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Sample records for astrographs

  1. DOUBLE STARS IN THE USNO CCD ASTROGRAPHIC CATALOG

    Energy Technology Data Exchange (ETDEWEB)

    Hartkopf, William I.; Mason, Brian D.; Finch, Charlie T.; Zacharias, Norbert; Wycoff, Gary L.; Hsu, Danley, E-mail: wih@usno.navy.mil, E-mail: bdm@usno.navy.mil, E-mail: finch@usno.navy.mil, E-mail: nz@usno.navy.mil [US Naval Observatory, Washington, DC 20392 (United States)

    2013-10-01

    The newly completed Fourth USNO CCD Astrographic Catalog (UCAC4) has proven to be a rich source of double star astrometry and photometry. Following initial comparisons of UCAC4 results against those obtained by speckle interferometry, the UCAC4 catalog was matched against known double stars in the Washington Double Star Catalog in order to provide additional differential astrometry and photometry for these pairs. Matches to 58,131 pairs yielded 61,895 astrometric and 68,935 photometric measurements. Finally, a search for possible new common proper motion (CPM) pairs was made using new UCAC4 proper motion data; this resulted in 4755 new potential CPM doubles (and an additional 27,718 astrometric and photometric measures from UCAC and other sources)

  2. Time Resolved Precision Differential Photometry with OAFA's Double Astrograph

    Science.gov (United States)

    González, E. P. A.; Podestá, F.; Podestá, R.; Pacheco, A. M.

    2018-01-01

    For the last 50 years, the Double Astrograph located at the Carlos U. Cesco station of the Observatorio Astronómico Félix Aguilar (OAFA), San Juan province, Argentina, was used for astrometric observations and research. The main programs involved the study of asteroid positions and proper motions of stars in the Southern hemisphere, being the latter a long time project that is near completion from which the SPM4 catalog is the most recent version (Girard et al. 2011). In this paper, new scientific applications in the field of photometry that can be accomplished with this telescope are presented. These first attempts show the potential of the instrument for such tasks.

  3. VizieR Online Data Catalog: FON Astrographic Catalogue, Version 3.0 (Andruk+, 2016)

    Science.gov (United States)

    Andruk, V. M.; Pakuliak, L. K.; Golovnia, V. V.; Ivanov, G. O.; Yatsenko, A. I.; Shatokhina, S. V.; Yizhakevych, O. M.

    2017-11-01

    A catalog of positions and B-magnitudes of 19 million objects (FONAC V3.0) is presented. The catalog is a result of digitizing, image processing, and reduction of 2260 photographic plates of FON observational project from MAO NAS of Ukraine glass archive, which is the part of the UkrVO national project. (94 data files).

  4. The StarScan Plate Measuring Machine: Overview and Calibrations

    National Research Council Canada - National Science Library

    Zacharias, N; Winter, L; Holdenried, E. R; De Cuyper, J. P; Rafferty, T. J; Wycoff, G. L

    2008-01-01

    ...) plates, and 300 Lick Astrograph plates have been measured. StarScan comprises a CCD camera, a telecentric lens, an air-bearing granite table, stepper motor screws, and Heidenhain scales to operate in a step-stare mode...

  5. The First U.S. Naval Observatory Robotic Astrometric Telescope Catalog

    Science.gov (United States)

    2015-10-01

    as the next step beyond the successful USNO CCD Astrograph Catalog (UCAC) project (Zacharias et al. 2013), providing accurate reference star positions...goals: first , to establish a highly accurate, dense, deep optical reference frame at current epochs; and second, to identify nearby stars without

  6. The Hipparcos, Tycho, TRC, and ACT catalogues - A whole sky comparison of the proper motions

    NARCIS (Netherlands)

    Hoogerwerf, R; Blaauw, A

    We present a whole sky comparison of the proper motions contained in the Hipparcos Catalogue, the Tycho Catalogue, the Tycho Reference Catalogue (TRC), and the Astro-graphic Catalogue plus Tycho Reference Catalogue (ACT). The catalogues are compared in the 20 declination zones defined by the

  7. Effect on the Reference Catalog System on the Asteroid Positions in the MPC Database

    Directory of Open Access Journals (Sweden)

    Maigurova, N.V.

    2017-01-01

    Full Text Available The results of analysis of the selected MPC asteroid positions are presented. Systematic errors in star positions, arising through the use of different reference catalogs, and astrometric weighting problems are discussed using observations of the 12 selected asteroids. The observational series for these asteroids include 30-year period obtained with Mykolaiv Zone Astrograph during 1960-1990. The analysis of the residuals (O-CRА,Dec of the selected asteroids has been performed.

  8. Systematic error corrections for UCAC2 positions

    Science.gov (United States)

    Zacharias, N.; Zacharias, M. I.

    2002-09-01

    The U.S. Naval Observatory (USNO) CCD Astrograph Catalog (UCAC) project begun observing from the Northern Hemisphere in November 2001, continuing the project started at CTIO in 1998. A catalog (UCAC2) of positions and proper motions for about 40 million stars (8 to 16 mag) is being constructed, covering the sky from the South Celestial Pole to about +30 degree declination. For the first time, the large number of available calibration observations are being utilized to significantly improve the systematic error corrections, beyond what has been achieved with the UCAC1 release. Due to the poor charge transfer efficiency of the 4k by 4k chip, systematic errors exist in the raw data mainly as a function of magnitude and x-coordinate, in various combinations. Important in the determination of these systematic errors is 1) the ability of the astrograph to operate on both sides of the pier, allowing frames to be taken which are flipped by 180o in orientation with respect to the sky; and 2) the stability of the instrument, giving repeatable results over years of operation. Other types of systematic errors and the expected positional accuracy of the upcoming UCAC2 will also be discussed.

