small Radio Telescope (SRT) project consists of a 2m dish with a 1420 MHz receiver. The antenna has a two axis mount that provides full sky coverage. The telescope is intended to provide students and faculty with an introduction to radio astronomy and instrument calibration. Observations of the sun and the galactic HI line are possible with the current version of this telescope. The 37-m telescope program is aimed at providing students with a research experience that can result in publishable results. The telescope has also been used in providing students with an introduction to the scope of radio astronomical data including continuum and spectral line observations. Classroom demonstrations have also been tested with non-science majors. Extensive supporting materials for the project have been developed on the world wide web. These include a radio astronomy tutorial, hardware and software information about both telescopes and project descriptions. We also provide curriculum suggestions to aid faculty incorporate radio astronomy into their courses.

  11. Examining the Teaching of Science, and Technology and Engineering Content and Practices: An Instrument Modification Study

    Science.gov (United States)

    Love, Tyler S.; Wells, John G.; Parkes, Kelly A.

    2017-01-01

    A modified Reformed Teaching Observation Protocol (RTOP) (Piburn & Sawada, 2000) instrument was used to separately examine eight technology and engineering (T&E) educators' teaching of science, and T&E content and practices, as called for by the "Standards for Technological Literacy: Content for the Study of Technology"…

  12. KMTNET: A Network of 1.6 m Wide-Field Optical Telescopes Installed at Three Southern Observatories

    Science.gov (United States)

    Kim, Seung-Lee; Lee, Chung-Uk; Park, Byeong-Gon; Kim, Dong-Jin; Cha, Sang-Mok; Lee, Yongseok; Han, Cheongho; Chun, Moo-Young; Yuk, Insoo

    2016-02-01

    The Korea Microlensing Telescope Network (KMTNet) is a wide-field photometric system installed by the Korea Astronomy and Space Science Institute (KASI). Here, we present the overall technical specifications of the KMTNet observation system, test observation results, data transfer and image processing procedure, and finally, the KMTNet science programs. The system consists of three 1.6 m wide-field optical telescopes equipped with mosaic CCD cameras of 18k by 18k pixels. Each telescope provides a 2.0 by 2.0 square degree field of view. We have finished installing all three telescopes and cameras sequentially at the Cerro-Tololo Inter-American Observatory (CTIO) in Chile, the South African Astronomical Observatory (SAAO) in South Africa, and the Siding Spring Observatory (SSO) in Australia. This network of telescopes, which is spread over three different continents at a similar latitude of about -30 degrees, enables 24-hour continuous monitoring of targets observable in the Southern Hemisphere. The test observations showed good image quality that meets the seeing requirement of less than 1.0 arcsec in I-band. All of the observation data are transferred to the KMTNet data center at KASI via the international network communication and are processed with the KMTNet data pipeline. The primary scientific goal of the KMTNet is to discover numerous extrasolar planets toward the Galactic bulge by using the gravitational microlensing technique, especially earth-mass planets in the habitable zone. During the non-bulge season, the system is used for wide-field photometric survey science on supernovae, asteroids, and external galaxies.

  13. The Pierre Auger Observatory

    International Nuclear Information System (INIS)

    Hojvat, C.

    1997-03-01

    The Pierre Auger Observatory is an international collaboration for the detailed study of the highest energy cosmic rays. It will operate at two similar sites, one in the northern hemisphere and one in the southern hemisphere. The Observatory is designed to collect a statistically significant data set of events with energies greater than 10 19 eV and with equal exposures for the northern and southern skies

  14. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Astronomical Observatory & Theoretical Astrophysics Center, Juliane Maries Vej 30, 2100 Copenhagen ɸ, Denmark; The Royal Swedish Academy of Sciences, Stockholm Observatory, SE-13336 Saltsjöbaden, Sweden; Dept. of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, ...

  15. Time-stamp correction of magnetic observatory data acquired during unavailability of time-synchronization services

    Science.gov (United States)

    Coïsson, Pierdavide; Telali, Kader; Heumez, Benoit; Lesur, Vincent; Lalanne, Xavier; Jiang Xin, Chang

    2017-09-01

    During magnetic observatory data acquisition, the data time stamp is kept synchronized with a precise source of time. This is usually done using a GPS-controlled pulse per second (PPS) signal. For some observatories located in remote areas or where internet restrictions are enforced, only the magnetometer data are transmitted, limiting the capabilities of monitoring the acquisition operations. The magnetic observatory in Lanzhou (LZH), China, experienced an unnoticed interruption of the GPS PPS starting 7 March 2013. The data logger clock drifted slowly in time: in 6 months a lag of 27 s was accumulated. After a reboot on 2 April 2014 the drift became faster, -2 s per day, before the GPS PPS could be restored on 8 July 2014. To estimate the time lags that LZH time series had accumulated, we compared it with data from other observatories located in East Asia. A synchronization algorithm was developed. Natural sources providing synchronous events could be used as markers to obtain the time lag between the observatories. The analysis of slices of 1 h of 1 s data at arbitrary UTC allowed estimating time lags with an uncertainty of ˜ 11 s, revealing the correct trends of LZH time drift. A precise estimation of the time lag was obtained by comparing data from co-located instruments controlled by an independent PPS. In this case, it was possible to take advantage of spikes and local noise that constituted precise time markers. It was therefore possible to determine a correction to apply to LZH time stamps to correct the data files and produce reliable 1 min averaged definitive magnetic data.

  16. Challenges and Opportunities to Developing Synergies Among Diverse Environmental Observatories: FSML, NEON, and GLEON

    Science.gov (United States)

    Williamson, C. E.; Weathers, K. C.; Knoll, L. B.; Brentrup, J.

    2012-12-01

    Recent rapid advances in sensor technology and cyberinfrastructure have enabled the development of numerous environmental observatories ranging from local networks at field stations and marine laboratories (FSML) to continental scale observatories such as the National Ecological Observatory Network (NEON) to global scale observatories such as the Global Lake Ecological Observatory Network (GLEON). While divergent goals underlie the initial development of these observatories, and they are often designed to serve different communities, many opportunities for synergies exist. In addition, the use of existing infrastructure may enhance the cost-effectiveness of building and maintaining large scale observatories. For example, FSMLs are established facilities with the staff and infrastructure to host sensor nodes of larger networks. Many field stations have existing staff and long-term databases as well as smaller sensor networks that are the product of a single or small group of investigators with a unique data management system embedded in a local or regional community. These field station based facilities and data are a potentially untapped gold mine for larger continental and global scale observatories; common ecological and environmental challenges centered on understanding the impacts of changing climate, land use, and invasive species often underlie these efforts. The purpose of this talk is to stimulate a dialog on the challenges of merging efforts across these different spatial and temporal scales, as well as addressing how to develop synergies among observatory networks with divergent roots and philosophical approaches. For example, FSMLs have existing long-term databases and facilities, while NEON has sparse past data but a well-developed template and closely coordinated team working in a coherent format across a continental scale. GLEON on the other hand is a grass-roots network of experts in science, information technology, and engineering with a common goal

  17. "Designing Instrument for Science Classroom Learning Environment in Francophone Minority Settings: Accounting for Voiced Concerns among Teachers and Immigrant/Refugee Students"

    Science.gov (United States)

    Bolivar, Bathélemy

    2015-01-01

    The three-phase process "-Instrument for Minority Immigrant Science Learning Environment," an 8-scale, 32-item see Appendix I- (I_MISLE) instrument when completed by teachers provides an accurate description of existing conditions in classrooms in which immigrant and refugee students are situated. Through the completion of the instrument…

  18. An international network of magnetic observatories

    Science.gov (United States)

    Love, Jeffrey J.; Chulliat, A.

    2013-01-01

    Since its formation in the late 1980s, the International Real-Time Magnetic Observatory Network (INTERMAGNET), a voluntary consortium of geophysical institutes from around the world, has promoted the operation of magnetic observatories according to modern standards [eg. Rasson, 2007]. INTERMAGNET institutes have cooperatively developed infrastructure for data exchange and management ads well as methods for data processing and checking. INTERMAGNET institute have also helped to expand global geomagnetic monitoring capacity, most notably by assisting magnetic observatory institutes in economically developing countries by working directly with local geophysicists. Today the INTERMAGNET consortium encompasses 57 institutes from 40 countries supporting 120 observatories (see Figures 1a and 1b). INTERMAGNET data record a wide variety of time series signals related to a host of different physical processes in the Earth's interiors and in the Earth's surrounding space environment [e.g., Love, 2008]. Observatory data have always had a diverse user community, and to meet evolving demand, INTERMAGNET has recently coordinated the introduction of several new data services.

  19. The EuroSITES network: Integrating and enhancing fixed-point open ocean observatories around Europe

    Science.gov (United States)

    Lampitt, Richard S.; Larkin, Kate E.; EuroSITES Consortium

    2010-05-01

    EuroSITES is a 3 year (2008-2011) EU collaborative project (3.5MEuro) with the objective to integrate and enhance the nine existing open ocean fixed point observatories around Europe (www.eurosites.info). These observatories are primarily composed of full depth moorings and make multidisciplinary in situ observations within the water column as the European contribution to the global array OceanSITES (www.oceansites.org). In the first 18 months, all 9 observatories have been active and integration has been significant through the maintenance and enhancement of observatory hardware. Highlights include the enhancement of observatories with sensors to measure O2, pCO2, chlorophyll, and nitrate in near real-time from the upper 1000 m. In addition, some seafloor missions are also actively supported. These include seafloor platforms currently deployed in the Mediterranean, one for tsunami detection and one to monitor fluid flow related to seismic activity and slope stability. Upcoming seafloor science missions in 2010 include monitoring benthic biological communities and associated biogeochemistry as indicators of climate change in both the Northeast Atlantic and Mediterranean. EuroSITES also promotes the development of innovative sensors and samplers in order to progress capability to measure climate-relevant properties of the ocean. These include further developing current technologies for autonomous long-term monitoring of oxygen consumption in the mesopelagic, pH and mesozooplankton abundance. Many of these science missions are directly related to complementary activities in other European projects such as EPOCA, HYPOX and ESONET. In 2010 a direct collaboration including in situ field work will take place between ESONET and EuroSITES. The demonstration mission MODOO (funded by ESONET) will be implemented in 2010 at the EuroSITES PAP observatory. Field work will include deployment of a seafloor lander system with various sensors which will send data to shore in real

  20. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1-Street, Urumqi 830011, China. Department of Physics and GXU-NAOC, Centre for Astrophysics and Space Sciences, Guangxi University, Nanning 530004, China. University of Chinese Academy of Sciences, Beijing 100049 ...

