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Sample records for sandiford cassegrain echelle

  1. High Resolution Stellar Spectroscopy with VBT Echelle Spectrometer

    Indian Academy of Sciences (India)

    Easy operations. We finally preferred the all transmitting system for the spectrometer with the optical surfaces anti-reflection coated to optimize the throughput rather than reflecting cameras with central obscurations. Following other optimized throughput spectrometers like. Sandiford at McDonald Observatory (McCarthy et al ...

  2. Post - SM4 Flux Calibration of the STIS Echelle Modes

    Science.gov (United States)

    Bostroem, Azalee; Aloisi, A.; Bohlin, R. C.; Proffitt, C. R.; Osten, R. A.; Lennon, D.

    2010-07-01

    Like all STIS spectroscopic modes, STIS echelle modes show a wavelength dependent decline in detector sensitivity with time. The echelle sensitivity is further affected by a time-dependent shift in the blaze function. To better correct the effects of the echelle sensitivity loss and the blaze function changes, we derive new baselines for echelle sensitivities from post-HST Servicing Mission 4 observations of the standard star G191-B2B. We present how these baseline sensitivities compare to pre-failure trends.

  3. A new Cassegrain calibration lamp unit for the Blanco Telescope

    Science.gov (United States)

    Points, S. D.; James, D. J.; Tighe, R.; Montané, A.; David, N.; Martínez, M.

    2016-08-01

    The f/8 RC-Cassegrain Focus of the Blanco Telescope at Cerro Tololo Inter-American Observatory, hosts two new instruments: COSMOS, a multi-object spectrograph in the visible wavelength range (350 - 1030nm), and ARCoIRIS, a NIR cross-dispersed spectrograph featuring 6 spectral orders spanning 0.8 - 2.45μm. Here we describe a calibration lamp unit designed to deliver the required illumination at the telescope focal plane for both instruments. These requirements are: (1) an f/8 beam of light covering a spot of 92mm diameter (or 10 arcmin) for a wavelength range of 0.35μm through 2.5μm and (2) no saturation of flat-field calibrations for the minimal exposure times permitted by each instrument, and (3) few saturated spectral lines when using the wavelength calibration lamps for the instruments. To meet these requirements this unit contains an adjustable quartz halogen lamp for flat-field calibrations, and one hollow cathode lamp and four penray lamps for wavelength calibrations. The wavelength calibration lamps are selected to provide optimal spectral coverage for the instrument mounted and can be used individually or in sets. The device designed is based on an 8-inch diameter integrating sphere, the output of which is optimized to match the f/8 calibration input delivery system which is a refractive system based on fused-silica lenses. We describe the optical design, the opto-mechanical design, the electronic control and give results of the performance of the system.

  4. Sistemas Correctores de Campo Para EL Telescopio Cassegrain IAC80

    Science.gov (United States)

    Galan, M. J.; Cobos, F. J.

    1987-05-01

    El proyecto de instrumentación de mayor importancia que ha tenido el Instituto de Astrofisica de Canarias en los últimos afios ha sido el diseflo y construcción del te1escopio IAC8O. Este requería del esfuerzo con junto en mec´nica, óptica y electrónica, lo que facilitó la estructuración y el crecimiento de los respectivos grupos de trabajo, que posteriormente se integraron en departamentos En su origen (1977), el telescopio IAC80 fue concebido como un sistema clásico tipo Cassegrain, con una razón focal F/i 1.3 para el sistema Casse grain y una razón focal F/20 para el sistema Coudé. Posteriormente, aunque se mantuvo la filosofia de que el sistema básico fuera el F/11.3, se consideró conveniente el diseño de secundarios para razones focales F/16 y F/32, y se eliminó el de F/20. Sin embargo, dada la importancia relativa que un foco estrictamente fotográfico tiene en un telescopio moderno, diseñado básicamente para fotometría fotoeléctrica y con un campo util mínimamente de 40 minutos de arco, se decídió Ilevar a cabo el diseño de un secundario F/8 con un sistema corrector de campo, pero que estuviera formado únicamente por lentes con superficies esféricas para que asl su construcción fuera posible en España ó en México. La creciente utilización de detectores bidimensionales para fines de investigación astron6mica y la viabilidad de que en un futuro cercano éstos tengan un área sensible cada vez mayor, hicieron atractiva la idea de tener diseñado un sistema corrector de campo para el foco primario (F/3), con un campo útil mínimo de un grado, y también con la limitante de que sus componentes tuvieron sólamente supérficies esféricas. Ambos diseños de los sis-temas correctores de campo se llevaron a cabo, en gran medida, como parte de un proyecto de colaboración e intercambio en el área de diseño y evaluación de sistemas ópticos.