  9. 166th Symposium of the International Astronomical Union

    CERN Document Server

    Seidelmann, P

    1995-01-01

    Astrometry is on the threshold of great changes due to the fact that this decade, alone, is witnessing an improvement of stellar positions equivalent to the total improvement of the previous two centuries. The Hipparcos Satellite has concluded its observations, and the catalog is in preparation. Preliminary results assure that the Hipparcos catalog will provide positions, parallaxes and annual proper motions for over 100,000 stars with accuracies of 1.5 milliarcseconds. In addition, the Tycho catalog will provide positions of about 30 milliarcseconds accuracy for over 1 million stars, and annual proper motions with 3 milliarcsecond accuracy will subsequently be ob­ tained by means of first epoch positions from the Astrographic Catalog. Optical interferometers on the ground are beginning operation, and these instruments can provide observational accuracies of approximately one milliarcsecond. Also, the traditional reference frame based on the Fun­ damental Catalog of bright stars is being replaced by the ext...

  10. Search for planet X

    Science.gov (United States)

    Harrington, Robert S.

    1991-01-01

    The observation of the region of the sky in which it is believed Planet X should now be, based on perturbations observed in the motions of Uranus and Neptune, was determined, and there was no reason to update that determination. A limited area of that region was photographed, and that will be continued. A given area is photographed with the twin 20 cm astrograph in New Zealand on two successive nights near the time that area is in opposition, and these plates are blinked in Washington to identify anything that has moved. The predicted region is in the south, which requires observations from a southern station, and it is in opposition in the April to June period, which means observations have not yet started for the year. Blinking will be done as soon as the plates are received in Washington.

  11. Puesta en marcha de un microdensitómetro automático basado en CCD

    Science.gov (United States)

    Calderón, J. H.; Bustos Fierro, I. H.

    We present the commisioning of a CCD-based microdensitometer intended to perform astrometric measurements of photographic plates. The work done consisted in the installation of a CCD camera, the modification of the motion system, the construction of a new illumination device, the adaptation of the electronics, and the development of software. The instrument is intended to be used for the astrometric measurement mainly of plates of the Astrographic Catalog and Carte du Ciel collections from Córdoba Observatory. In this phase of the project we counted with the collaboration of the Instituto Provincial de Enseñanza Media No 59, 25 de Mayo, Cruz Alta (Province of Córdoba). The origin and importance of such collaboration is commented.

  12. VizieR Online Data Catalog: MOST photometry of Proxima (Kipping+, 2017)

    Science.gov (United States)

    Kipping, D. M.; Cameron, C.; Hartman, J. D.; Davenport, J. R. A.; Matthews, J. M.; Sasselov, D.; Rowe, J.; Siverd, R. J.; Chen, J.; Sandford, E.; Bakos, G. A.; Jordan, A.; Bayliss, D.; Henning, T.; Mancini, L.; Penev, K.; Csubry, Z.; Bhatti, W.; da Silva Bento, J.; Guenther, D. B.; Kuschnig, R.; Moffat, A. F. J.; Rucinski, S. M.; Weiss, W. W.

    2017-06-01

    Microwave and Oscillations of STars (MOST) telescope is a 53kg satellite in low Earth orbit with a 15cm aperture visible band camera (35-750nm). MOST observed Proxima Centauri in 2014 May (beginning on HJD(2000) 2456793.18) for about 12.5 days. MOST again observed Proxima Centauri in 2015 May (starting on HJD(2000) 2457148.54), this time for a total of 31 days. Independent of the MOST observations, Proxima Cen was also monitored by the HATSouth ground-based telescope network. The network consists of six wide-field photometric instruments located at three observatories in the Southern Hemisphere (Las Campanas Observatory [LCO] in Chile, the High Energy Stereoscopic System [HESS] site in Namibia, and Siding Spring Observatory [SSO] in Australia), with two instruments per site. Each instrument consists of four 18cm diameter astrographs and associated 4K*4K backside-illuminated CCD cameras and Sloan r-band filters, placed on a common robotic mount. The four astrographs and cameras together cover a 8.2°*8.2° mosaic field of view at a pixel scale of 3.7''/pixel. Observations of a field containing Proxima Cen were collected as part of the general HATSouth transit survey, with a total of 11071 (this number does not count observations that were rejected as not useful for high-precision photometry, or those that produced large-amplitude outliers in the Proxima Cen light curve) composite 3*80s exposures gathered between 2012 June 14 and 2014 September 20. These include 3430 observations made with the HS-2 unit at LCO, 4630 observations made with the HS-4 unit at the HESS site, and 3011 observations made with the HS-6 unit at the SSO site. Due to weather and other factors, the cadence was nonuniform. The median time difference between consecutive observations in the full time series is 368s. (2 data files).

  13. Astrometric observations of planetary satellites at the Abastumani Astrophysical Observatory

    Science.gov (United States)

    Kiseleva, T. P.; Chanturiya, S. M.; Vasil'eva, T. A.; Kalinichenko, O. A.