  1. Investigating On-Orbit Attitude Determination Anomalies for the Solar Dynamics Observatory Mission

    Science.gov (United States)

    Vess, Melissa F.; Starin, Scott R.; Chia-Kuo, Alice Liu

    2011-01-01

    The Solar Dynamics Observatory (SDO) was launched on February 11, 2010 from Kennedy Space Center on an Atlas V launch vehicle into a geosynchronous transfer orbit. SDO carries a suite of three scientific instruments, whose observations are intended to promote a more complete understanding of the Sun and its effects on the Earth's environment. After a successful launch, separation, and initial Sun acquisition, the launch and flight operations teams dove into a commissioning campaign that included, among other things, checkout and calibration of the fine attitude sensors and checkout of the Kalman filter (KF) and the spacecraft s inertial pointing and science control modes. In addition, initial calibration of the science instruments was also accomplished. During that process of KF and controller checkout, several interesting observations were noticed and investigated. The SDO fine attitude sensors consist of one Adcole Digital Sun Sensor (DSS), two Galileo Avionica (GA) quaternion-output Star Trackers (STs), and three Kearfott Two-Axis Rate Assemblies (hereafter called inertial reference units, or IRUs). Initial checkout of the fine attitude sensors indicated that all sensors appeared to be functioning properly. Initial calibration maneuvers were planned and executed to update scale factors, drift rate biases, and alignments of the IRUs. After updating the IRU parameters, the KF was initialized and quickly reached convergence. Over the next few hours, it became apparent that there was an oscillation in the sensor residuals and the KF estimation of the IRU bias. A concentrated investigation ensued to determine the cause of the oscillations, their effect on mission requirements, and how to mitigate them. The ensuing analysis determined that the oscillations seen were, in fact, due to an oscillation in the IRU biases. The low frequencies of the oscillations passed through the KF, were well within the controller bandwidth, and therefore the spacecraft was actually

  2. Merging fluxgate and induction coil data to produce low-noise geomagnetic observatory data meeting the INTERMAGNET definitive 1 s data standard

    Science.gov (United States)

    Brunke, Heinz-Peter; Widmer-Schnidrig, Rudolf; Korte, Monika

    2017-11-01

    For frequencies above 30 mHz the instrument intrinsic noise level of typical fluxgate magnetometers used at geomagnetic observatories usually masks ambient magnetic field variations on magnetically quiet days. This is especially true for stations located at middle and low latitudes, where variations are generally smaller than at high latitudes. INTERMAGNET has set a minimum quality standard for definitive 1 s data. Natural field variations referred to as pulsations (Pc-1, Pc-2, Pi-1) fall in this band. Usually their intensity is so small that they rarely surpass the instrumental noise of fluxgate magnetometers. Moreover, high-quality magnetic field observations in the band 30 mHz-0.5 Hz contain interesting information, e.g., for the study of ionospheric electron interactions with electromagnetic ion cyclotron plasma waves. We propose a method to improve 1 Hz observatory data by merging data from the proven and tested fluxgate magnetometers currently in use with induction coil magnetometers into a single data stream. We show how measurements of both instruments can be combined without information loss or phase distortion. The result is a time series of the magnetic field vector components, combining the benefits of both instruments: long-term stability (fluxgate) and low noise at high frequencies (induction coil). This new data stream fits perfectly into the data management procedures of INTERMAGNET and meets the requirements defined in the definitive 1 s data standard. We describe the applied algorithm and validate the result by comparing power spectra of the fluxgate magnetometer output with the merged signal. Daily spectrograms from the Niemegk observatory show that the resulting data series reveal information at frequencies above 30 mHz that cannot be seen in raw fluxgate data.

  3. Instruments of Science and Citizenship: Science Education for Dutch Orphans During the Late Eighteenth Century

    Science.gov (United States)

    Roberts, Lissa L.

    2012-01-01

    One of the two most extensive instrument collections in the Netherlands during the second half of the eighteenth century—rivaling the much better known collection at the University of Leiden—belonged to an orphanage in The Hague that was specially established to mold hand-picked orphans into productive citizens. (The other was housed at the Mennonite Seminary in Amsterdam, for use in the education of its students.) The educational program at this orphanage, one of three established by the Fundatie van Renswoude, grew out of a marriage between the socially-oriented generosity of the wealthy Baroness van Renswoude and the pedagogical vision of the institute's director and head teacher—a vision that fit with the larger movement of oeconomic patriotism. Oeconomic patriotism, similar to `improvement' and oeconomic movements in other European countries and their colonies, sought to tie the investigation of nature to an improvement of society's material and moral well-being. Indeed, it was argued that these two facets of society should be viewed as inseparable from each other, distinguishing the movement from more modern conceptions of economics. While a number of the key figures in this Dutch movement also became prominent Patriots during the revolutionary period at the end of the century, fighting against the House of Orange, they did not have a monopoly on oeconomic ideas of societal improvement. This is demonstrated by the fact that an explicitly pro-Orangist society, Mathesis Scientiarum Genitrix, was organized in 1785 to teach science and mathematics to poor boys and orphans for very similar reasons: to turn them into productive and useful citizens. As was the case with the Fundatie van Renswoude, a collection of instruments was assembled to help make this possible. This story is of interest because it discusses a hitherto under-examined use to which science education was put during this period, by revealing the link between such programs and the highly

  4. Lunar Riometry: Proof-of-Concept Instrument Package

    Science.gov (United States)

    Lazio, J.; Jones, D. L.; MacDowall, R. J.; Stewart, K.; Giersch, L.; Burns, J. O.; Farrell, W. M.; Kasper, J. C.; O'Dwyer, I.; Hartman, J.

    2012-12-01

    The lunar exosphere is the exemplar of a plasma near the surface of an airless body. Exposed to both the solar and interstellar radiation fields, the lunar exosphere is mostly ionized, and enduring questions regarding its properties include its density and vertical extent, the extent of contributions from volatile outgassing from the Moon, and its behavior over time, including response to the solar wind and modification by landers. Relative ionospheric measurements (riometry) is based on the simple physical principle that electromagnetic waves cannot propagate through a partially or fully ionized medium below the plasma frequency, and riometers have been deployed on the Earth in numerous remote and hostile environments. A multi-frequency riometer on the lunar surface would be able to monitor, in situ, the vertical extent of the lunar exosphere over time. We describe a concept for a riometer implemented as a secondary science payload on future lunar landers, such as those recommended in the recent Planetary Sciences Decadal Survey report. The instrument concept is simple, consisting of an antenna implemented as a metal deposited on polyimide film and receiver. We illustrate various deployment mechanisms and performance of a prototype in increasing lunar analog conditions. While the prime mission of such a riometer would be probing the lunar exosphere, our concept would also be capable to measuring the properties of dust impactors. The Lunar University Network for Astrophysical Research consortium is funded by the NASA Lunar Science Institute to investigate concepts for astrophysical observatories on the Moon. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.

  5. Artificial intelligence for the CTA Observatory scheduler

    Science.gov (United States)

    Colomé, Josep; Colomer, Pau; Campreciós, Jordi; Coiffard, Thierry; de Oña, Emma; Pedaletti, Giovanna; Torres, Diego F.; Garcia-Piquer, Alvaro

    2014-08-01

    The Cherenkov Telescope Array (CTA) project will be the next generation ground-based very high energy gamma-ray instrument. The success of the precursor projects (i.e., HESS, MAGIC, VERITAS) motivated the construction of this large infrastructure that is included in the roadmap of the ESFRI projects since 2008. CTA is planned to start the construction phase in 2015 and will consist of two arrays of Cherenkov telescopes operated as a proposal-driven open observatory. Two sites are foreseen at the southern and northern hemispheres. The CTA observatory will handle several observation modes and will have to operate tens of telescopes with a highly efficient and reliable control. Thus, the CTA planning tool is a key element in the control layer for the optimization of the observatory time. The main purpose of the scheduler for CTA is the allocation of multiple tasks to one single array or to multiple sub-arrays of telescopes, while maximizing the scientific return of the facility and minimizing the operational costs. The scheduler considers long- and short-term varying conditions to optimize the prioritization of tasks. A short-term scheduler provides the system with the capability to adapt, in almost real-time, the selected task to the varying execution constraints (i.e., Targets of Opportunity, health or status of the system components, environment conditions). The scheduling procedure ensures that long-term planning decisions are correctly transferred to the short-term prioritization process for a suitable selection of the next task to execute on the array. In this contribution we present the constraints to CTA task scheduling that helped classifying it as a Flexible Job-Shop Problem case and finding its optimal solution based on Artificial Intelligence techniques. We describe the scheduler prototype that uses a Guarded Discrete Stochastic Neural Network (GDSN), for an easy representation of the possible long- and short-term planning solutions, and Constraint

  6. An urban observatory for quantifying phosphorus and suspended solid loads in combined natural and stormwater conveyances.

    Science.gov (United States)

    Melcher, Anthony A; Horsburgh, Jeffery S

    2017-06-01

    Water quality in urban streams and stormwater systems is highly dynamic, both spatially and temporally, and can change drastically during storm events. Infrequent grab samples commonly collected for estimating pollutant loadings are insufficient to characterize water quality in many urban water systems. In situ water quality measurements are being used as surrogates for continuous pollutant load estimates; however, relatively few studies have tested the validity of surrogate indicators in urban stormwater conveyances. In this paper, we describe an observatory aimed at demonstrating the infrastructure required for surrogate monitoring in urban water systems and for capturing the dynamic behavior of stormwater-driven pollutant loads. We describe the instrumentation of multiple, autonomous water quality and quantity monitoring sites within an urban observatory. We also describe smart and adaptive sampling procedures implemented to improve data collection for developing surrogate relationships and for capturing the temporal and spatial variability of pollutant loading events in urban watersheds. Results show that the observatory is able to capture short-duration storm events within multiple catchments and, through inter-site communication, sampling efforts can be synchronized across multiple monitoring sites.

  7. Using XML and Java for Astronomical Instrumentation Control

    Science.gov (United States)

    Ames, Troy; Koons, Lisa; Sall, Ken; Warsaw, Craig

    2000-01-01

    Traditionally, instrument command and control systems have been highly specialized, consisting mostly of custom code that is difficult to develop, maintain, and extend. Such solutions are initially very costly and are inflexible to subsequent engineering change requests, increasing software maintenance costs. Instrument description is too tightly coupled with details of implementation. NASA Goddard Space Flight Center is developing a general and highly extensible framework that applies to any kind of instrument that can be controlled by a computer. The software architecture combines the platform independent processing capabilities of Java with the power of the Extensible Markup Language (XML), a human readable and machine understandable way to describe structured data. A key aspect of the object-oriented architecture is software that is driven by an instrument description, written using the Instrument Markup Language (IML). ]ML is used to describe graphical user interfaces to control and monitor the instrument, command sets and command formats, data streams, and communication mechanisms. Although the current effort is targeted for the High-resolution Airborne Wideband Camera, a first-light instrument of the Stratospheric Observatory for Infrared Astronomy, the framework is designed to be generic and extensible so that it can be applied to any instrument.

  8. Solar Dynamics Observatory Guidance, Navigation, and Control System Overview

    Science.gov (United States)

    Morgenstern, Wendy M.; Bourkland, Kristin L.; Hsu, Oscar C.; Liu, Kuo-Chia; Mason, Paul A. C.; O'Donnell, James R., Jr.; Russo, Angela M.; Starin, Scott R.; Vess, Melissa F.