  5. NRES: The Network of Robotic Echelle Spectrographs

    Science.gov (United States)

    Siverd, Robert; Brown, Tim; Henderson, Todd; Hygelund, John; Barnes, Stuart; de Vera, Jon; Eastman, Jason; Kirby, Annie; Smith, Cary; Taylor, Brook; Tufts, Joseph; van Eyken, Julian

    2018-01-01

    Las Cumbres Observatory (LCO) is building the Network of Robotic Echelle Spectrographs (NRES), which will consist of four (up to six in the future) identical, optical (390 - 860 nm) high-precision spectrographs, each fiber-fed simultaneously by up to two 1-meter telescopes and a Thorium-Argon calibration source. We plan to install one at up to 6 observatory sites in the Northern and Southern hemispheres, creating a single, globally-distributed, autonomous spectrograph facility using up to ten 1-m telescopes. Simulations suggest we will achieve long-term radial velocity precision of 3 m/s in less than an hour for stars brighter than V = 11 or 12 once the system reaches full capability. Acting in concert, these four spectrographs will provide a new, unique facility for stellar characterization and precise radial velocities.Following a few months of on-sky evaluation at our BPL test facility, the first spectrograph unit was shipped to CTIO in late 2016 and installed in March 2017. After several more months of additional testing and commissioning, regular science operations began with this node in September 2017. The second NRES spectrograph was installed at McDonald Observatory in September 2017 and released to the network after its own brief commissioning period, extending spectroscopic capability to the Northern hemisphere. The third NRES spectrograph was installed at SAAO in November 2017 and released to our science community just before year's end. The fourth NRES unit shipped in October and is currently en route to Wise Observatory in Israel with an expected release to the science community in early 2018.We will briefly overview the LCO telescope network, the NRES spectrograph design, the advantages it provides, and development challenges we encountered along the way. We will further discuss real-world performance from our first three units, initial science results, and the ongoing software development effort needed to automate such a facility for a wide array of

  6. The effect of struts on the radiation diagram of Cassegrain antennas

    International Nuclear Information System (INIS)

    Henriques, L.M.D.

    1981-09-01

    This work presents a study on the effect of subreflector support members of Cassegrain antennas using the theory of scattering by cylinders structures. Expression for the surface current densities and arbitrary cross sections cylinders are developed, and the components for the scattered field are obtained. Using these results we analyse the effect of the struts on the gain reduction, and the rise of maximum side-lobe level. The final results obtained are then compared to other approximate theories. (author)

  7. Design, development, and testing of the DCT Cassegrain instrument support assembly

    Science.gov (United States)

    Bida, Thomas A.; Dunham, Edward W.; Nye, Ralph A.; Chylek, Tomas; Oliver, Richard C.

    2012-09-01

    The 4.3m Discovery Channel Telescope delivers an f/6.1 unvignetted 0.5° field to its RC focal plane. In order to support guiding, wavefront sensing, and instrument installations, a Cassegrain instrument support assembly has been developed which includes a facility guider and wavefront sensor package (GWAVES) and multiple interfaces for instrumentation. A 2-element, all-spherical, fused-silica corrector compensates for field curvature and astigmatism over the 0.5° FOV, while reducing ghost pupil reflections to minimal levels. Dual roving GWAVES camera probes pick off stars in the outer annulus of the corrected field, providing simultaneous guiding and wavefront sensing for telescope operations. The instrument cube supports 5 co-mounted instruments with rapid feed selection via deployable fold mirrors. The corrected beam passes through a dual filter wheel before imaging with the 6K x 6K single CCD of the Large Monolithic Imager (LMI). We describe key development strategies for the DCT Cassegrain instrument assembly and GWAVES, including construction of a prime focus test assembly with wavefront sensor utilized in fall 2011 to begin characterization of the DCT primary mirror support. We also report on 2012 on-sky test results of wavefront sensing, guiding, and imaging with the integrated Cassegrain cube.

  8. Development of technology for lightweight Beryllium Cassegrain Telescope for space applications and lessons learnt

    Science.gov (United States)

    Greger, R.; Rugi, E.; Hausner, Th.; Jahnen, W.; Frei, S.; Pellaton, D.; Mueller, P.; Hollenbach, I.

    2017-11-01

    This paper gives an overview on the development of a light weighted Cassegrain telescope with a 200 mm optical aperture as one key element of the Laser Altimeter which will fly on the BepiColombo mission to Mercury (BELA).The Receiver Telescope (RTL) collects the light pulse transmitted to Mercury and reflected from the planet's surface. Mercury's challenging thermal environment, the thermo-mechanical stability of the telescope and the stringent instrument's mass budget require the implementation of an innovative design solution to achieve the requested optical performance over an extended temperature range.