    2012-11-01

    We present and discuss the results of the astrometry project during which we observed the satellites of Mars, Jupiter, Saturn, Uranus, and Neptune at the Abastumani Astrophysical Observatory (Georgia) between 1983 and 1994. Observations at the Abastumani Observatory were performed with the double Zeiss astrograph (DZA: D/ F = 400/3024 mm) and AZT-11 telescope ( F = 16 m). We processed a large array of observations and determined exact coordinates of the planets and their satellites in a system of reference stars of modern catalogues as well as relative coordinates of the satellites. The results were compared with modern ephemerides using the MULTI-SAT software. The comparison enabled us to estimate the accuracy of observations (their random and systematic uncertainties) and the accuracy of modern theories of the motion of planets and their satellites. Random uncertainties of observations are estimated to be 0.10″-0.40″ for various objects and observational conditions. Observational results obtained for Uranus, Neptune and the satellites Titania and Oberon were shown to deviate appreciably and systematically from theories of their motion. The results of observations are presented in the Pulkovo database for Solar System bodies that is available at the website http://www.puldb.ru.

  14. PIRATE: A Remotely Operable Telescope Facility for Research and Education

    Science.gov (United States)

    Holmes, S.; Kolb, U.; Haswell, C. A.; Burwitz, V.; Lucas, R. J.; Rodriguez, J.; Rolfe, S. M.; Rostron, J.; Barker, J.

    2011-10-01

    We introduce PIRATE, a new remotely operable telescope facility for use in research and education, constructed from off-the-shelf hardware, operated by The Open University. We focus on the PIRATE Mark 1 operational phase, in which PIRATE was equipped with a widely used 0.35 m Schmidt-Cassegrain system (now replaced with a 0.425 m corrected Dall-Kirkham astrograph). Situated at the Observatori Astronòmic de Mallorca, PIRATE is currently used to follow up potential transiting extrasolar planet candidates produced by the SuperWASP North experiment, as well as to hunt for novae in M31 and other nearby galaxies. It is operated by a mixture of commercially available software and proprietary software developed at the Open University. We discuss problems associated with performing precision time-series photometry when using a German Equatorial Mount, investigating the overall performance of such off-the-shelf solutions in both research and teaching applications. We conclude that PIRATE is a cost-effective research facility, and it also provides exciting prospects for undergraduate astronomy. PIRATE has broken new ground in offering practical astronomy education to distance-learning students in their own homes.

  15. A multimembership catalogue for 1876 open clusters using UCAC4 data

    Science.gov (United States)

    Sampedro, L.; Dias, W. S.; Alfaro, E. J.; Monteiro, H.; Molino, A.

    2017-10-01

    The main objective of this work is to determine the cluster members of 1876 open clusters, using positions and proper motions of the astrometric fourth United States Naval Observatory (USNO) CCD Astrograph Catalog (UCAC4). For this purpose, we apply three different methods, all based on a Bayesian approach, but with different formulations: a purely parametric method, another completely non-parametric algorithm and a third, recently developed by Sampedro & Alfaro, using both formulations at different steps of the whole process. The first and second statistical moments of the members' phase-space subspace, obtained after applying the three methods, are compared for every cluster. Although, on average, the three methods yield similar results, there are also specific differences between them, as well as for some particular clusters. The comparison with other published catalogues shows good agreement. We have also estimated, for the first time, the mean proper motion for a sample of 18 clusters. The results are organized in a single catalogue formed by two main files, one with the most relevant information for each cluster, partially including that in UCAC4, and the other showing the individual membership probabilities for each star in the cluster area. The final catalogue, with an interface design that enables an easy interaction with the user, is available in electronic format at the Stellar Systems Group (SSG-IAA) web site (http://ssg.iaa.es/en/content/sampedro-cluster-catalog).

  16. An Investigation on the Use of Different Centroiding Algorithms and Star Catalogs in Astro-Geodetic Observations

    Science.gov (United States)

    Basoglu, Burak; Halicioglu, Kerem; Albayrak, Muge; Ulug, Rasit; Tevfik Ozludemir, M.; Deniz, Rasim

    2017-04-01

    In the last decade, the importance of high-precise geoid determination at local or national level has been pointed out by Turkish National Geodesy Commission. The Commission has also put objective of modernization of national height system of Turkey to the agenda. Meanwhile several projects have been realized in recent years. In Istanbul city, a GNSS/Levelling geoid was defined in 2005 for the metropolitan area of the city with an accuracy of ±3.5cm. In order to achieve a better accuracy in this area, "Local Geoid Determination with Integration of GNSS/Levelling and Astro-Geodetic Data" project has been conducted in Istanbul Technical University and Bogazici University KOERI since January 2016. The project is funded by The Scientific and Technological Research Council of Turkey. With the scope of the project, modernization studies of Digital Zenith Camera System are being carried on in terms of hardware components and software development. Accentuated subjects are the star catalogues, and centroiding algorithm used to identify the stars on the zenithal star field. During the test observations of Digital Zenith Camera System performed between 2013-2016, final results were calculated using the PSF method for star centroiding, and the second USNO CCD Astrograph Catalogue (UCAC2) for the reference star positions. This study aims to investigate the position accuracy of the star images by comparing different centroiding algorithms and available star catalogs used in astro-geodetic observations conducted with the digital zenith camera system.