    2011-01-01

    The Solar Dynamics Observatory (SDO) was designed and built at the Goddard Space Flight Center, launched from Cape Canaveral on February 11, 2010, and reached its final geosynchronous science orbit on March 16, 2010. The purpose of SDO is to observe the Sun and continuously relay data to a dedicated ground station. SDO remains Sun-pointing throughout most of its mission for the instruments to take measurements of the Sun. The SDO attitude control system (ACS) is a single-fault tolerant design. Its fully redundant attitude sensor complement includes sixteen coarse Sun sensors (CSSs), a digital Sun sensor (DSS), three two-axis inertial reference units (IRUs), and two star trackers (STs). The ACS also makes use of the four guide telescopes included as a part of one of the science instruments. Attitude actuation is performed using four reaction wheels assemblies (RWAs) and eight thrusters, with a single main engine used to provide velocity-change thrust for orbit raising. The attitude control software has five nominal control modes, three wheel-based modes and two thruster-based modes. A wheel-based Safehold running in the attitude control electronics box improves the robustness of the system as a whole. All six modes are designed on the same basic proportional-integral-derivative attitude error structure, with more robust modes setting their integral gains to zero. This paper details the final overall design of the SDO guidance, navigation, and control (GN&C) system and how it was used in practice during SDO launch, commissioning, and nominal operations. This overview will include the ACS control modes, attitude determination and sensor calibration, the high gain antenna (HGA) calibration, and jitter mitigation operation. The Solar Dynamics Observatory mission is part of the NASA Living With a Star program, which seeks to understand the changing Sun and its effects on the Solar System, life, and society. To this end, the SDO spacecraft carries three Sun

  9. High-Speed On-Board Data Processing for Science Instruments: HOPS

    Science.gov (United States)

    Beyon, Jeffrey

    2015-01-01

    The project called High-Speed On-Board Data Processing for Science Instruments (HOPS) has been funded by NASA Earth Science Technology Office (ESTO) Advanced Information Systems Technology (AIST) program during April, 2012 â€" April, 2015. HOPS is an enabler for science missions with extremely high data processing rates. In this three-year effort of HOPS, Active Sensing of CO2 Emissions over Nights, Days, and Seasons (ASCENDS) and 3-D Winds were of interest in particular. As for ASCENDS, HOPS replaces time domain data processing with frequency domain processing while making the real-time on-board data processing possible. As for 3-D Winds, HOPS offers real-time high-resolution wind profiling with 4,096-point fast Fourier transform (FFT). HOPS is adaptable with quick turn-around time. Since HOPS offers reusable user-friendly computational elements, its FPGA IP Core can be modified for a shorter development period if the algorithm changes. The FPGA and memory bandwidth of HOPS is 20 GB/sec while the typical maximum processor-to-SDRAM bandwidth of the commercial radiation tolerant high-end processors is about 130-150 MB/sec. The inter-board communication bandwidth of HOPS is 4 GB/sec while the effective processor-to-cPCI bandwidth of commercial radiation tolerant high-end boards is about 50-75 MB/sec. Also, HOPS offers VHDL cores for the easy and efficient implementation of ASCENDS and 3-D Winds, and other similar algorithms. A general overview of the 3-year development of HOPS is the goal of this presentation.

  10. Societal need for improved understanding of climate change, anthropogenic impacts, and geo-hazard warning drive development of ocean observatories in European Seas

    NARCIS (Netherlands)

    Ruhl, H.A.; Andre, M.; Beranzoli, L.; Çagatay, M.N.; Colaço, A.; Cannat, M.; Dañobeitia, J.J.; Favali, P.; Géli, L.; Gillooly, M.; Greinert, J.; Hall, P.O.J.; Huber, R.; Karstensen, J.; Lampitt, R.S.; Larkin, K.E.; Lykousis, V.; Mienert, J.; Miranda, J.M.; Person, R.; Priede, I.G.; Puillat, I.; Thomsen, L.; Waldmann, C.

    2011-01-01

    Society's needs for a network of in situ ocean observing systems cross many areas of earth and marine science. Here we review the science themes that benefit from data supplied from ocean observatories. Understanding from existing studies is fragmented to the extent that it lacks the coherent

  11. Status of a Novel 4-Band Submm/mm Camera for the Caltech Submillimeter Observatory

    Science.gov (United States)

    Noroozian, Omid; Day, P.; Glenn, J.; Golwala, S.; Kumar, S.; LeDuc, H. G.; Mazin, B.; Nguyen, H. T.; Schlaerth, J.; Vaillancourt, J. E.; Vayonakis, A.; Zmuidzinas, J.

    2007-12-01

    Submillimeter observations are important to the understanding of galaxy formation and evolution. Determination of the spectral energy distribution in the millimeter and submillimeter regimes allows important and powerful diagnostics. To this end, we are undertaking the construction of a 4-band (750, 850, 1100, 1300 microns) 8-arcminute field of view camera for the Caltech Submillimeter Observatory. The focal plane will make use of three novel technologies: photolithographic phased array antennae, on-chip band-pass filters, and microwave kinetic inductance detectors (MKID). The phased array antenna design obviates beam-defining feed horns. On-chip band-pass filters eliminate band-defining metal-mesh filters. Together, the antennae and filters enable each spatial pixel to observe in all four bands simultaneously. MKIDs are highly multiplexable background-limited photon detectors. Readout of the MKID array will be done with software-defined radio (See poster by Max-Moerbeck et al.). This camera will provide an order-of-magnitude larger mapping speed than existing instruments and will be comparable to SCUBA 2 in terms of the detection rate for dusty sources, but complementary to SCUBA 2 in terms of wavelength coverage. We present results from an engineering run with a demonstration array, the baseline design for the science array, and the status of instrument design, construction, and testing. We anticipate the camera will be available at the CSO in 2010. This work has been supported by NASA ROSES APRA grants NNG06GG16G and NNG06GC71G, the NASA JPL Research and Technology Development Program, and the Gordon and Betty Moore Foundation.

  12. Infrared Astrophysics in the SOFIA Era - An Overview

    Science.gov (United States)

    Yorke, Harold W.

    2018-06-01

    The Stratospheric Observatory for Infrared Astronomy (SOFIA) provides the international astronomical community access to a broad range of instrumentation that covers wavelengths spanning the near to far infrared. The high spectral resolution of many of these instruments in several wavelength bands is unmatched by any existing or near future planned facility. The far infrared polarization capabilities of one of its instruments, HAWC+, is also unique. Moreover, SOFIA allows for additional instrument augmentations, as new state-of-the-art photometric, spectrometric, and polarimetric capabilities have been added and are being further improved. The fact that SOFIA provides ample mass, power, computing capabilities as well as 4K cooling eases the constraints on future instrument design, technical readiness, and the instrument build to an extent not possible for space-borne missions. We will review SOFIA's current and future planned capabilities and highlight specific science areas for which the stratospheric observatory will be able to significantly advance Origins science topics.

  13. Worldwide R&D of Virtual Observatory

    Science.gov (United States)

    Cui, C. Z.; Zhao, Y. H.

    2008-07-01

    Virtual Observatory (VO) is a data intensive online astronomical research and education environment, taking advantages of advanced information technologies to achieve seamless and uniform access to astronomical information. The concept of VO was introduced in the late 1990s to meet the challenges brought up with data avalanche in astronomy. In the paper, current status of International Virtual Observatory Alliance, technical highlights from world wide VO projects are reviewed, a brief introduction of Chinese Virtual Observatory is given.

  14. NASA's Great Observatories Celebrate the International Year of Astronomy With a National Unveiling of Spectacular Images

    Science.gov (United States)

    2009-02-01

    In 1609, Galileo first turned his telescope to the heavens and gave birth to modern astronomy. To commemorate four hundred years of exploring the universe, 2009 is designated the International Year of Astronomy. NASA's Great Observatories - the Hubble Space Telescope, Spitzer Space Telescope, and Chandra X-ray Observatory - are marking the occasion with the release of a suite of images at over 100 planetariums, museums, nature centers, and schools across the country in conjunction with Galileo's birthday on February 15. The selected sites will unveil a large 9-square-foot print of the spiral galaxy Messier 101 that combines the optical view of Hubble, the infrared view of Spitzer, and the X-ray view of Chandra into one multi-wavelength picture. "It's like using your eyes, night vision goggles, and X-ray vision all at the same time," says Dr. Hashima Hasan, lead scientist for the International Year of Astronomy at NASA Headquarters in Washington. Cas A animation Chandra X-ray Image of M101 Participating institutions also will display a matched trio of Hubble, Spitzer, and Chandra images of Messier 101. Each image shows a different wavelength view of the galaxy that illustrates not only the different science uncovered by each observatory, but also just how far astronomy has come since Galileo. Messier 101 is a face-on spiral galaxy about 22 million light-years away in the constellation Ursa Major. It is in many ways similar to, but larger than, our own Milky Way galaxy. Hubble's visible light view shows off the swirls of bright stars and glowing gas that give the galaxy its nickname the Pinwheel Galaxy. In contrast, Spitzer's infrared-light image sees into the spiral arms and reveals the glow of dust lanes where dense clouds can collapse to form new stars. Chandra's X-ray picture uncovers the high-energy features in the galaxy, such as remnants of exploded stars or matter zooming around black holes. The juxtaposition of observations from these three telescopes

  15. SOFIA: The Next Generation Airborne Observatory

    Science.gov (United States)

    Dunham, Edward; Witteborn, Fred C. (Technical Monitor)

    1995-01-01

    SOFIA, the Stratospheric Observatory For Infrared Astronomy, will carry a 2.5 meter telescope into the stratosphere on 160 7.5 hour flights per year. At stratospheric altitudes SOFIA will operate above 99% of the water vapor in the Earth's atmosphere, allowing observation of wide regions of the infrared spectrum that are totally obscured from even the best ground-based sites. Its mobility and long range will allow worldwide observation of ephemeral events such as occultations and eclipses. SOFIA will be developed jointly by NASA and DARA, the German space agency. It has been included in the President's budget request to Congress for a development start in FY96 (this October!) and enjoys strong support in Germany. This talk will cover SOFIA's scientific goals, technical characteristics, science operating plan, and political status.

  16. Ultra-high energy cosmic rays. Results and status of the Pierre Auger Observatory

    Energy Technology Data Exchange (ETDEWEB)

    Peters, Christine [III. Physikalisches Institut A, RWTH Aachen University (Germany); Collaboration: Pierre-Auger-Collaboration

    2016-07-01

    The Pierre Auger Observatory is the world's largest experiment detecting extensive air showers initiated by cosmic rays at the highest energies. An area of 3000 km{sup 2} is instrumented by 1660 water Cherenkov detector stations, and 27 fluorescence telescopes overlook the atmosphere above the surface detector array. A hybrid detection principle is achieved by utilizing information of both detectors. A major upgrade of the experiment (AugerPrime) has been decided adding a third detector type, scintillator detector stations located on the water Cherenkov tanks. Thereby, the composition sensitivity of the Pierre Auger Observatory is extended by an improved determination of the muonic shower component. Additionally, underground muon detectors (AMIGA) are deployed. The experiment has been further extended by antennas measuring the emission of radio signals from air showers (AERA). An overview about recent results and the current status of the experiment are given in this talk. Highlights are updated results, e.g. on the energy spectrum, chemical composition or proton-air cross section.

  17. ESO Advanced Data Products for the Virtual Observatory

    Science.gov (United States)

    Retzlaff, J.; Delmotte, N.; Rite, C.; Rosati, P.; Slijkhuis, R.; Vandame, B.

    2006-07-01

    Advanced Data Products, that is, completely reduced, fully characterized science-ready data sets, play a crucial role for the success of the Virtual Observatory as a whole. We report on on-going work at ESO towards the creation and publication of Advanced Data Products in compliance with present VO standards on resource metadata. The new deep NIR multi-color mosaic of the GOODS/CDF-S region is used to showcase different aspects of the entire process: data reduction employing our MVM-based reduction pipeline, calibration and data characterization procedures, standardization of metadata content, and, finally, a prospect of the scientific potential illustrated by new results on deep galaxy number counts.

  18. An integrated payload design for the Exoplanet Characterisation Observatory (EChO)

    DEFF Research Database (Denmark)

    Swinyard, Bruce; Tinetti, Giovanna; Tennyson, Jonathan

    2012-01-01

    by ESA in the context of a medium class mission within the Cosmic Vision programme for launch post 2020. The payload suite is required to provide simultaneous coverage from the visible to the mid-infrared and must be highly stable and effectively operate as a single instrument. In this paper we describe......The Exoplanet Characterisation Observatory (EChO) is a space mission dedicated to undertaking spectroscopy of transiting exoplanets over the widest wavelength range possible. It is based around a highly stable space platform with a 1.2 m class telescope. The mission is currently being studied...