  9. A Python Script for Aligning the STIS Echelle Blaze Function

    Science.gov (United States)

    Baer, Malinda; Proffitt, Charles R.; Lockwood, Sean A.

    2018-01-01

    Accurate flux calibration for the STIS echelle modes is heavily dependent on the proper alignment of the blaze function for each spectral order. However, due to changes in the instrument alignment over time and between exposures, the blaze function can shift in wavelength. This may result in flux calibration inconsistencies of up to 10%. We present the stisblazefix Python module as a tool for STIS users to correct their echelle spectra. The stisblazefix module assumes that the error in the blaze alignment is a linear function of spectral order, and finds the set of shifts that minimizes the flux inconsistencies in the overlap between spectral orders. We discuss the uses and limitations of this tool, and show that its use can provide significant improvements to the default pipeline flux calibration for many observations.

  10. Development and investigation of a CPV module with Cassegrain mirror optics

    Science.gov (United States)

    Dreger, Max; Wiesenfarth, Maike; Kisser, Arne; Schmid, Tobias; Bett, Andreas W.

    2014-09-01

    One approach to concentrate the sunlight in concentrating photovoltaic (CPV) modules is using Cassegrain mirror optics. The advantage is that a passively cooled solar cell can be mounted to a large heat spreader that does not shade the primary optics. In addition, the height of the module, hence weight, can be low. The design was selected on the basis of the results of a design study comparing different CPV module approaches presented in [1]. In this work, we present the development of a new prototype micro dish module. First results of the characterization are shown. Besides of the electrical performance, a machined optics and an injection molded was investigated regarding sensitivity to misalignment errors between the optical elements as well as measurement of the acceptance angle in- and outdoors. The machined optics was used as reference.

  11. SpUpNIC (Spectrograph Upgrade: Newly Improved Cassegrain) on the South African Astronomical Observatory's 74-inch telescope

    Science.gov (United States)

    Crause, Lisa A.; Carter, Dave; Daniels, Alroy; Evans, Geoff; Fourie, Piet; Gilbank, David; Hendricks, Malcolm; Koorts, Willie; Lategan, Deon; Loubser, Egan; Mouries, Sharon; O'Connor, James E.; O'Donoghue, Darragh E.; Potter, Stephen; Sass, Craig; Sickafoose, Amanda A.; Stoffels, John; Swanevelder, Pieter; Titus, Keegan; van Gend, Carel; Visser, Martin; Worters, Hannah L.

    2016-08-01

    SpUpNIC (Spectrograph Upgrade: Newly Improved Cassegrain) is the extensively upgraded Cassegrain Spectrograph on the South African Astronomical Observatory's 74-inch (1.9-m) telescope. The inverse-Cassegrain collimator mirrors and woefully inefficient Maksutov-Cassegrain camera optics have been replaced, along with the CCD and SDSU controller. All moving mechanisms are now governed by a programmable logic controller, allowing remote configuration of the instrument via an intuitive new graphical user interface. The new collimator produces a larger beam to match the optically faster Folded-Schmidt camera design and nine surface-relief diffraction gratings offer various wavelength ranges and resolutions across the optical domain. The new camera optics (a fused silica Schmidt plate, a slotted fold flat and a spherically figured primary mirror, both Zerodur, and a fused silica field-flattener lens forming the cryostat window) reduce the camera's central obscuration to increase the instrument throughput. The physically larger and more sensitive CCD extends the available wavelength range; weak arc lines are now detectable down to 325 nm and the red end extends beyond one micron. A rear-of-slit viewing camera has streamlined the observing process by enabling accurate target placement on the slit and facilitating telescope focus optimisation. An interactive quick-look data reduction tool further enhances the user-friendliness of SpUpNI

  12. Study on power coupling of annular vortex beam propagating through a two-Cassegrain-telescope optical system in turbulent atmosphere.

    Science.gov (United States)

    Wu, Huiyun; Sheng, Shen; Huang, Zhisong; Zhao, Siqing; Wang, Hua; Sun, Zhenhai; Xu, Xiegu

    2013-02-25

    As a new attractive application of the vortex beams, power coupling of annular vortex beam propagating through a two- Cassegrain-telescope optical system in turbulent atmosphere has been investigated. A typical model of annular vortex beam propagating through a two-Cassegrain-telescope optical system is established, the general analytical expression of vortex beams with limited apertures and the analytical formulas for the average intensity distribution at the receiver plane are derived. Under the H-V 5/7 turbulence model, the average intensity distribution at the receiver plane and power coupling efficiency of the optical system are numerically calculated, and the influences of the optical topological charge, the laser wavelength, the propagation path and the receiver apertures on the power coupling efficiency are analyzed. These studies reveal that the average intensity distribution at the receiver plane presents a central dark hollow profile, which is suitable for power coupling by the Cassegrain telescope receiver. In the optical system with optimized parameters, power coupling efficiency can keep in high values with the increase of the propagation distance. Under the atmospheric turbulent conditions, great advantages of vortex beam in power coupling of the two-Cassegrain-telescope optical system are shown in comparison with beam without vortex.