  17. BOSS discovery of 3 probable nearby supernovae

    Science.gov (United States)

    Parker, Stuart; Marples, Peter; Bock, Greg; Drecher, Colin; Search, Pat Pearl Backyard Observatory Supernova

    2017-03-01

    During the on going BOSS sky survey on 2017 March 7th and 8th using data from Parkdale Observatory, Stuart Parker, Canterbury, New Zealand, reports the discovery of 3 apparent supernovae on a 30-s Clear filter CCD image (limiting mag 18) taken by himself with a 30-cm Astro-Tech AT12RC Ritchey-Chretien astrograph (+ ST10 camera) . AT2017caw RA=08:07:50.10, DEC=-61:46:15.60, Discovery date=2017-03-08.078, Discovery mag=18 Filter:Clear-offset 1.5W 14.6S AT2017bzc RA=23:16:14.69, DEC=-42:34:10.90, Discovery date=2017-03-07.219, Discovery mag=12.8 Filder:Clear- offset 45E 50N AT2017bzb RA=22:57:17.30, DEC=-41:00:57.60, Discovery date=2017-03-07.213, Discovery mag=13 Filter: Clear-offset 12W 196N AT2017bzb and AT2017bzc are very early morning targets being very low just before sunrise.

  18. Photographic stellar photometry in the late 19th and early 20th centuries

    Science.gov (United States)

    Hearnshaw, John B.

    2001-10-01

    The development of photographic stellar photometry in the late nineteenth and early twentieth centuries is reviewed. Major pioneers in this field were the Pickerings at Harvard, who early on recognized the immense potential of photography as well as some of its inherent problems. Two huge programmes in celestial photography dominated late 19th century astronomy, the CPD and the Carte du Ciel. The problems of obtaining magnitudes from field star images were numerous, including reciprocity failure, unknown wavelength response and variable seeing. Plate calibration techniques and the use of standard stars also created new problems. Some observers preferred extrafocal images, as these gave more reliable results for brighter stars. The ill-fated North Polar Sequence and the associated International System were products of this era. The NPS originated from Harvard about 1907, was adopted by the Astrographic Congress in 1909 and (in greatly expanded form) also by the IAU at its first General Assembly in 1922, but was never able to deliver a completely reliable and transferable system of standard stellar magnitudes for use by all observers.

  19. CCD Camera Observations

    Science.gov (United States)

    Buchheim, Bob; Argyle, R. W.

    One night late in 1918, astronomer William Milburn, observing the region of Cassiopeia from Reverend T.H.E.C. Espin's observatory in Tow Law (England), discovered a hitherto unrecorded double star (Wright 1993). He reported it to Rev. Espin, who measured the pair using his 24-in. reflector: the fainter star was 6.0 arcsec from the primary, at position angle 162.4 ^{circ } (i.e. the fainter star was south-by-southeast from the primary) (Espin 1919). Some time later, it was recognized that the astrograph of the Vatican Observatory had taken an image of the same star-field a dozen years earlier, in late 1906. At that earlier epoch, the fainter star had been separated from the brighter one by only 4.8 arcsec, at position angle 186.2 ^{circ } (i.e. almost due south). Were these stars a binary pair, or were they just two unrelated stars sailing past each other? Some additional measurements might have begun to answer this question. If the secondary star was following a curved path, that would be a clue of orbital motion; if it followed a straight-line path, that would be a clue that these are just two stars passing in the night. Unfortunately, nobody took the trouble to re-examine this pair for almost a century, until the 2MASS astrometric/photometric survey recorded it in late 1998. After almost another decade, this amateur astronomer took some CCD images of the field in 2007, and added another data point on the star's trajectory, as shown in Fig. 15.1.

  20. Progressive Research and Outreach at the WestRock Observatory

    Science.gov (United States)

    Brown, Johnny Eugene; Lantz Caughey, Austin; O'Keeffe, Brendon; Johnson, Michael; Murphy Williams, Rosa Nina

    2016-01-01

    The WestRock Observatory (WRO), located in Columbus State University's Coca-Cola Space Science Center (CCSSC), is dedicated to education and research in astronomy through hands-on engagement and public participation. The WRO has recently received funding to upgrade the PlaneWave CDK 24-inch Corrected Dall-Kirkham Astrograph telescope. Recent additions to the telescope include an all-new Apogee Alta F16 CCD camera complete with a filter wheel (with narrowband and broadband filters) and a Minor Planet Center Observatory Code (W22). These new upgrades have allowed Astrophysics students to conduct unique research ranging from high precision minor planet astrometry, to broad- and narrow-band imaging of nebulae, to light curve analysis for variable star photometry. These new endeavours, in conjunction with an existing suite of Solar telescopes, gives the WRO the ability to live-stream solar and night-time observing. These streams are available both online and through interactive displays at the CCSSC making the WRO an educational outreach program for a worldwide public audience and a growing astronomical community.Current funding is allowing students to get even more research experience than previously attainable further enabling the expansion of our publicly available gallery of nebula and galaxy images. Support and funding for the acquirement,installation, and upgrading of the new PlaneWave CDK24 has been provided by the International Museum and Library Services via the Museums for America Award Additionally, individual NASA Space Grant Scholarships have helped to secure a number of student interns partially responsible for recent improvements.