  19. Latest developments of neutron scattering instrumentation at the Juelich Centre for Neutron Science

    International Nuclear Information System (INIS)

    Ioffe, Alexander

    2013-01-01

    Jülich Centre for Neutron Science (JCNS) is operating a number of world-class neutron scattering instruments situated at the most powerful and advanced neutron sources (FRM II, ILL and SNS) and is continuously undertaking significant efforts in the development and upgrades to keep this instrumentation in line with the continuously changing scientific request. These developments are mostly based upon the latest progress in neutron optics and polarized neutron techniques. For example, the low-Q limit of the suite of small angle-scattering instruments has been extended to 4·10 -5 Å -1 by the successful use of focusing optics. A new generation of correction elements for the neutron spin-echo spectrometer has allowed for the use of the full field integral available, thus pushing further the instrument resolution. A significant progress has been achieved in the developments of 3 He neutron spin filters for purposes of the wide-angle polarization analysis for off-specular reflectometry and (grazing incidence) small-angle neutron scattering, e.g. the on-beam polarization of 3 He in large cells is allowing to achieve a high neutron beam polarization without any degradation in time. The wide Q-range polarization analysis using 3 He neutron spin filters has been implemented for small-angle neutron scattering that lead to the reduction up to 100 times of the intrinsic incoherent background from non-deuterated biological molecules. Also the work on wide-angle XYZ magnetic cavities (Magic PASTIS) will be presented. (author)

  20. Early German plans for southern observatories

    Science.gov (United States)

    Wolfschmidt, G.

    2002-07-01

    As early as the 18th and 19th centuries, French and English observers were active in South Africa. Around the beginning of the 20th century, Heidelberg and Potsdam astronomers proposed a southern observatory. Then Göttingen astronomers suggested building an observatory in Windhoek for photographing the sky and measuring the solar constant. In 1910 Karl Schwarzschild (1873-1916), after a visit to observatories in the United States, pointed out the usefulness of an observatory in South West Africa, in a climate superior to that in Germany, giving German astronomers access to the southern sky. Seeing tests were begun in 1910 by Potsdam astronomers, but WW I stopped the plans. In 1928 Erwin Finlay-Freundlich (1885-1964), inspired by the Hamburg astronomer Walter Baade (1893-1960), worked out a detailed plan for a southern observatory with a reflecting telescope, spectrographs and an astrograph with an objective prism. Paul Guthnick (1879-1947), director of the Berlin observatory, in cooperation with APO Potsdam and Hamburg, made a site survey to Africa in 1929 and found the conditions in Windhoek to be ideal. Observations were started in the 1930s by Berlin and Breslau astronomers, but were stopped by WW II. In the 1950s, astronomers from Hamburg and The Netherlands renewed the discussion in the framework of European cooperation, and this led to the founding of ESO in 1963.

  1. The UTMOST: A Hybrid Digital Signal Processor Transforms the Molonglo Observatory Synthesis Telescope

    Science.gov (United States)

    Bailes, M.; Jameson, A.; Flynn, C.; Bateman, T.; Barr, E. D.; Bhandari, S.; Bunton, J. D.; Caleb, M.; Campbell-Wilson, D.; Farah, W.; Gaensler, B.; Green, A. J.; Hunstead, R. W.; Jankowski, F.; Keane, E. F.; Krishnan, V. Venkatraman; Murphy, Tara; O'Neill, M.; Osłowski, S.; Parthasarathy, A.; Ravi, V.; Rosado, P.; Temby, D.

    2017-10-01

    The Molonglo Observatory Synthesis Telescope (MOST) is an 18000 m2 radio telescope located 40 km from Canberra, Australia. Its operating band (820-851 MHz) is partly allocated to telecommunications, making radio astronomy challenging. We describe how the deployment of new digital receivers, Field Programmable Gate Array-based filterbanks, and server-class computers equipped with 43 Graphics Processing Units, has transformed the telescope into a versatile new instrument (UTMOST) for studying the radio sky on millisecond timescales. UTMOST has 10 times the bandwidth and double the field of view compared to the MOST, and voltage record and playback capability has facilitated rapid implementaton of many new observing modes, most of which operate commensally. UTMOST can simultaneously excise interference, make maps, coherently dedisperse pulsars, and perform real-time searches of coherent fan-beams for dispersed single pulses. UTMOST operates as a robotic facility, deciding how to efficiently target pulsars and how long to stay on source via real-time pulsar folding, while searching for single pulse events. Regular timing of over 300 pulsars has yielded seven pulsar glitches and three Fast Radio Bursts during commissioning. UTMOST demonstrates that if sufficient signal processing is applied to voltage streams, innovative science remains possible even in hostile radio frequency environments.

  2. One second vector and scalar magnetic measurements at the low-latitude Choutuppal (CPL) magnetic observatory

    Science.gov (United States)

    Phani Chandrasekhar, Nelapatla; Potharaju, Sai Vijay Kumar; Arora, Kusumita; Shakar Rao Kasuba, Chandra; Rakhlin, Leonid; Tymoshyn, Sergey; Merenyi, Laszlo; Chilukuri, Anusha; Bulusu, Jayashree; Khomutov, Sergey

    2017-12-01

    One second measurements of the geomagnetic field variations, which meet INTERMAGNET quality and transmission specifications, require very special conditions to be maintained at the observatories over sustained periods of time, which pose serious challenges for the operators, particularly when infrastructural and environmental conditions are far from ideal. This work presents the progressive steps, which led to the successful setup of such measurements at the new magnetic observatory of the Council of Scientific and Industrial Research (CSIR)-National Geophysical Research Institute (NGRI) in the Choutuppal (CPL) campus, Hyderabad (HYB), India. The 1 s magnetic measurements in trial mode commenced in 2015 using the newly developed observatory-grade 1 s fluxgate magnetometer, GEOMAG-02MO, from Research Centre GEOMAGNET (GM), Ukraine, and the Overhauser proton precession magnetometer, GSM-90F1, along with the data acquisition system, Magrec-4B from Mingeo, Hungary. Iterative tuning of the setup led to the generation of good quality data from 2016 onward. The processes of commissioning this setup in low-latitude conditions, with the aim of producing 1 s definitive data, and the characteristics of the data from this new instrument are presented here.

  3. One second vector and scalar magnetic measurements at the low-latitude Choutuppal (CPL magnetic observatory

    Directory of Open Access Journals (Sweden)

    N. Phani Chandrasekhar

    2017-12-01

    Full Text Available One second measurements of the geomagnetic field variations, which meet INTERMAGNET quality and transmission specifications, require very special conditions to be maintained at the observatories over sustained periods of time, which pose serious challenges for the operators, particularly when infrastructural and environmental conditions are far from ideal. This work presents the progressive steps, which led to the successful setup of such measurements at the new magnetic observatory of the Council of Scientific and Industrial Research (CSIR-National Geophysical Research Institute (NGRI in the Choutuppal (CPL campus, Hyderabad (HYB, India. The 1 s magnetic measurements in trial mode commenced in 2015 using the newly developed observatory-grade 1 s fluxgate magnetometer, GEOMAG-02MO, from Research Centre GEOMAGNET (GM, Ukraine, and the Overhauser proton precession magnetometer, GSM-90F1, along with the data acquisition system, Magrec-4B from Mingeo, Hungary. Iterative tuning of the setup led to the generation of good quality data from 2016 onward. The processes of commissioning this setup in low-latitude conditions, with the aim of producing 1 s definitive data, and the characteristics of the data from this new instrument are presented here.

  4. Climate Change Literacy across the Critical Zone Observatory Network

    Science.gov (United States)

    Moore, A.; Derry, L. A.; Zabel, I.; Duggan-Haas, D.; Ross, R. M.

    2017-12-01

    Earth's Critical Zone extends from the top of the tree canopy to the base of the groundwater lens. Thus the Critical Zone is examined as a suite of interconnected systems and study of the CZ is inherently interdisciplinary. Climate change is an important driver of CZ processes. The US Critical Zone Observatory Network comprises nine observatories and a coordinating National Office. Educational programs and materials developed at each CZO and the National Office have been collected, reviewed, and presented on-line at the CZONO (criticalzone.org/national/education-outreach/resources). Because the CZOs are designed to observe and measure a suite of common parameters on varying geological substrates and within different ecological contexts, educational resources reflect the diversity of processes represented across the network. As climate change has a network-wide impact, the fundamental building blocks of climate change literacy are key elements in many activities within the CZONO resource collection. Carbon-cycle and hydrologic cycle processes are well-represented, with emphasis on human interactions with these resources, as well as the impact of extreme events and the changing climate. Current work on the resource collection focuses on connecting individual resources to "Teach Climate Science" project and the Teacher-Friendly Guide to Climate Change (teachclimatescience.wordpress.com). The Teacher-Friendly Guide is a manual for K-12 teachers that presents both the fundamentals of climate science alongside resources for effective teaching of this controversial topic. Using the reach of the CZO network we hope to disseminate effective climate literacy resources and support to the K-12 community.

  5. Use of Statistical Estimators as Virtual Observatory Search ParametersEnabling Access to Solar and Planetary Resources through the Virtual Observatory

    Science.gov (United States)

    Merka, J.; Dolan, C. F.

    2015-12-01

    Finding and retrieving space physics data is often a complicated taskeven for publicly available data sets: Thousands of relativelysmall and many large data sets are stored in various formats and, inthe better case, accompanied by at least some documentation. VirtualHeliospheric and Magnetospheric Observatories (VHO and VMO) help researches by creating a single point of uniformdiscovery, access, and use of heliospheric (VHO) and magnetospheric(VMO) data.The VMO and VHO functionality relies on metadata expressed using theSPASE data model. This data model is developed by the SPASE WorkingGroup which is currently the only international group supporting globaldata management for Solar and Space Physics. The two Virtual Observatories(VxOs) have initiated and lead a development of a SPASE-related standardnamed SPASE Query Language for provided a standard way of submittingqueries and receiving results.The VMO and VHO use SPASE and SPASEQL for searches based on various criteria such as, for example, spatial location, time of observation, measurement type, parameter values, etc. The parameter values are represented by their statisticalestimators calculated typically over 10-minute intervals: mean, median, standard deviation, minimum, and maximum. The use of statistical estimatorsenables science driven data queries that simplify and shorten the effort tofind where and/or how often the sought phenomenon is observed, as we will present.

  6. The Ocean Observatories Initiative Data Management and QA/QC: Lessons Learned and the Path Ahead

    Science.gov (United States)

    Vardaro, M.; Belabbassi, L.; Garzio, L. M.; Knuth, F.; Smith, M. J.; Kerfoot, J.; Crowley, M. F.

    2016-02-01

    The Ocean Observatories Initiative (OOI) is a multi-decadal, NSF-funded program that will provide long-term, near real-time cabled and telemetered measurements of climate variability, ocean circulation, ecosystem dynamics, air-sea exchange, seafloor processes, and plate-scale geodynamics. The OOI platforms consist of seafloor sensors, fixed moorings, and mobile assets containing over 700 operational instruments in the Atlantic and Pacific oceans. Rutgers University operates the Cyberinfrastructure (CI) component of the OOI, which acquires, processes and distributes data to scientists, researchers, educators and the public. It will also provide observatory mission command and control, data assessment and distribution, and long-term data management. The Rutgers Data Management Team consists of a data manager and four data evaluators, who are tasked with ensuring data completeness and quality, as well as interaction with OOI users to facilitate data delivery and utility. Here we will discuss the procedures developed to guide the data team workflow, the automated QC algorithms and human-in-the-loop (HITL) annotations that are used to flag suspect data (whether due to instrument failures, biofouling, or unanticipated events), system alerts and alarms, long-term data storage and CF (Climate and Forecast) standard compliance, and the lessons learned during construction and the first several months of OOI operations.