  13. An echelle spectrograph for middle ultraviolet solar spectroscopy from rockets.

    Science.gov (United States)

    Tousey, R; Purcell, J D; Garrett, D L

    1967-03-01

    An echelle grating spectrograph is ideal for use in a rocket when high resolution is required becaus itoccupies a minimum of space. The instrument described covers the range 4000-2000 A with a resolution of 0.03 A. It was designed to fit into the solar biaxial pointing-control section of an Aerobee-150 rocket. The characteristics of the spectrograph are illustrated with laboratory spectra of iron and carbon are sources and with solar spectra obtained during rocket flights in 1961 and 1964. Problems encountered in analyzing the spectra are discussed. The most difficult design problem was the elimination of stray light when used with the sun. Of the several methods investigated, the most effective was a predispersing system in the form of a zero-dispersion double monochromator. This was made compact by folding the beam four times.

  14. Performance of the Multi-Spectral Solar Telescope Array. III - Optical characteristics of the Ritchey-Chretien and Cassegrain telescopes

    Science.gov (United States)

    Hoover, Richard B.; Baker, Phillip C.; Hadaway, James B.; Johnson, R. B.; Peterson, Cynthia; Gabardi, David R.; Walker, Arthur B., Jr.; Lindblom, J. F.; Deforest, Craig; O'Neal, R. H.

    1991-12-01

    The Multi-Spectral Solar Telescope Array (MSSTA), which is a sounding-rocket-borne observatory for investigating the sun in the soft X-ray/EUV and FUV regimes of the electromagnetic spectrum, utilizes single reflection multilayer coated Herschelian telescopes for wavelengths below 100 A, and five doubly reflecting multilayer coated Ritchey-Chretien and two Cassegrain telescopes for selected wavelengths in the EUV region between 100 and 1000 A. The paper discusses the interferometric alignment, testing, focusing, visible light testing, and optical performance characteristics of the Ritchey-Chretien and Cassegrain telescopes of MSSTA. A schematic diagram of the MSSTA Ritchey-Chretien telescope is presented together with diagrams of the system autocollimation testing.

  15. Subreflector extension for improved efficiencies in Cassegrain antennas - GTD/PO analysis. [Geometrical Theory of Diffraction/Physical Optics

    Science.gov (United States)

    Rahmat-Samii, Yahya

    1986-01-01

    Both offset and symmetric Cassegrain reflector antennas are used in satellite and ground communication systems. It is known that the subreflector diffraction can degrade the performance of these reflectors. A geometrical theory of diffraction/physical optics analysis technique is used to investigate the effects of the extended subreflector, beyond its optical rim, on the reflector efficiency and far-field patterns. Representative numerical results are shown for an offset Cassegrain reflector antenna with different feed illumination tapers and subreflector extensions. It is observed that for subreflector extensions as small as one wavelength, noticeable improvements in the overall efficiencies can be expected. Useful design data are generated for the efficiency curves and far-field patterns.

  16. The alignment and isostatic mount bonding technique of the aerospace Cassegrain telescope primary mirror

    Science.gov (United States)

    Lin, Wei Cheng; Chang, Shenq-Tsong; Lin, Yu-Chuan; Hsu, Ming-Ying; Chang, Yu-Ting; Chang, Sheng-Hsiung; Huang, Ting-Ming

    2012-10-01

    In order to meet both optical performance and structural stiffness requirements of the aerospace Cassegrain telescope, iso-static mount is used as the interface between the primary mirror and the main plate. This article describes the alignment and iso-static mount bonding technique of the primary mirror by assistance of CMM. The design and assembly of mechanical ground support equipment (MGSE) which reduces the deformation of primary mirror by the gravity effect is also presented. The primary mirror adjusting MGSE consists of X-Y linear translation stages, rotation stage and kinematic constrain platform which provides the function of decenter, orientation, tilt and height adjustment of the posture sequentially. After CMM measurement, the radius of curvature, conic constant, decenter and tilt, etc. will be calculated. According to these results, the posture of the mirror will be adjusted to reduce the tilt by the designed MGSE within 0.02 degrees and the distance deviation from the best fitted profile of mirror to main plate shall be less than 0.01 mm. After that, EC 2216 adhesive is used to bond mirror and iso-static mount. During iso-static mount bonding process, CMM is selected to monitor the relative position deviation of the iso-static mount until the adhesive completely cured. After that, the wave front sensors and strain gauges are used to monitor the strain variation while the iso-static mount mounted in the main plate with the screws by the torque wrench. This step is to prevent deformation of the mirror caused from force of the iso-static mount during the mounting process. In the end, the interferometer is used for the optical performance test with +1G and -1G to check the alignment and bonding technique is well or not.