  1. Photographic and CCD Sky Patrols with Small Telescopes

    Science.gov (United States)

    Kroll, Peter

    Since the twenties of the last century Sonneberg Observatory runs in each clear night a photographic Sky Patrol with a system of small telescopes (55/250 mm) reaching 14m in the blue and 13m in the yellow-red. In addition, a so-called Field Patrol is run with 2 astrographs (400/2000 mm) and a Schmidt camera (500/700/1720 mm) covering 80 selected fields along or near the Milky Way. From these instruments an archive of alomost 300,000 photographic plates arose, documenting the history of the starry night over more than 75 years. Currently much effort is made to take over this photographic sky patrol by a system of electronic detectors. Owing to the fact, that wide-field systems need either large CCDs or arrays of CCDs in order to cover the whole field of view, the technical availability of large detectors was one of the central problems in past. We now invent the use of a PHILIPS 4K×7K chip in wide-field astronomy for Whole-Sky Patrol. Although the chip has a quantum efficiency of only about 30 %, its big size (12μm pixel size) of 48×84 mm offers, for the first time, the replacement of large photographic plates by a single CCD chip. We report our first experiences with this chip when using it with a super wide-angle objective for whole-sky imaging each minute down to ca. 10m for investigating different targets (variable stars, meteors, GRB counterparts, etc.) and first trial to use the large-size chip with other small telescopes (400 to 600 mm diameter) at Sonneberg Observatory.

  2. CSU's MWV Observatory: A Facility for Research, Education and Outreach

    Science.gov (United States)

    Hood, John; Carpenter, N. D.; McCarty, C. B.; Samford, J. H.; Johnson, M.; Puckett, A. W.; Williams, R. N.; Cruzen, S. T.

    2014-01-01

    The Mead Westvaco Observatory (MWVO), located in Columbus State University's Coca-Cola Space Science Center, is dedicated to education and research in astronomy through hands-on engagement and public participation. The MWVO has recently received funding to upgrade from a 16-inch Meade LX-200 telescope to a PlaneWave CDK 24-inch Corrected Dall-Kirkham Astrograph telescope. This and other technological upgrades will allow this observatory to stream live webcasts for astronomical events, allowing a worldwide public audience to become a part of the growing astronomical community. This poster will explain the upgrades that are currently in progress as well as the results from the current calibrations. The goal of these upgrades is to provide facilities capable of both research-class projects and widespread use in education and public outreach. We will present our initial calibration and tests of the observatory equipment, as well as its use in webcasts of astronomical events, in solar observing through the use of specialized piggy-backed telescopes, and in research into such topics as asteroids, planetary and nebula imaging. We will describe a pilot research project on asteroid orbit refinement and light curves, to be carried out by Columbus State University students. We will also outline many of the K-12 educational and public outreach activities we have designed for these facilities. Support and funding for the acquisition and installation of the new PlaneWave CDK 24 has been provided by the International Museum and Library Services via the Museums for America Award.

  3. The challenges and frustrations of a veteran astronomical optician: Robert Lundin, 1880-1962

    Science.gov (United States)

    Briggs, John W.; Osterbrock, Donald E.

    1998-12-01

    Robert Lundin, apprenticed in nineteenth century optical craftsmanship but employed in twenty century fabrication and engineering, suffered many frustrations during a nonetheless productive career. Son of Carl A.R. Lundin, a senior optician at the famous American firm of Alvan Clark & Sons, Robert grew up building telescopes. As a teenager, he assisted with projects including the 1-m [40-inch] objective for Yerkes Observatory. After his father's death in 1915, he became manager of the Clark Corporation and was responsible for many smaller, successful refractors and reflectors. Lundin also completed major projects, including a highly praised 50.8-cm achromat for Van Vleck Observatory, as well as a successful 33-cm astrograph used at Lowell to discover Pluto. In 1929, a dispute with the owners of the Clark Corporation led to Lundin's resignation and his creation of a new business, "C.A. Robert Lundin and Associates." This short-lived firm built several observatory refractors, including a 26.7 cm for E.W. Rice, the retired chairman of General Electric. But none was entirely successful, and the Great Depression finished off the company. In 1933, Lundin took a job as head of Warner & Swasey's new optical shop, only to experience his greatest disasters. The 2.08-m [82-inch] reflector for McDonald Observatory was delayed for years until astronomers uncovered an error in Lundin's procedure for testing the primary mirror. A 38.1-cm photographic lens for the Naval Observatory was a complete failure. Under pressure to complete a 61-cm Schmidt camera, Lundin seems to have attempted to deceive visiting astronomers. After retirement in the mid 1940s, Lundin moved to Austin, Texas, the home of his daughter, where he died. His difficulties should not obscure his success with many instruments that continue to serve as important research and education tools.

  4. First results of the Test-Bed Telescopes (TBT) project: Cebreros telescope commissioning

    Science.gov (United States)

    Ocaña, Francisco; Ibarra, Aitor; Racero, Elena; Montero, Ángel; Doubek, Jirí; Ruiz, Vicente