  7. Merging fluxgate and induction coil data to produce low-noise geomagnetic observatory data meeting the INTERMAGNET definitive 1 s data standard

    Directory of Open Access Journals (Sweden)

    H.-P. Brunke

    2017-11-01

    Full Text Available For frequencies above 30 mHz the instrument intrinsic noise level of typical fluxgate magnetometers used at geomagnetic observatories usually masks ambient magnetic field variations on magnetically quiet days. This is especially true for stations located at middle and low latitudes, where variations are generally smaller than at high latitudes. INTERMAGNET has set a minimum quality standard for definitive 1 s data. Natural field variations referred to as pulsations (Pc-1, Pc-2, Pi-1 fall in this band. Usually their intensity is so small that they rarely surpass the instrumental noise of fluxgate magnetometers. Moreover, high-quality magnetic field observations in the band 30 mHz–0.5 Hz contain interesting information, e.g., for the study of ionospheric electron interactions with electromagnetic ion cyclotron plasma waves. We propose a method to improve 1 Hz observatory data by merging data from the proven and tested fluxgate magnetometers currently in use with induction coil magnetometers into a single data stream. We show how measurements of both instruments can be combined without information loss or phase distortion. The result is a time series of the magnetic field vector components, combining the benefits of both instruments: long-term stability (fluxgate and low noise at high frequencies (induction coil. This new data stream fits perfectly into the data management procedures of INTERMAGNET and meets the requirements defined in the definitive 1 s data standard. We describe the applied algorithm and validate the result by comparing power spectra of the fluxgate magnetometer output with the merged signal. Daily spectrograms from the Niemegk observatory show that the resulting data series reveal information at frequencies above 30 mHz that cannot be seen in raw fluxgate data.

  8. Earth-Affecting Solar Causes Observatory (EASCO): a mission at the Sun-Earth L5

    DEFF Research Database (Denmark)

    Gopalswamy, Nat; Davila, Joseph M.; Auchère, Frédéric

    2011-01-01

    Observatory (STEREO) missions, but these missions lacked some key measurements: STEREO did not have a magnetograph; SOHO did not have in-situ magnetometer. SOHO and other imagers such as the Solar Mass Ejection Imager (SMEI) located on the Sun-Earth line are also not well-suited to measure Earth-directed CMEs....... The Earth-Affecting Solar Causes Observatory (EASCO) is a proposed mission to be located at the Sun-Earth L5 that overcomes these deficiencies. The mission concept was recently studied at the Mission Design Laboratory (MDL), NASA Goddard Space Flight Center, to see how the mission can be implemented....... The study found that the scientific payload (seven remote-sensing and three in-situ instruments) can be readily accommodated and can be launched using an intermediate size vehicle; a hybrid propulsion system consisting of a Xenon ion thruster and hydrazine has been found to be adequate to place the payload...

  9. The UNH Earth Systems Observatory: A Regional Application in Support of GEOSS Global-Scale Objectives

    Science.gov (United States)

    Vorosmarty, C. J.; Braswell, B.; Fekete, B.; Glidden, S.; Hartmann, H.; Magill, A.; Prusevich, A.; Wollheim, W.; Blaha, D.; Justice, D.; Hurtt, G.; Jacobs, J.; Ollinger, S.; McDowell, W.; Rock, B.; Rubin, F.; Schloss, A.

    2006-12-01

    The Northeast corridor of the US is emblematic of the many changes taking place across the nation's and indeed the world's watersheds. Because ecosystem and watershed change occurs over many scales and is so multifaceted, transferring scientific knowledge to applications as diverse as remediation of local ground water pollution, setting State-wide best practices for non-point source pollution control, enforcing regional carbon sequestration treaties, or creating public/private partnerships for protecting ecosystem services requires a new generation of integrative environmental surveillance systems, information technology, and information transfer to the user community. Geographically complex ecosystem interactions justify moving toward more integrative, regionally-based management strategies to deal with issues affecting land, inland waterways, and coastal waterways. A unified perspective that considers the full continuum of processes which link atmospheric forcings, terrestrial responses, watershed exports along drainage networks, and the final delivery to the coastal zone, nearshore, and off shore waters is required to adequately support the management challenge. A recent inventory of NOAA-supported environmental surveillance systems, IT resources, new sensor technologies, and management-relevant decision support systems shows the community poised to formulate an integrated and operational picture of the environment of New England. This paper presents the conceptual framework and early products of the newly-created UNH Earth Systems Observatory. The goal of the UNH Observatory is to serve as a regionally-focused yet nationally-prominent platform for observation-based, integrative science and management of the New England/Gulf of Maine's land, air, and ocean environmental systems. Development of the UNH Observatory is being guided by the principles set forth under the Global Earth Observation System of Systems and is cast as an end-to-end prototype for GEOSS

  10. Data from the Mars Science Laboratory CheMin XRD/XRF Instrument

    Science.gov (United States)

    Vaniman, David; Blake, David; Bristow, Tom; DesMarais, David; Achilles, Cherie; Anderson, Robert; Crips, Joy; Morookian, John Michael; Spanovich, Nicole; Vasavada, Ashwin; hide

    2013-01-01

    The CheMin instrument on the Mars Science Laboratory (MSL) rover Curiosity uses a Co tube source and a CCD detector to acquire mineralogy from diffracted primary X-rays and chemical information from fluoresced X-rays. CheMin has been operating at the MSL Gale Crater field site since August 5, 2012 and has provided the first X-ray diffraction (XRD) analyses in situ on a body beyond Earth. Data from the first sample collected, the Rocknest eolian soil, identify a basaltic mineral suite, predominantly plagioclase (approx.An50), forsteritic olivine (approx.Fo58), augite and pigeonite, consistent with expectation that detrital grains on Mars would reflect widespread basaltic sources. Minor phases (each XRD. This amorphous component is attested to by a broad rise in background centered at approx.27deg 2(theta) (Co K(alpha)) and may include volcanic glass, impact glass, and poorly crystalline phases including iron oxyhydroxides; a rise at lower 2(theta) may indicate allophane or hisingerite. Constraints from phase chemistry of the crystalline components, compared with a Rocknest bulk composition from the APXS instrument on Curiosity, indicate that in sum the amorphous or poorly crystalline components are relatively Si, Al, Mg-poor and enriched in Ti, Cr, Fe, K, P, S, and Cl. All of the identified crystalline phases are volatile-free; H2O, SO2 and CO2 volatile releases from a split of this sample analyzed by the SAM instrument on Curiosity are associated with the amorphous or poorly ordered materials. The Rocknest eolian soil may be a mixture of local detritus, mostly crystalline, with a regional or global set of dominantly amorphous or poorly ordered components. The Rocknest sample was targeted by MSL for "first time analysis" to demonstrate that a loose deposit could be scooped, sieved to <150 microns, and delivered to instruments in the body of the rover. A drilled sample of sediment in outcrop is anticipated. At the time of writing this abstract, promising outcrops are

  11. Lamont-Doherty Earth Observatory Student Research Opportunities in Support of the Next Generation Science Standards

    Science.gov (United States)

    Passow, M. J.; Xu, C.; Newton, R.; Turrin, M.

    2016-12-01

    The Framework for K-12 Science and Next Generation Science Standards envision that students engage in practices that scientists use to deepen understanding of scientific ideas over time. The Lamont-Doherty Earth Observatory (LDEO) of Columbia University provides a suite of educational programs for high school students which strongly support this goal. Through summer and school year programs, LDEO offers access to vibrant, world-class research laboratories and scientists who have contributed to our understanding about the solid Earth, oceans, atmosphere, climate change, ice sheets, and more. Students become part of a research campus with state-of-the-art facilities. Programs include: A Day in the Life (collecting water variable data to construct a picture of Hudson River estuary dynamics); Rockland PLUS (experiences for students interested in planning sustainable development in their own communities); the Secondary School Field Research program (project-based research focused on biodiversity and environmental problem in New York metro area wetlands); Earth2Class (monthly Saturday workshops on a range of themes); and internships with cooperating researchers . Other examples of the scientific content include analyzing deep-sea sediments, examining rocks formed during an interglacial period 125,000 years ago to gain new insights about sea-level change, and monitoring invasive species in a nearby salt marsh. Students from NYC have their first exposure to collecting water samples, seining, and canoeing in the Hudson River, a contrast to the laboratory-based experiences ASR programs in cooperating hospitals. Students attend talks about cutting-edge investigations from Lamont scientists who are leaders in many fields, as well as advice about careers and college choices. Programs differ in length and location, but have fundamental commonalities: mentoring by early career and senior scientists, minimum scaffolding, treating data as publishable, and ensuring rigorous

  12. Scientific Workflows and the Sensor Web for Virtual Environmental Observatories

    Science.gov (United States)

    Simonis, I.; Vahed, A.

    2008-12-01

    Virtual observatories mature from their original domain and become common practice for earth observation research and policy building. The term Virtual Observatory originally came from the astronomical research community. Here, virtual observatories provide universal access to the available astronomical data archives of space and ground-based observatories. Further on, as those virtual observatories aim at integrating heterogeneous ressources provided by a number of participating organizations, the virtual observatory acts as a coordinating entity that strives for common data analysis techniques and tools based on common standards. The Sensor Web is on its way to become one of the major virtual observatories outside of the astronomical research community. Like the original observatory that consists of a number of telescopes, each observing a specific part of the wave spectrum and with a collection of astronomical instruments, the Sensor Web provides a multi-eyes perspective on the current, past, as well as future situation of our planet and its surrounding spheres. The current view of the Sensor Web is that of a single worldwide collaborative, coherent, consistent and consolidated sensor data collection, fusion and distribution system. The Sensor Web can perform as an extensive monitoring and sensing system that provides timely, comprehensive, continuous and multi-mode observations. This technology is key to monitoring and understanding our natural environment, including key areas such as climate change, biodiversity, or natural disasters on local, regional, and global scales. The Sensor Web concept has been well established with ongoing global research and deployment of Sensor Web middleware and standards and represents the foundation layer of systems like the Global Earth Observation System of Systems (GEOSS). The Sensor Web consists of a huge variety of physical and virtual sensors as well as observational data, made available on the Internet at standardized

  13. The development and validation of a two-tiered multiple-choice instrument to identify alternative conceptions in earth science

    Science.gov (United States)

    Mangione, Katherine Anna

    This study was to determine reliability and validity for a two-tiered, multiple- choice instrument designed to identify alternative conceptions in earth science. Additionally, this study sought to identify alternative conceptions in earth science held by preservice teachers, to investigate relationships between self-reported confidence scores and understanding of earth science concepts, and to describe relationships between content knowledge and alternative conceptions and planning instruction in the science classroom. Eighty-seven preservice teachers enrolled in the MAT program participated in this study. Sixty-eight participants were female, twelve were male, and seven chose not to answer. Forty-seven participants were in the elementary certification program, five were in the middle school certification program, and twenty-nine were pursuing secondary certification. Results indicate that the two-tiered, multiple-choice format can be a reliable and valid method for identifying alternative conceptions. Preservice teachers in all certification areas who participated in this study may possess common alternative conceptions previously identified in the literature. Alternative conceptions included: all rivers flow north to south, the shadow of the Earth covers the Moon causing lunar phases, the Sun is always directly overhead at noon, weather can be predicted by animal coverings, and seasons are caused by the Earth's proximity to the Sun. Statistical analyses indicated differences, however not all of them significant, among all subgroups according to gender and certification area. Generally males outperformed females and preservice teachers pursuing middle school certification had higher scores on the questionnaire followed by those obtaining secondary certification. Elementary preservice teachers scored the lowest. Additionally, self-reported scores of confidence in one's answers and understanding of the earth science concept in question were analyzed. There was a

  14. New instruments and science around SINQ. Lecture notes of the 4. summer school on neutron scattering

    International Nuclear Information System (INIS)

    Furrer, A.