  17. Post-SM4 Sensitivity Calibration of the STIS Echelle Modes

    Science.gov (United States)

    Bostroem, K. Azalee; Aloisi, A.; Bohlin, R.; Hodge, P.; Proffitt, C.

    2012-01-01

    On-orbit sensitivity curves for all echelle modes were derived for post - servicing mis- sion 4 data using observations of the DA white dwarf G191-B2B. Additionally, new echelle ripple tables and grating dependent bad pixel tables were created for the FUV and NUV MAMA. We review the procedures used to derive the adopted throughputs and implement them in the pipeline as well as the motivation for the modification of the additional reference files and pipeline procedures.

  18. Echelle grating multi-order imaging spectrometer utilizing a catadioptric lens

    Science.gov (United States)

    Chrisp, Michael P; Bowers, Joel M

    2014-05-27

    A cryogenically cooled imaging spectrometer that includes a spectrometer housing having a first side and a second side opposite the first side. An entrance slit is on the first side of the spectrometer housing and directs light to a cross-disperser grating. An echelle immersions grating and a catadioptric lens are positioned in the housing to receive the light. A cryogenically cooled detector is located in the housing on the second side of the spectrometer housing. Light from the entrance slit is directed to the cross-disperser grating. The light is directed from the cross-disperser grating to the echelle immersions grating. The light is directed from the echelle immersions grating to the cryogenically cooled detector on the second side of the spectrometer housing.

  19. Determination of chemical concentration with a 2 dimensional CCD array in the Echelle grating spectrometer

    Energy Technology Data Exchange (ETDEWEB)

    Lewis, D.K. [Lawrence Livermore National Lab., CA (United States); Stevens, C.G.

    1994-11-15

    The Echelle grating spectrometer (EGS) uses a stepped Echelle grating, prisms and a folded light path to miniaturize an infrared spectrometer. Light enters the system through a slit and is spread out along Y by a prism. This light then strikes the grating and is diffracted out along X. This spreading results in a superposition of spectral orders since the grating has a high spectral range. These orders are then separated by again passing through a prism. The end result of a measurement is a 2 dimensional image which contains the folded spectrum of the region under investigation. The data lies in bands from top to bottom, for example, with wavenumber increments as small as 0.1 lying from left to right such that the right end of band N is the same as the left end of band N+1. This is the image which must be analyzed.

  20. Total reduction of distorted echelle spectrograms - An automatic procedure. [for computer controlled microdensitometer

    Science.gov (United States)

    Peterson, R. C.; Title, A. M.

    1975-01-01

    A total reduction procedure, notable for its use of a computer-controlled microdensitometer for semi-automatically tracing curved spectra, is applied to distorted high-dispersion echelle spectra recorded by an image tube. Microdensitometer specifications are presented and the FORTRAN, TRACEN and SPOTS programs are outlined. The intensity spectrum of the photographic or electrographic plate is plotted on a graphic display. The time requirements are discussed in detail.

  1. Imaging and image restoration of an on-axis three-mirror Cassegrain system with wavefront coding technology.

    Science.gov (United States)

    Guo, Xiaohu; Dong, Liquan; Zhao, Yuejin; Jia, Wei; Kong, Lingqin; Wu, Yijian; Li, Bing

    2015-04-01

    Wavefront coding (WFC) technology is adopted in the space optical system to resolve the problem of defocus caused by temperature difference or vibration of satellite motion. According to the theory of WFC, we calculate and optimize the phase mask parameter of the cubic phase mask plate, which is used in an on-axis three-mirror Cassegrain (TMC) telescope system. The simulation analysis and the experimental results indicate that the defocused modulation transfer function curves and the corresponding blurred images have a perfect consistency in the range of 10 times the depth of focus (DOF) of the original TMC system. After digital image processing by a Wiener filter, the spatial resolution of the restored images is up to 57.14 line pairs/mm. The results demonstrate that the WFC technology in the TMC system has superior performance in extending the DOF and less sensitivity to defocus, which has great value in resolving the problem of defocus in the space optical system.