    2016-07-01

    The TBT project is being developed under ESA's General Studies and Technology Programme (GSTP), and shall implement a test-bed for the validation of an autonomous optical observing system in a realistic scenario within the Space Situational Awareness (SSA) programme of the European Space Agency (ESA). The goal of the project is to provide two fully robotic telescopes, which will serve as prototypes for development of a future network. The system consists of two telescopes, one in Spain and the second one in the Southern Hemisphere. The telescope is a fast astrograph with a large Field of View (FoV) of 2.5 x 2.5 square-degrees and a plate scale of 2.2 arcsec/pixel. The tube is mounted on a fast direct-drive mount moving with speed up to 20 degrees per second. The focal plane hosts a 2-port 4K x 4K back-illuminated CCD with readout speeds up to 1MHz per port. All these characteristics ensure good survey performance for transients and fast moving objects. Detection software and hardware are optimised for the detection of NEOs and objects in high Earth orbits (objects moving from 0.1-40 arcsec/second). Nominal exposures are in the range from 2 to 30 seconds, depending on the observational strategy. Part of the validation scenario involves the scheduling concept integrated in the robotic operations for both sensors. Every night it takes all the input needed and prepares a schedule following predefined rules allocating tasks for the telescopes. Telescopes are managed by RTS2 control software, that performs the real-time scheduling of the observation and manages all the devices at the observatory.1 At the end of the night the observing systems report astrometric positions and photometry of the objects detected. The first telescope was installed in Cebreros Satellite Tracking Station in mid-2015. It is currently in the commissioning phase and we present here the first results of the telescope. We evaluate the site characteristics and the performance of the TBT Cebreros

  5. Reduction of EAO Positional Observations Database

    Science.gov (United States)

    Nefedyev, Yuri; Andreev, Alexey; Demina, Natalya; Churkin, Konstantin

    2016-07-01

    There is a large data bank of positional observations of Solar System bodies at Engelhadt Astronomical Observatory (EAO). The positional observations include the major planets, except Jupiter. Modern technologies replace classical methods of observations in astronomy and in astrometry as well. At the same time many positional observations have been gathered at astronomical observatories. So taking into account that observations of the past epochs have presenteda great value for astronomy and as times goes by their importance is growing it is obvious that positional astrometry will not lose its practical importance. This was noted in B3 XXIV IAU resolution by the General Assembly. The results of reduction of solar system bodies observations were published mainly in Proceeding of EAO and Transactions of Kazan City Astronomical Observatory. Earlier there have been made about three thousand observations at EAO and Zelenchuk station with the Zeiss telescope (D=400mm, f=2000mm), AFR-18 (photo visual, D=200, f=2000), refractor (D=400mm, f=3450mm), Meniscus camera (D=340mm, f=1200mm), Schmidt camera (D=350mm, f=2000mm). The major planets except Pluto and Neptune were observed with a special cassette chamber equipped with a rotating disk which had an open sector to reduce the brightness of the planets. The dimension of the sector was chosen accordingto the brightness of the planets. The disk was placed in the centre of the astrograph's field. The stars' true brightness was preserved. A large number of catalogues were compiled by the end of the 20th century. We used Tycho-2 catalogue for reducing our observations. As it is known the catalogue Tycho-2 (Tycho-2 catalogue, 2000) includes 2539913 stars. The stars' proper motions given in the catalogue were obtained by comparing positions from Tycho-2 with positions from the Astrographic Catalogue. Therefore they are considered to be highly accurate. The accuracy of stellar positions in Tycho-2 is about 60 mas and the accuracy of

  6. Early epoch stellar positions from the Bordeaux Carte du Ciel

    Science.gov (United States)

    Odenkirchen, Michael; Soubiran, Caroline; Le Campion, J. François

    Astrometric measurements made by the satellite Hipparcos have brought forth a homogeneous system of precise proper motions of about 105 stars, which is unprecedented in its combination of quality and quantity. Such proper motions are of great importance in various sorts of kinematic studies. However, the proper motion system needs to be disseminated and extended to stars of fainter magnitudes by means of earth-bound observations. Here, photographic records of star positions from the beginning of the 20th century present a valuable and indispensable source of information. A first important step was made with the construction of the ACT Catalogue (Urban et al. 1997), which incorporates the ancient plate measurements of the so-called Astrographic Catalogue (AC). A second series of plates, the so-called Carte du Ciel (CdC), taken as part of the same survey project as the AC, has not been used systematically for astrometry so far. The advantage of the CdC is that it reaches about 3 mag fainter than the AC. It provides however less redundancy from plate overlap. The Observatoire de Bordeaux has initiated a program for the digitisation and measurement of its collection of CdC plates which covers the zone of +11 to +17 declination and contains positions for about 8 × 105 stars at epochs mostly between 1910 and 1920. As a pilot study for this program, we are currently working on two regions near the galactic anticenter, one surrounding the open cluster NGC 2355, the other intersecting the galactic plane at l 195. These regions were selected for practical as well as for scientific reasons. The plates have been digitised on the MAMA machine at the Observatoire de Paris. Object detection was made using the software SExtractor (Bertin & Arnouts 1996). The plate limit proves to be at B = 15 and a completeness of 80 percent is reached up to 14th magnitude. The plates of the CdC provide three equal exposures with a small angular separation of 10 arc second. A loss of about 20

  7. Obituary: Geoffrey Gardner Douglass, 1942-2005

    Science.gov (United States)