    1996-01-01

    The spallation neutron source at PSI will be commissioned towards the end of this year together with a set of first generation instruments. This facility should then be available for the initial scientific work after spring next year. One of the main goals of this year's summer school for neutron scattering was therefore the preparation of the potential customers at this facility for its scientific exploitation. In order to give them the - so to speak - last finish, we have dedicated the school to the discussion of the instruments at SINQ and their scientific potential. These proceedings are divided into two parts: Part A gives a complete description of the first-generation instruments and sample environment at SINQ. For all the instruments the relevant parameters for planning experiments are listed. Part A is completed by G. Bauer's summary on experimental facilities and future developments at SINQ. Part B presents the lecture notes dealing with relevant applications of neutron based techniques in science and technology. The summary lecture by S.W. Lovesey is also included. (author) figs., tabs., refs

  15. New instruments and science around SINQ. Lecture notes of the 4. summer school on neutron scattering

    Energy Technology Data Exchange (ETDEWEB)

    Furrer, A [ed.

    1996-11-01

    The spallation neutron source at PSI will be commissioned towards the end of this year together with a set of first generation instruments. This facility should then be available for the initial scientific work after spring next year. One of the main goals of this year`s summer school for neutron scattering was therefore the preparation of the potential customers at this facility for its scientific exploitation. In order to give them the - so to speak - last finish, we have dedicated the school to the discussion of the instruments at SINQ and their scientific potential. These proceedings are divided into two parts: Part A gives a complete description of the first-generation instruments and sample environment at SINQ. For all the instruments the relevant parameters for planning experiments are listed. Part A is completed by G. Bauer`s summary on experimental facilities and future developments at SINQ. Part B presents the lecture notes dealing with relevant applications of neutron based techniques in science and technology. The summary lecture by S.W. Lovesey is also included. (author) figs., tabs., refs.

  16. Calibration and Validation of the National Ecological Observatory Network's Airborne Imaging Spectrometers

    Science.gov (United States)

    Leisso, N.

    2015-12-01

    The National Ecological Observatory Network (NEON) is being constructed by the National Science Foundation and is slated for completion in 2017. NEON is designed to collect data to improve the understanding of changes in observed ecosystems. The observatory will produce data products on a variety of spatial and temporal scales collected from individual sites strategically located across the U.S. including Alaska, Hawaii, and Puerto Rico. Data sources include standardized terrestrial, instrumental, and aquatic observation systems in addition to three airborne remote sensing observation systems installed into leased Twin Otter aircraft. The Airborne Observation Platforms (AOP) are designed to collect 3-band aerial imagery, waveform and discrete LiDAR, and high-fidelity imaging spectroscopy data over the NEON sites annually at or near peak-greenness. The NEON Imaging Spectrometer (NIS) is a Visible and Shortwave Infrared (VSWIR) sensor designed by NASA JPL for ecological applications. Spectroscopic data is collected at 5-nm intervals across the solar-reflective spectral region (380-nm to 2500-nm) in a 34-degree FOV swath. A key uncertainty driver to the derived remote sensing NEON data products is the calibration of the imaging spectrometers. In addition, the calibration and accuracy of the higher-level data product algorithms is essential to the overall NEON mission to detect changes in the collected ecosystems over the 30-year expected lifetime. The typical calibration workflow of the NIS consists of the characterizing the focal plane, spectral calibration, and radiometric calibration. Laboratory spectral calibration is based on well-defined emission lines in conjunction with a scanning monochromator to define the individual spectral response functions. The radiometric calibration is NIST traceable and transferred to the NIS with an integrating sphere calibrated through the use of transfer radiometers. The laboratory calibration is monitored and maintained through

  17. The Malaysian Robotic Solar Observatory (P29)

    Science.gov (United States)

    Othman, M.; Asillam, M. F.; Ismail, M. K. H.

    2006-11-01

    Robotic observatory with small telescopes can make significant contributions to astronomy observation. They provide an encouraging environment for astronomers to focus on data analysis and research while at the same time reducing time and cost for observation. The observatory will house the primary 50cm robotic telescope in the main dome which will be used for photometry, spectroscopy and astrometry observation activities. The secondary telescope is a robotic multi-apochromatic refractor (maximum diameter: 15 cm) which will be housed in the smaller dome. This telescope set will be used for solar observation mainly in three different wavelengths simultaneously: the Continuum, H-Alpha and Calcium K-line. The observatory is also equipped with an automated weather station, cloud & rain sensor and all-sky camera to monitor the climatic condition, sense the clouds (before raining) as well as to view real time sky view above the observatory. In conjunction with the Langkawi All-Sky Camera, the observatory website will also display images from the Malaysia - Antarctica All-Sky Camera used to monitor the sky at Scott Base Antarctica. Both all-sky images can be displayed simultaneously to show the difference between the equatorial and Antarctica skies. This paper will describe the Malaysian Robotic Observatory including the systems available and method of access by other astronomers. We will also suggest possible collaboration with other observatories in this region.

  18. Virtual observatory tools and amateur radio observations supporting scientific analysis of Jupiter radio emissions

    Science.gov (United States)

    Cecconi, Baptiste; Hess, Sebastien; Le Sidaner, Pierre; Savalle, Renaud; Stéphane, Erard; Coffre, Andrée; Thétas, Emmanuel; André, Nicolas; Génot, Vincent; Thieman, Jim; Typinski, Dave; Sky, Jim; Higgins, Chuck; Imai, Masafumi

    2016-04-01

    In the frame of the preparation of the NASA/JUNO and ESA/JUICE (Jupiter Icy Moon Explorer) missions, and the development of a planetary sciences virtual observatory (VO), we are proposing a new set of tools directed to data providers as well as users, in order to ease data sharing and discovery. We will focus on ground based planetary radio observations (thus mainly Jupiter radio emissions), trying for instance to enhance the temporal coverage of jovian decametric emission. The data service we will be using is EPN-TAP, a planetary science data access protocol developed by Europlanet-VESPA (Virtual European Solar and Planetary Access). This protocol is derived from IVOA (International Virtual Observatory Alliance) standards. The Jupiter Routine Observations from the Nancay Decameter Array are already shared on the planetary science VO using this protocol, as well as data from the Iitate Low Frquency Radio Antenna, in Japan. Amateur radio data from the RadioJOVE project is also available. The attached figure shows data from those three providers. We will first introduce the VO tools and concepts of interest for the planetary radioastronomy community. We will then present the various data formats now used for such data services, as well as their associated metadata. We will finally show various prototypical tools that make use of this shared datasets.

  19. The Australian SKA Pathfinder: First Science Results

    Science.gov (United States)

    Harvey-Smith, Lisa

    2015-08-01

    The Australian SKA Pathfinder (ASKAP) is a precursor and technology demonstrator for the Square Kilometre Array.A specialist wide-field survey instrument, ASKAP compises 36 x 12m dish antennas with a maximum separation of 6km. The array operates in the frequency range 700 - 1800 MHz and has an instantaneous bandwidth of 300 MHz. Each dish is mounted with a 'phased array feed', a radio receiver that dramatically enhances the telescope's field-of-view from 1 to 30 square degrees. ASKAP is located at the Murchison Radio-astronomy Observatory, Australia's core site for the SKA.Ten Science Survey Projects have been established by teams of more than 600 astronomers from around the world. Astronomical research topics tackled by these teams include galaxy evolution, cosmic magnetism, the history of gas in galaxies and cosmology. A program of ASKAP Early Science will commence in late 2015. The 6-antenna Boolardy Engineering Test Array (BETA) is currently being used by the commissioning team and at the time of writing has produced its first scientific discovery paper.In this talk, hear the ASKAP Project Scientist report some of the exciting new capabilities demonstrated by ASKAP and learn about the first scientific discoveries made by the commissioning and early science team.

  20. COR1 Engineering Test Unit Measurements at the Mauna Loa Solar Observatory, September 2003

    Science.gov (United States)

    Thompson, William; Reginald, Nelson; Streander, Kim

    2003-01-01

    The COR1 Engineering Test Unit (ETU), which had been previously tested at the NCAR/HAO and NRL test facilities, was modified into an instrument capable of observing the Sun. It was then taken to the Mauna Loa Solar Observatory to observe the corona. The changes made to observe the Sun were as follows: 1. The plate scale was changed to accommodate the smaller Apogee camera. This change had already been made for the NRL tests. 2. The previous Oriel polarizer was replaced with a commercial Polarcor polarizer from Newport to be more flight-like. However, because of cost and availability considerations, this polarizer was smaller than those which will be used for flight. 3. A structure was placed around the back section of the instrument, to protect it from stray light. 4. A pointing spar borrowed from HAO was used to track the Sun. A few days into the test, it became evident that some artifacts were appearing in the data, and these artifacts were changing as the polarizer was rotated. It was decided to test two other polarizers, the Oriel polarizer which had been used in the previous tests at HAO and NRL, and a Nikon polarizer which was borrowed from a camera belonging to one of the observatory staff members. These three polarizers had much different qualities are shown.

  1. International lunar observatory / power station: from Hawaii to the Moon

    Science.gov (United States)

    Durst, S.

    Astronomy's great advantages from the Moon are well known - stable surface, diffuse atmosphere, long cool nights (14 days), low gravity, far side radio frequency silence. A large variety of astronomical instruments and observations are possible - radio, optical and infrared telescopes and interferometers; interferometry for ultra- violet to sub -millimeter wavelengths and for very long baselines, including Earth- Moon VLBI; X-ray, gamma-ray, cosmic ray and neutrino detection; very low frequency radio observation; and more. Unparalleled advantages of lunar observatories for SETI, as well as for local surveillance, Earth observation, and detection of Earth approaching objects add significant utility to lunar astronomy's superlatives. At least nine major conferences in the USA since 1984 and many elsewhere, as well as ILEWG, IAF, IAA, LEDA and other organizations' astronomy-from-the-Moon research indicate a lunar observatory / power station, robotic at first, will be one of the first mission elements for a permanent lunar base. An international lunar observatory will be a transcending enterprise, highly principled, indispensable, soundly and broadly based, and far- seeing. Via Astra - From Hawaii to the Moon: The astronomy and scie nce communities, national space agencies and aerospace consortia, commercial travel and tourist enterprises and those aspiring to advance humanity's best qualities, such as Aloha, will recognize Hawaii in the 21st century as a new major support area and pan- Pacific port of embarkation to space, the Moon and beyond. Astronomical conditions and facilities on Hawaii's Mauna Kea provide experience for construction and operation of observatories on the Moon. Remote and centrally isolated, with diffuse atmosphere, sub-zero temperature and limited working mobility, the Mauna Kea complex atop the 4,206 meter summit of the largest mountain on the planet hosts the greatest collection of large astronomical telescopes on Earth. Lunar, extraterrestrial

  2. The Fram Strait integrated ocean observatory

    Science.gov (United States)

    Fahrbach, E.; Beszczynska-Möller, A.; Rettig, S.; Rohardt, G.; Sagen, H.; Sandven, S.; Hansen, E.