  2. Development of a light-weight beryllium Cassegrain telescope: from the optical design to the performance measurement

    Science.gov (United States)

    Viertl, Jacques; Greger, Ralf; Di Domenico, Maurizio; Francou, Laurent; Ellouzi, Marina; Blum, Steffen; Kudielka, Klaus; Weigel, Thomas; Rugi Grond, Elisabetta; Piazza, Daniele

    2012-12-01

    The BepiColombo Laser Altimeter (BELA) is selected to fly on board of the ESA's BepiColombo Mercury Planetary Orbiter (MPO). The instrument will be the first European planetary laser altimeter system. RUAG Space is the industrial prime for the Receiver part of the scientific instrument. The BELA Receiver is a joined effort of Swiss industries under the leading role of RUAG and University of Bern as co-Prime. A core element is the light weighted Receiver Telescope (RTL), to collect the laser pulse reflected from the planet's surface. An innovative design was required to deal with the very challenging Mercury's environmental conditions and with the very stringent instrument's mass budget. The Optothermo- mechanical analyses lead to the design of a 1250mm focal length Cassegrain telescope made of Beryllium. It provides an aperture of 204 mm diameter and a 2 mm thick primary mirror for a total mass of less than 600gr. The manufacturing and the integration needed special developments. This paper presents the design analyses and the major challenges which had to be solved. Discussing some aspects of the telescope integration and test campaign, the finally achieved performances and lessons learnt will be presented.

  3. Establishment and correction of an Echelle cross-prism spectrogram reduction model

    Science.gov (United States)

    Zhang, Rui; Bayanheshig; Li, Xiaotian; Cui, Jicheng

    2017-11-01

    The accuracy of an echelle cross-prism spectrometer depends on the matching degree between the spectrum reduction model and the actual state of the spectrometer. However, the error of adjustment can change the actual state of the spectrometer and result in a reduction model that does not match. This produces an inaccurate wavelength calibration. Therefore, the calibration of a spectrogram reduction model is important for the analysis of any echelle cross-prism spectrometer. In this study, the spectrogram reduction model of an echelle cross-prism spectrometer was established. The image position laws of a spectrometer that varies with the system parameters were simulated to the influence of the changes in prism refractive index, focal length and so on, on the calculation results. The model was divided into different wavebands. The iterative method, least squares principle and element lamps with known characteristic wavelength were used to calibrate the spectral model in different wavebands to obtain the actual values of the system parameters. After correction, the deviation of actual x- and y-coordinates and the coordinates calculated by the model are less than one pixel. The model corrected by this method thus reflects the system parameters in the current spectrometer state and can assist in accurate wavelength extraction. The instrument installation and adjustment would be guided in model-repeated correction, reducing difficulty of equipment, respectively.

  4. The assembly, calibration, and preliminary results from the Colorado high-resolution Echelle stellar spectrograph (CHESS)

    Science.gov (United States)

    Hoadley, Keri; France, Kevin; Nell, Nicholas; Kane, Robert; Schultz, Ted; Beasley, Matthew; Green, James; Kulow, Jen; Kersgaard, Eliot; Fleming, Brian

    2014-07-01

    The Colorado High-resolution Echelle Stellar Spectrograph (CHESS) is a far ultraviolet (FUV) rocket-borne experiment designed to study the atomic-to-molecular transitions within translucent interstellar clouds. CHESS is an objective echelle spectrograph operating at f/12.4 and resolving power of 120,000 over a band pass of 100 - 160 nm. The echelle flight grating is the product of a research and development project with LightSmyth Inc. and was coated at Goddard Space Flight Center (GSFC) with Al+LiF. It has an empirically-determined groove density of 71.67 grooves/mm. At the Center for Astrophysics and Space Astronomy (CASA) at the University of Colorado (CU), we measured the efficiencies of the peak and adjacent dispersion orders throughout the 90 - 165 nm band pass to characterize the behavior of the grating for pre-flight calibrations and to assess the scattered-light behavior. The crossdispersing grating, developed and ruled by Horiba Jobin-Yvon, is a holographically-ruled, low line density (351 grooves/mm), powered optic with a toroidal surface curvature. The CHESS cross-disperser was also coated at GSFC; Cr+Al+LiF was deposited to enhance far-UV efficiency. Results from final efficiency and reflectivity measurements of both optics are presented. We utilize a cross-strip anode microchannel plate (MCP) detector built by Sensor Sciences to achieve high resolution (25 μm spatial resolution) and data collection rates (~ 106 photons/second) over a large format (40mm round, digitized to 8k x 8k) for the first time in an astronomical sounding rocket flight. The CHESS instrument was successfully launched from White Sands Missile Range on 24 May 2014. We present pre-flight sensitivity, effective area calculations, lab spectra and calibration results, and touch on first results and post-flight calibration plans.