    Mason, Brian D.; Hartkopf, William; Corbin, Thomas

    2005-12-01

    Geoffrey Gardner Douglass passed away on 15 February 2005, following a long illness. Geoff was born 11 June 1942 in Rocky River, Ohio, and grew up there with a passion for science, theatre, and pets. He attended the nearby Case Institute of Technology (Cleveland, Ohio) before coming to the U.S. Naval Observatory on 28 April 1967. He worked at the USNO for over 30 years, until his retirement in January 1999. He was involved in the observing and measurement of parallax and double star plates on the SAMM and MANN measuring engines, and was stationed at Blenheim, New Zealand from 1985-1988 working at the Black Birch site on the Twin Astrograph Telescope. While there he and his wife Doris travelled extensively throughout New Zealand and Australia, He later worked with an early iteration of the USNO StarScan measuring machine. However, most of his work involved observations of visual double stars with the USNO 26-inch Clark Refractor, collaborating with F.J. ("Jerry") Josties on the photographic program in the late 1960s to the development of the USNO's speckle interferometry program throughout the 1990s. Geoff collaborated closely with Charles Worley from 1968 until Charles's death in December 1997, writing much of the double star software and assisting in the production of the USNO's double star catalogs. This was a period of transition, when some 200,000 punch cards of the Lick IDS (Index Catalog of Double Stars) were transferred from Lick Observatory to the USNO, then converted to magnetic tape. This ultimately resulted in the 1984 WDS catalog (currently maintained online). It was often joked that the "W" and "D" in the WDS (officially the "Washington Double Star" catalog) really stood for "Worley" and "Douglass." The "Curmudgeon" and the "Dour Scot" were a team for nearly thirty years. Geoff's first observation, of BU 442, was made 2 June 1967 with the USNO double star (photographic) camera, and his last, STF 342, was made on 28 November 1998 with the USNO speckle

  8. VizieR Online Data Catalog: Periods of 4-10 Myr old T Tauri members of Orion OB1 (Karim+, 2016)

    Science.gov (United States)

    Karim, M. T.; Stassun, K. G.; Briceno, C.; Vivas, A. K.; Raetz, S.; Mateu, C.; Downes, J. J.; Calvet, N.; Hernandez, J.; Neuhauser, R.; Mugrauer, M.; Takahashi, H.; Tachihara, K.; Chini, R.; Cruz-Dias, G. A.; Aarnio, A.; James, D. J.; Hackstein, M.

    2017-02-01

    The Astronomia Variability Survey of Orion (CVSO) was carried out at the Llano del Hato National Astronomical Observatory in Venezuela, with the QUEST CCD mosaic camera (8000*8000pixels) on the 1m (clear aperture) Schmidt telescope, with a plate scale of 1.02''/pixel and field of view of 5.4 deg2. This V-, RC-, and IC-band multi-epoch survey, covering ~180deg2 of the Orion OB1 association, spans a time baseline of 12yr, from 1998 December to 2011 February. The 25 Ori cluster was observed by the 0.6/0.9m Schmidt-type telescope at Jena Observatory (Germany), the two 5.9'' telescopes at Observatorio Cerro Armazones (OCA, Chile), and the 1.5m reflector at the Gunma Astronomical Observatory in Japan, over four observing campaigns during the years 2010-2013. The Jena Schmidt-type telescope was equipped with the optical Schmidt Telescope Camera (STK), with an e2v 42-10 2048*2048 detector, yielding a plate scale of 1.55''/pixel and a field of view of 53'*53', thus encompassing most of the cluster. The Jena 50s exposures, all taken through the R filter, were centered on 25 Ori. A total of 8506 individual exposures were obtained in 108 nights. The Gunma 1.5m reflector observations were carried out by obtaining 60s integrations in R with the Gunma Low-resolution Spectrograph and Imager (GLOWS), which has an e2v CCD55-30 1250*1152 pixel detector with a 0.6''/pixel scale, covering a field of view of 12.5'*11.5'. Observations were obtained during four nights in year 2010. The Observatorio Cerro Armazones observations were done in the R band using the RoBoTT (Robotic Bochum TWin Telescope), which consists of twin Takahashi 150mm aperture apochromatic astrographs, each equipped with an Apogee U16M camera with a KAF-16803 4096*4096 pixel CCD, providing a 2.7°*2.7° field of view with 2.37''/pixel scale. The 60s exposures were centered on 25 Ori, spanning an area much larger than the cluster. OCA data were obtained during all YETI seasons. During the nights of 2006 January 8-15, we

  9. Obituary: Julena Steinheider Duncombe, 1911-2003

    Science.gov (United States)

    Seidelmann, P. Kenneth

    2004-12-01

    Julena Steinheider Duncombe died on 13 September 2003, just eight days before her 92nd birthday. Julena Steinheider was born September 21, 1911 on a farm in Dorchester, Nebraska and grew up in Goehner, Nebraska. Her parents were Frederick and Ella Beenders Steinheider, and she had four brothers. She began college at the age of 17 and graduated at 21 from Doane College in Crete, Nebraska with a major in mathematics and a minor in astronomy. She started teaching in a one-room schoolhouse, where, with assistance from her family, she started possibly the first school lunch program by fixing lunches on the schoolhouse stove to provide food for children who only had popcorn to eat. Then she taught in Minatare and Scotts Bluff, Nebraska, and in a Japanese Relocation Camp in Wyoming. In 1945 she moved to Washington DC to begin working at the US Naval Observatory (USNO). She was the first woman observer on the 6-inch transit circle. She worked as an observer and mathematician reducing and analyzing observations of the Sun, Moon, planets, and stars. At the Naval Observatory she met Raynor Duncombe and married him in Goehner, Nebraska, in January 1948. She resigned from the USNO in 1948 to go with her husband to Yale University. At Yale the Duncombes introduced punched card equipment into the Astronomy Department. Ray also took graduate classes and Julie worked on Astrographic Catalog reductions. Upon returning to USNO in 1950 she joined the Nautical Almanac Office. She supervised the punched card operated typewriter to produce tables of positions of celestial bodies for air and sea navigation. With Dorrit Hoffleit she directed the keypunching of over 150 star catalogs, approximating 1.5 million cards. Several thousand errata to the catalogs were discovered and corrected on the cards and tape versions of the catalogs. This activity was the basis for future stellar databases. From 1963 she was responsible for producing the tabular predictions and maps for solar and lunar