    2012-04-01

    A long-term oceanographic moored array has been operated since 1997 to measure the ocean water column properties and oceanic advective fluxes through Fram Strait. While the mooring line along 78°50'N is devoted to monitoring variability of the physical environment, the AWI Hausgarten observatory, located north of it, focuses on ecosystem properties and benthic biology. Under the EU DAMOCLES and ACOBAR projects, the oceanographic observatory has been extended towards the innovative integrated observing system, combining the deep ocean moorings, multipurpose acoustic system and a network of gliders. The main aim of this system is long-term environmental monitoring in Fram Strait, combining satellite data, acoustic tomography, oceanographic measurements at moorings and glider sections with high-resolution ice-ocean circulation models through data assimilation. In future perspective, a cable connection between the Hausgarten observatory and a land base on Svalbard is planned as the implementation of the ESONET Arctic node. To take advantage of the planned cabled node, different technologies for the underwater data transmission were reviewed and partially tested under the ESONET DM AOEM. The main focus was to design and evaluate available technical solutions for collecting data from different components of the Fram Strait ocean observing system, and an integration of available data streams for the optimal delivery to the future cabled node. The main components of the Fram Strait integrated observing system will be presented and the current status of available technologies for underwater data transfer will be reviewed. On the long term, an initiative of Helmholtz observatories foresees the interdisciplinary Earth-Observing-System FRAM which combines observatories such as the long term deep-sea ecological observatory HAUSGARTEN, the oceanographic Fram Strait integrated observing system and the Svalbard coastal stations maintained by the Norwegian ARCTOS network. A vision

  3. Low-frequency Radio Observatory on the Lunar Surface (LROLS)

    Science.gov (United States)

    MacDowall, Robert; Network for Exploration and Space Science (NESS)

    2018-06-01

    A radio observatory on the lunar surface will provide the capability to image solar radio bursts and other sources. Radio burst imaging will improve understanding of radio burst mechanisms, particle acceleration, and space weather. Low-frequency observations (less than ~20 MHz) must be made from space, because lower frequencies are blocked by Earth’s ionosphere. Solar radio observations do not mandate an observatory on the farside of the Moon, although such a location would permit study of less intense solar bursts because the Moon occults the terrestrial radio frequency interference. The components of the lunar radio observatory array are: the antenna system consisting of 10 – 100 antennas distributed over a square kilometer or more; the system to transfer the radio signals from the antennas to the central processing unit; electronics to digitize the signals and possibly to calculate correlations; storage for the data until it is down-linked to Earth. Such transmission requires amplification and a high-gain antenna system or possibly laser comm. For observatories on the lunar farside a satellite or other intermediate transfer system is required to direct the signal to Earth. On the ground, the aperture synthesis analysis is completed to display the radio image as a function of time. Other requirements for lunar surface systems include the power supply, utilizing solar arrays with batteries to maintain the system at adequate thermal levels during the lunar night. An alternative would be a radioisotope thermoelectric generator requiring less mass. The individual antennas might be designed with their own solar arrays and electronics to transmit data to the central processing unit, but surviving lunar night would be a challenge. Harnesses for power and data transfer from the central processing unit to the antennas are an alternative, but a harness-based system complicates deployment. The concept of placing the antennas and harnesses on rolls of polyimide and

  4. First Light from the 4.3-meter Discovery Channel Telescope At Lowell Observatory

    Science.gov (United States)

    Hall, Jeffrey C.; Levine, S.

    2013-01-01

    Seven years after groundbreaking on July 12, 2005, the 4.3-meter Discovery Channel Telescope (DCT) is now complete and into commissioning. We obtained first light images in mid 2012 with a 4K x 4K CCD and have recently obtained our first images with the DCT's main camera, the 6K x 6K Large Monolithic Imager (LMI, see adjacent poster by Massey). We held a celebratory gala on July 21, 2012, in Flagstaff. The DCT's delivered image quality is regularly subarcsecond with near-uniform image quality across the FOV from zenith to >2 airmasses, although we have not fully commissioned the active optics system. We attribute this to the outstanding quality of the mirror figures, performed by the University of Arizona's College of Optical Sciences (for M1) and L3 Brashear (for M2). The instrument cube at the RC focus can accommodate four instruments plus the LMI. Designed and built at Lowell Observatory, the cube also contains the DCT's autoguider and wavefront sensor. First light instruments include the 4000 DeVeny spectrograph (the former KPNO White Spectrograph), a low-resolution, high-throughput IR spectrograph, and a higher-resolution IR spectrograph/imager being built by Goddard Space Flight Center in collaboration with the University of Maryland. We are seeking funding for long-slit and fiber-fed echelle spectrographs for higher resolution optical spectroscopy. The DCT can also be configured to host Nasmyth and prime focus instruments. Discovery Communications and its founder John Hendricks contributed $16M to the $53M cost of the telescope, in return for naming rights and first rights to public, educational use of images in their programming. Analysis of data and publication by astronomers in professional journals follows the same procedure as for any other major telescope facility. Discovery's first DCT feature, "Scanning the Skies," aired on September 9, 2012. Future outreach plans include initiating webcasts to classrooms via the Discovery Education networks

  5. Preventing Rape of the Observatory: Thoughts on the Urgency of Preserving Historic Astronomical Artifacts

    Science.gov (United States)

    Bell, T. E.

    2005-12-01

    "What good is this century-old monster refractor? Sell it and use the money to buy a brand new go-to reflector useful for teaching students and advancing astronomy." So argues logic that is endangering an increasing number of university observatories around the U.S. (if not the rest of the world), even up to the Yerkes Observatory and its 40-inch Clark, world's largest refractor by the acknowledged world's best lens-makers. While most non-historians readily accept the value of preserving our cultural heritage in rare and precious documents (such as the Declaration of Independence), artifacts (such as Stradivarius violins), and institutions (such as the birthplaces of U.S. Presidents), they tend not to think of astronomical observatories as part of cultural heritage-with a result that history is crumbling apace to the wrecking ball. In early October, the Antique Telescope Society convened a special 60-minute session discussing philosophical why's and practical how's of preserving astronomical assets (including historically significant telescopes, observatory buildings, auxiliary equipment used to make observations or calculate results, and libraries of books and papers). This paper will summarize the discussion's key insights - including the assessing and assigning of value to old vs. new telescopes, and the roles of politics, funding and fund-raising, publicity (positive and negative), education, use as a form of preservation, innovative solutions by private collectors (including "half-way houses" for homeless instruments), restoration vs. renovation, special problems facing very large telescopes, and lessons learned from both failures and success.

  6. What's New for the Orbiting Carbon Observatory-2? A Summary of Changes between the Original and Re-flight Missions

    Science.gov (United States)

    Boland, S. W.; Kahn, P. B.

    2012-12-01

    The original Orbiting Carbon Observatory mission was lost in 2009 when the spacecraft failed to achieve orbit due to a launch vehicle failure. In 2010, NASA authorized a re-flight mission, known as the Orbiting Carbon Observatory-2 (OCO-2) mission, with direction to re-use the original hardware, designs, drawings, documents, and procedures wherever possible in order to minimize cost, schedule, and performance risk. During implementation, it was realized that some changes were required due to parts obsolescence, incorporation of lessons learned from the original OCO mission, and to provide optimal science return. In response to the OCO and Glory launch vehicle failures, a change in launch vehicle was also recently announced. A summary of changes, including those to hardware, orbit, and launch vehicle is provided, along with rationale, implementation approach, and impact (if any) on mission science.

  7. The United Nations Basic Space Science Initiative

    Science.gov (United States)

    Haubold, Hans; Balogh, Werner

    2014-05-01

    The basic space science initiative was a long-term effort for the development of astronomy and space science through regional and international cooperation in this field on a worldwide basis, particularly in developing nations. Basic space science workshops were co-sponsored and co-organized by ESA, JAXA, and NASA. A series of workshops on basic space science was held from 1991 to 2004 (India 1991, Costa Rica and Colombia 1992, Nigeria 1993, Egypt 1994, Sri Lanka 1995, Germany 1996, Honduras 1997, Jordan 1999, France 2000, Mauritius 2001, Argentina 2002, and China 2004; http://neutrino.aquaphoenix.com/un-esa/) and addressed the status of astronomy in Asia and the Pacific, Latin America and the Caribbean, Africa, and Western Asia. Through the lead of the National Astronomical Observatory Japan, astronomical telescope facilities were inaugurated in seven developing nations and planetariums were established in twenty developing nations based on the donation of respective equipment by Japan.Pursuant to resolutions of the Committee on the Peaceful Uses of Outer Space of the United Nations (COPUOS) and its Scientific and Technical Subcommittee, since 2005, these workshops focused on the preparations for and the follow-ups to the International Heliophysical Year 2007 (UAE 2005, India 2006, Japan 2007, Bulgaria 2008, South Korea 2009; www.unoosa.org/oosa/SAP/bss/ihy2007/index.html). IHY's legacy is the current operation of 16 worldwide instrument arrays with more than 1000 instruments recording data on solar-terrestrial interaction from coronal mass ejections to variations of the total electron content in the ionosphere (http://iswisecretariat.org/). Instruments are provided to hosting institutions by entities of Armenia, Brazil, France, Israel, Japan, Switzerland, and the United States. Starting in 2010, the workshops focused on the International Space Weather Initiative (ISWI) as mandated in a three-year-work plan as part of the deliberations of COPUOS. Workshops on ISWI

  8. 195-Year History of Mykolayiv Observatory: Events and People

    Directory of Open Access Journals (Sweden)

    Shulga, O.V.

    2017-01-01

    Full Text Available The basic stages of the history of the Mykolaiv Astronomical Observatory are shown. The main results of the Observatory activities are presented by the catalogs of star positions, major and minor planets in the Solar system, space objects in the Earth orbit. The information on the qualitative and quantitative structure of the Observatory, cooperation with the observatories of Ukraine and foreign countries as well as major projects carried out in the Observatory is provided.

  9. The integrated water balance and soil data set of the Rollesbroich hydrological observatory

    Science.gov (United States)

    Qu, Wei; Bogena, Heye R.; Huisman, Johan A.; Schmidt, Marius; Kunkel, Ralf; Weuthen, Ansgar; Schiedung, Henning; Schilling, Bernd; Sorg, Jürgen; Vereecken, Harry

    2016-10-01

    The Rollesbroich headwater catchment located in western Germany is a densely instrumented hydrological observatory and part of the TERENO (Terrestrial Environmental Observatories) initiative. The measurements acquired in this observatory present a comprehensive data set that contains key hydrological fluxes in addition to important hydrological states and properties. Meteorological data (i.e., precipitation, air temperature, air humidity, radiation components, and wind speed) are continuously recorded and actual evapotranspiration is measured using the eddy covariance technique. Runoff is measured at the catchment outlet with a gauging station. In addition, spatiotemporal variations in soil water content and temperature are measured at high resolution with a wireless sensor network (SoilNet). Soil physical properties were determined using standard laboratory procedures from samples taken at a large number of locations in the catchment. This comprehensive data set can be used to validate remote sensing retrievals and hydrological models, to improve the understanding of spatial temporal dynamics of soil water content, to optimize data assimilation and inverse techniques for hydrological models, and to develop upscaling and downscaling procedures of soil water content information. The complete data set is freely available online (http://www.tereno.net, doi:10.5880/TERENO.2016.001, doi:10.5880/TERENO.2016.004, doi:10.5880/TERENO.2016.003) and additionally referenced by three persistent identifiers securing the long-term data and metadata availability.

  10. On the feasibility of routine baseline improvement in processing of geomagnetic observatory data

    Science.gov (United States)

    Soloviev, Anatoly; Lesur, Vincent; Kudin, Dmitry

    2018-02-01

    We propose a new approach to the calculation of regular baselines at magnetic observatories. The proposed approach is based on the simultaneous analysis of the irregular absolute observations and the continuous time-series deltaF, widely used for estimating the data quality. The systematic deltaF analysis allows to take into account all available information about the operation of observatory instruments (i.e., continuous records of the field variations and its modulus) in the intervals between the times of absolute observations, as compared to the traditional baseline calculation where only spot values are considered. To establish a connection with the observed spot baseline values, we introduce a function for approximate evaluation of the intermediate baseline values. An important feature of the algorithm is its quantitative estimation of the resulting data precision and thus determination of the problematic fragments in raw data. We analyze the robustness of the algorithm operation using synthetic data sets. We also compare baselines and definitive data derived by the proposed algorithm with those derived by the traditional approach using Saint Petersburg observatory data, recorded in 2015 and accepted by INTERMAGNET. It is shown that the proposed method allows to essentially improve the resulting data quality when baseline data are not good enough. The obtained results prove that the baseline variability in time might be quite rapid.[Figure not available: see fulltext.