  5. Design of FHiRE: the Fiber High Resolution Echelle Spectrograph

    Science.gov (United States)

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

    2018-01-01

    The enormous success of the Kepler mission in the discovery of transiting exoplanets implies that the majority of stars have planetary systems. NASA's upcomming Transiting Exoplanet Survey Satellite (TESS) is designed to survey the brightest stars over the entire sky, systems that are accessible to spectroscopic follow-up with mid-sized telescopes. We have undertaken the development of a precision radial velocity spectrograph with the goal of providing ground-based suppoert for TESS. The instrument, known as FHiRE (Fiber High Resolution Echelle spectrograph), is being developed in collaboration with Indiana University and will deployed at the 2.3-meter telescope of the Wyoming InfraRed Observatory (WIRO). FHiRE features a traditional white pupil echelle design with R ~ 60,000 that is fed via two optical fibers from the telescope. Both the science fiber and a simultaneously sampled Thorium-Argon comparison fiber will make use of double mode scramblers. FHiRE itself will be housed within a vacuum enclosure in order to minimize any temperatue variations of the instrument and maximize its radial velocity precision. Together, these two features should enable FHiRE to reach a long-term velocity precision of < 1 m/s. We present the design of FHiRE and its expected performance. In a companion poster (Jang-Condell et al.) we will present the exoplanet science goals of the project.

  6. The Coude spectrograph and echelle scanner of the 2.7 m telescope at McDonald observatory

    Science.gov (United States)

    Tull, R. G.

    1972-01-01

    The design of the Coude spectrograph of the 2.7 m McDonald telescope is discussed. A description is given of the Coude scanner which uses the spectrograph optics, the configuration of the large echelle and the computer scanner control and data systems.

  7. Digital TV-echelle spectrograph for simultaneous multielemental analysis using microcomputer control

    International Nuclear Information System (INIS)

    Davidson, J.B.; Case, A.L.

    1980-12-01

    A digital TV-echelle spectrograph with microcomputer control was developed for simultaneous multielemental analysis. The optical system is a commercially available unit originally equipped for film and photomultiplier (single element) readout. The film port was adapted for the intensifier camera. The camera output is digitized and stored in a microcomputer-controlled, 512 x 512 x 12 bit memory and image processor. Multiple spectra over the range of 200 to 800 nm are recorded in a single exposure. Spectra lasting from nanoseconds to seconds are digitized and stored in 0.033 s and displayed on a TV monitor. An inexpensive microcomputer controls the exposure, reads and displays the intensity of predetermined spectral lines, and calculates wavelengths of unknown lines. The digital addresses of unknown lines are determined by superimposing a cursor on the TV display. The microcomputer also writes into memory wavelength fiducial marks for alignment of the TV camera

  8. Compact high-resolution echelle-AOTF NIR spectrometer for atmospheric measurements

    Science.gov (United States)

    Korablev, Oleg I.; Bertaux, Jean-Loup; Vinogradov, Imant I.; Kalinnikov, Yurii K.; Nevejans, D.; Neefs, E.; Le Barbu, T.; Durry, G.

    2017-11-01

    A new concept of a high-resolution near-IR spectrometer consisting of an echelle grating combined with an acousto-optic tunable filter (AOTF) for separation of diffraction orders, is developed for space-borne studies of planetary atmospheres. A compact design with no moving parts within the mass budget of 3-5 kg allows to reach the resolving power λ/Δλ of 20000-30000. Only a small piece of spectrum in high diffraction orders can be measured at a time, but thanks to flexibility of the AOTF electrical tuning, such pieces of spectrum can be measured randomly and rapidly within the spectral range. This development can be used for accurate measurements of important atmospheric gases, such as CO2 in terrestrial atmosphere, isotopic ratios and minor gases. A spectrometer, based on this principle, SOIR (Solar Occultation InfraRed) is being built for Venus Express (2005) ESA mission. Instruments based on this principle have high potential for the studies of the Earth, in particular for measurements of isotopes of water in the lower atmosphere, either in solar occultation profiling (tangent altitude <10 km), or observing solar glint for integral quantities of the components. Small size of hardware makes them ideal for micro-satellites, which are now agile enough to provide necessary pointing for solar occultation or glint observations. Also, the atmosphere of Mars has never been observed at local scales with such a high spectral resolution. A laboratory prototype consisting of 275-mm echelle spectrometer with Hamamatsu InGaAs 512-pixel linear array and the AOTF has demonstrated λ/Δλ≍30000 in the spectral range of 1-1.7 μm. The next set up, covering the spectral ranges of 1-1.7 μm and 2.3-4.3 μm, and the Venus Express SOIR are briefly discussed.

  9. PEPSI: the Potsdam Echelle Polarimetric and Spectroscopic Instrument for the LBT

    Science.gov (United States)

    Strassmeier, K. G.; Woche, M.; Ilyin, I.; Popow, E.; Bauer, S.-M.; Dionies, F.; Fechner, T.; Weber, M.; Hofmann, A.; Storm, J.; Materne, R.; Bittner, W.; Bartus, J.; Granzer, T.; Denker, C.; Carroll, T.; Kopf, M.; DiVarano, I.; Beckert, E.; Lesser, M.