  10. VizieR Online Data Catalog: Photometry for HATS-31 through HATS-35 (de Val-Borro+, 2016)

    Science.gov (United States)

    de Val-Borro, M.; Bakos, G. A.; Brahm, R.; Hartman, J. D.; Espinoza, N.; Penev, K.; Ciceri, S.; Jordan, A.; Bhatti, W.; Csubry, Z.; Bayliss, D.; Bento, J.; Zhou, G.; Rabus, M.; Mancini, L.; Henning, T.; Schmidt, B.; Tan, T. G.; Tinney, C. G.; Wright, D. J.; Kedziora-Chudczer, L.; Bailey, J.; Suc, V.; Durkan, S.; Lazar, J.; Papp, I.; Sari, P.

    2017-05-01

    The HATSouth survey is a global network of homogeneous, completely automated wide-field telescopes located at three sites in the Southern Hemisphere: HS-1 and -2 are located at Las Campanas Observatory (LCO) in Chile, HS-3 and -4 are located at the High Energy Stereoscopic Survey (H.E.S.S.) site in Namibia, and HS-5 and -6 are located at Siding Spring Observatory (SSO) in Australia. Observations are performed using a Sloan-r filter with four-minute exposures. The HATSouth network was commissioned in 2009 and since then has proved to be a robust system for the monitoring of time-variable phenomena. Each HATSouth unit consists of four Takahashi E180 astrographs with an aperture of 18cm and an f/2.8 focal ratio on a common mount, equipped with Apogee 4096*4096 U16M ALTA cameras. HATS-31 was observed with the HS-1.4/G565 on 2012 Dec-2013 Jun, with the HS-3.4/G565 on 2012 Dec-2013 Jul, and with the HS-5.4/G565 on 2012 Dec-2013 Jul. HATS-32 was observed with the HS-2.3/G586 on 2010 Aug-2011 Nov, with the HS-4.3/G586 on 2010 Aug-2011 Nov, and with the HS-6.3/G586 on 2010 Aug-2011 Nov. HATS-33 was observed with the HS-1.4/G747 on 2013 Mar-2013 Oct, with the HS-2.4/G747 on 2013 Sep-2013 Oct, with the HS-3.4/G747 on 2013 Apr-2013 Nov, with the HS-4.4/G747 on 2013 Sep-2013 Nov, with the HS-5.4/G747 on 2013 Mar-2013 Nov, and with the HS-6.4/G747 on 2013 Sep-2013 Nov. HATS-34 was observed with the HS-2.4/G754 on 2012 Sep-2012 Dec, with the HS-4.4/G754 on 2012 Sep-2013 Jan, and with the HS-6.4/G754 on 2012 Sep-2012 Dec. HATS-35 was observed with the HS-2.4/G778 on 2011 May-2012 Nov, with the HS-4.4/G778 on 2011 Jul-2012 Nov, with the HS-6.4/G778 on 2011 Apr-2012 Oct. The egress of HATS-31b was observed on 2015 February 28 and 2015 April 02 with the Las Cumbres Observatory Global Telescope (LCOGT) 1m+Cerro Tololo Inter-American Observatory (CTIO) telescope network and the Swope 1m telescopes, respectively. Additionally, an almost full transit of HATS-31b was observed with LCOGT 1

  11. SN1987A's Twentieth Anniversary

    Science.gov (United States)

    2007-02-01

    Looking back at 20 Years of Observations of this Supernova with ESO telescopes The unique supernova SN 1987A has been a bonanza for astrophysicists. It provided several observational 'firsts,' like the detection of neutrinos from an exploding star, the observation of the progenitor star on archival photographic plates, the signatures of a non-spherical explosion, the direct observation of the radioactive elements produced during the blast, observation of the formation of dust in the supernova, as well as the detection of circumstellar and interstellar material. ESO PR Photo 08a/07 ESO PR Photo 08a/07 SN1987A in the Large Magellanic Cloud Today, it is exactly twenty years since the explosion of Supernova 1987A in the Large Magellanic Cloud was first observed, at a distance of 163,000 light-years. It was the first naked-eye supernova to be seen for 383 years. Few events in modern astronomy have met with such an enthusiastic response by the scientists and now, after 20 years, it continues to be an extremely exciting object that is further studied by astronomers around the world, in particular using ESO's telescopes. When the first signs of Supernova 1987A, the first supernova of the year 1987, were noticed early on 24 February of that year, it was clear that this would be an unusual event. It was discovered by naked-eye and on a panoramic photographic plate taken with a 10-inch astrograph on Las Campanas in Chile by Oscar Duhalde and Ian Shelton, respectively. A few hours earlier, still on 23 February, two large underground detectors - in Japan and the USA - had registered the passage of high-energy neutrinos. Since SN 1987A exploded in the Large Magellanic Cloud (LMC), it was only accessible to telescopes in the Southern Hemisphere, more particularly in Australia, South Africa, and South America. In Chile, ESO's observatory at La Silla with its armada of telescopes with sizes between 0.5 and 3.6-m, played an important role. ESO PR Photo 08c/07 ESO PR Photo 08c/07 The