  11. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Development of a Low-order Adaptive Optics System at Udaipur Solar Observatory ... A low-order Adaptive Optics (AO) system is being developed at the Udaipur Solar Observatory and we present in this paper the status of the project, which includes ... Articles are also visible in Web of Science immediately.

  12. Characteristics of the telescope for high energy gamma-ray astronomy selected for definition studies on the Gamma Ray Observatory

    Science.gov (United States)

    Hughes, E. B.; Hofstadter, R.; Rolfe, J.; Johansson, A.; Bertsch, D. L.; Cruickshank, W. J.; Ehrmann, C. H.; Fichtel, C. E.; Hartman, R. C.; Kniffen, D. A.

    1980-01-01

    The high energy gamma-ray telescope selected for definition studies on the Gamma Ray Observatory provides a substantial improvement in observational capability over earlier instruments. It will have about 20 times more sensitivity, cover a much broader energy range, have considerably better energy resolution and provide a significantly improved angular resolution. The design and performance are described.

  13. WFIRST Project Science Activities

    Science.gov (United States)

    Gehrels, Neil

    2012-01-01

    The WFIRST Project is a joint effort between GSFC and JPL. The project scientists and engineers are working with the community Science Definition Team to define the requirements and initial design of the mission. The objective is to design an observatory that meets the WFIRST science goals of the Astr02010 Decadal Survey for minimum cost. This talk will be a report of recent project activities including requirements flowdown, detector array development, science simulations, mission costing and science outreach. Details of the interim mission design relevant to scientific capabilities will be presented.

  14. International Lunar Observatory Association Advancing 21st Century Astronomy from the Moon

    Science.gov (United States)

    Durst, Steve

    2015-08-01

    Long considered a prime location to conduct astronomical observations, the Moon is beginning to prove its value in 21st Century astronomy through the Lunar Ultraviolet Telescope aboard China’s Chang’e-3 Moon lander and through the developing missions of the International Lunar Observatory Association (ILOA). With 24 hours / Earth day of potential operability facilitating long-duration observations, the stable platform of the lunar surface and extremely thin exosphere guaranteeing superior observation conditions, zones of radio-quiet for radio astronomy, and the resources and thermal stability at the lunar South Pole, the Moon provides several pioneering advantages for astronomy. ILOA, through MOUs with NAOC and CNSA, has been collaborating with China to make historic Galaxy observations with the Chang’e-3 LUT, including imaging Galaxy M101 in December 2014. LUT has an aperture of 150mm, covers a wavelength range of 245 to 340 nanometers and is capable of detecting objects at a brightness down to 14 mag. The success of China’s mission has provided support and momentum for ILOA’s mission to place a 2-meter dish, multifunctional observatory at the South Pole of the Moon NET 2017. ILOA also has plans to send a precursor observatory instrument (ILO-X) on the inaugural mission of GLXP contestant Moon Express. Advancing astronomy and astrophysics from the Moon through public-private and International partnerships will provide many valuable research opportunities while also helping to secure humanity’s position as multi world species.

  15. MMS Observatory Thermal Vacuum Results Contamination Summary

    Science.gov (United States)

    Rosecrans, Glenn P.; Errigo, Therese; Brieda, Lubos

    2014-01-01

    The MMS mission is a constellation of 4 observatories designed to investigate the fundamental plasma physics of reconnection in the Earths magnetosphere. Each spacecraft has undergone extensive environmental testing to prepare it for its minimum 2 year mission. The various instrument suites measure electric and magnetic fields, energetic particles, and plasma composition. Thermal vacuum testing was conducted at the Naval Research Laboratory (NRL) in their Big Blue vacuum chamber. The individual spacecraft were tested and enclosed in a cryopanel enclosure called a Hamster cage. Specific contamination control validations were actively monitored by several QCMs, a facility RGA, and at times, with 16 Ion Gauges. Each spacecraft underwent a bakeout phase, followed by 4 thermal cycles. Unique aspects of the TV environment included slow pump downs with represses, thruster firings, Helium identification, and monitoring pressure spikes with Ion gauges. Various data from these TV tests will be shown along with lessons learned.

  16. Seismic isolation of Advanced LIGO: Review of strategy, instrumentation and performance

    International Nuclear Information System (INIS)

    Matichard, F; Mittleman, R; Mason, K; Biscans, S; Barnum, S; Evans, M; Foley, S; Lantz, B; Celerier, C; Clark, D; DeBra, D; Kissel, J; Allwine, E; Abbott, B; Abbott, R; Abbott, S; Coyne, D; McIver, J; Birch, J; DeRosa, R

    2015-01-01

    The new generation of gravitational waves detectors require unprecedented levels of isolation from seismic noise. This article reviews the seismic isolation strategy and instrumentation developed for the Advanced LIGO observatories. It summarizes over a decade of research on active inertial isolation and shows the performance recently achieved at the Advanced LIGO observatories. The paper emphasizes the scientific and technical challenges of this endeavor and how they have been addressed. An overview of the isolation strategy is given. It combines multiple layers of passive and active inertial isolation to provide suitable rejection of seismic noise at all frequencies. A detailed presentation of the three active platforms that have been developed is given. They are the hydraulic pre-isolator, the single-stage internal isolator and the two-stage internal isolator. The architecture, instrumentation, control scheme and isolation results are presented for each of the three systems. Results show that the seismic isolation sub-system meets Advanced LIGO’s stringent requirements and robustly supports the operation of the two detectors. (paper)

  17. Pollutant Concentrations in the Rime and Fog Water at the Milesovka Observatory

    Czech Academy of Sciences Publication Activity Database

    Fišák, Jaroslav; Tesař, Miroslav; Fottová, D.

    2009-01-01

    Roč. 196, 1-4 (2009), s. 273-285 ISSN 0049-6979 R&D Projects: GA AV ČR IAA3042301; GA AV ČR 1QS200420562 Institutional research plan: CEZ:AV0Z30420517; CEZ:AV0Z20600510 Keywords : Deposited precipitation * Fog collection * Fog water * Milesovka observatory * Rime water Subject RIV: DG - Athmosphere Sciences, Meteorology Impact factor: 1.676, year: 2009 http://springerlink.metapress.com/content/18q3lr7681736qp2/fulltext.pdf

  18. Early German Plans for a Southern Observatory

    Science.gov (United States)

    Wolfschmidt, Gudrun

    As early as the 18th and 19th centuries, French and English observers were active in South Africa. Around the beginning of the 20th century the Heidelberg astronomer Max Wolf (1863-1932) proposed a southern observatory. In 1907 Hermann Carl Vogel (1841-1907), director of the Astrophysical Observatory Potsdam, suggested a southern station in Spain. His ideas for building an observatory in Windhuk for photographing the sky and measuring the solar constant were taken over by the Göttingen astronomers. In 1910 Karl Schwarzschild (1873-1916), after having visited the observatories in America, pointed out the usefulness of an observatory in South West Africa, where it would have better weather than in Germany and also give access to the southern sky. Seeing tests were begun in 1910 by Potsdam astronomers, but WW I stopped the plans. In 1928 Erwin Finlay-Freundlich (1885-1964), inspired by the Hamburg astronomer Walter Baade (1893-1960), worked out a detailed plan for a southern observatory with a reflecting telescope, spectrographs and an astrograph with an objective prism. Paul Guthnick (1879-1947), director of the Berlin observatory, in cooperation with APO Potsdam and Hamburg, made a site survey to Africa in 1929 and found the conditions in Windhuk to be ideal. Observations were started in the 1930s by Berlin and Breslau astronomers, but were stopped by WW II. In the 1950s, astronomers from Hamburg and The Netherlands renewed the discussion in the framework of European cooperation, and this led to the founding of ESO in 1963, as is well described by Blaauw (1991). Blaauw, Adriaan: ESO's Early History. The European Southern Observatory from Concept to Reality. Garching bei München: ESO 1991.

  19. A Green Robotic Observatory for Astronomy Education

    Science.gov (United States)

    Reddy, Vishnu; Archer, K.

    2008-09-01

    With the development of robotic telescopes and stable remote observing software, it is currently possible for a small institution to have an affordable astronomical facility for astronomy education. However, a faculty member has to deal with the light pollution (observatory location on campus), its nightly operations and regular maintenance apart from his day time teaching and research responsibilities. While building an observatory at a remote location is a solution, the cost of constructing and operating such a facility, not to mention the environmental impact, are beyond the reach of most institutions. In an effort to resolve these issues we have developed a robotic remote observatory that can be operated via the internet from anywhere in the world, has a zero operating carbon footprint and minimum impact on the local environment. The prototype observatory is a clam-shell design that houses an 8-inch telescope with a SBIG ST-10 CCD detector. The brain of the observatory is a low draw 12-volt harsh duty computer that runs the dome, telescope, CCD camera, focuser, and weather monitoring. All equipment runs of a 12-volt AGM-style battery that has low lead content and hence more environmental-friendly to dispose. The total power of 12-14 amp/hrs is generated from a set of solar panels that are large enough to maintain a full battery charge for several cloudy days. This completely eliminates the need for a local power grid for operations. Internet access is accomplished via a high-speed cell phone broadband connection or satellite link eliminating the need for a phone network. An independent observatory monitoring system interfaces with the observatory computer during operation. The observatory converts to a trailer for transportation to the site and is converted to a semi-permanent building without wheels and towing equipment. This ensures minimal disturbance to local environment.

  20. On DESTINY Science Instrument Electrical and Electronics Subsystem Framework

    Science.gov (United States)

    Kizhner, Semion; Benford, Dominic J.; Lauer, Tod R.

    2009-01-01

    Future space missions are going to require large focal planes with many sensing arrays and hundreds of millions of pixels all read out at high data rates'' . This will place unique demands on the electrical and electronics (EE) subsystem design and it will be critically important to have high technology readiness level (TRL) EE concepts ready to support such missions. One such omission is the Joint Dark Energy Mission (JDEM) charged with making precise measurements of the expansion rate of the universe to reveal vital clues about the nature of dark energy - a hypothetical form of energy that permeates all of space and tends to increase the rate of the expansion. One of three JDEM concept studies - the Dark Energy Space Telescope (DESTINY) was conducted in 2008 at the NASA's Goddard Space Flight Center (GSFC) in Greenbelt, Maryland. This paper presents the EE subsystem framework, which evolved from the DESTINY science instrument study. It describes the main challenges and implementation concepts related to the design of an EE subsystem featuring multiple focal planes populated with dozens of large arrays and millions of pixels. The focal planes are passively cooled to cryogenic temperatures (below 140 K). The sensor mosaic is controlled by a large number of Readout Integrated Circuits and Application Specific Integrated Circuits - the ROICs/ASICs in near proximity to their sensor focal planes. The ASICs, in turn, are serviced by a set of "warm" EE subsystem boxes performing Field Programmable Gate Array (FPGA) based digital signal processing (DSP) computations of complex algorithms, such as sampling-up-the-ramp algorithm (SUTR), over large volumes of fast data streams. The SUTR boxes are supported by the Instrument Control/Command and Data Handling box (ICDH Primary and Backup boxes) for lossless data compression, command and low volume telemetry handling, power conversion and for communications with the spacecraft. The paper outlines how the JDEM DESTINY concept