    2008-07-01

    We present the status of PEPSI, the bench-mounted fibre-fed and stabilized "Potsdam Echelle Polarimetric and Spectroscopic Instrument" for the 2×8.4m Large Binocular Telescope in southern Arizona. PEPSI is under construction at AIP and is scheduled for first light in 2009/10. Its ultra-high-resolution mode will deliver an unprecedented spectral resolution of approximately R=310,000 at high efficiency throughout the entire optical/red wavelength range 390-1050nm without the need for adaptive optics. Besides its polarimetric Stokes IQUV mode, the capability to cover the entire optical range in three exposures at resolutions of 40,000, 130,000 and 310,000 will surpass all existing facilities in terms of light-gathering-power times spectral-coverage product. A solar feed will make use of the spectrograph also during day time. As such, we hope that PEPSI will be the most powerful spectrometer of its kind for the years to come.

  10. A search for lithium in Pleiades brown dwarf candidates using the Keck hires echelle

    Science.gov (United States)

    Marcy, Geoffrey W.; Basri, Gibor; Graham, James R.

    1994-01-01

    We report Keck Observatory high-resolution echelle spectra of lithium at 670.8 nm in two of the lowest luminosity brown dwarf candidates in the Pleiades. These objects have estimated masses of 0.055 to 0.059 solar mass from their location on a color-magnitude diagram relative to theoretical isochrones. Stellar interior models predict that Li has not burned in them. However, we find no evidence of the Li line, at limits 100 to 1000 times below the initial abundance. This indicates that Li has in fact been depleted, presumably by nuclear processing as occurs in Pleiades stars. Interior models suggest that such large Li depletion occurs only for objects with M greater than 0.09 solar mass at the age of the Pleiades. Thus, it is unlikely that the candidates are brown dwarfs. The brown dwarf candidates present a conflict: either they have masses greater than suggested from their placement on the H-R diagram, or they do have the very low suggested masses but are nonetheless capable of destroying Li, in only 70 Myr. Until this dilemma is resolved, the photometric identification of brown dwarfs will remain difficult. Resolution may reside in higher T(sub eff) derived from optical and IR colors or in lower T(sub eff) in the interior models.

  11. VizieR Online Data Catalog: Abundances in the local region. I. G and K giants (Luck, 2015)

    Science.gov (United States)

    Luck, R. E.

    2015-10-01

    At the start of this program, the observation list for giants was set to sample the G/K giants of the local region out to about 100pc from the Sun in all directions. The region was subdivided into cubes that were 25pc on a side; from each sub-volume, appropriate stars were selected north of declination -30°. This sample yielded the 286 G/K giants found in Luck et al. 2007 (cat. J/AJ/133/2464). This data set was also augmented by the addition of numerous G/K giants, increasing the number in the 100pc volume to 594 stars. Because the volume selection criteria used in Luck et al. 2007 (cat. J/AJ/133/2464) formally extended out to 115pc, a more precise comparison is that the current sample has 740 stars out to the older limit. Additional stars from the Bright Star Catalog (Hoffleit & Jaschek, 1991bsc..book.....H) were added, driving the sample out to about 200pc. The spectral database was supplemented using the ELODIE and ESO Archives. The ESO addition adds the southern sky. The bulk of the northern stars were observed using the McDonald Observatory Struve Telescope and Sandiford Cassegrain Echelle Spectrograph. For the ELODIE and ESO data archives, a list of all stars available was obtained and spectral type for each from SIMBAD was retrieved. Stars having a spectral type of F, G, or K III were then processed. The ESO data derives from the HARPS and UVES spectrographs. Basic observational data for the program stars can be found in Table1, along with some derived quantities, such as distance. The primary source of observational data for this study is a set of high signal-to-noise ratio (S/N) spectra obtained during numerous observing runs between 1997 and 2010 at McDonald Observatory using the 2.1m Struve Telescope and the Sandiford Cassegrain Echelle Spectrograph. The spectra continuously cover a wavelength range from about 484 to 700nm, with a resolving power of about 60000. Typical S/N values for the spectra are in excess of 150. To enable cancellation of telluric

  12. The science case of the PEPSI high-resolution echelle spectrograph and polarimeter for the LBT

    Science.gov (United States)

    Strassmeier, K. G.; Pallavicini, R.; Rice, J. B.; Andersen, M. I.

    2004-05-01

    We lay out the scientific rationale for and present the instrumental requirements of a high-resolution adaptive-optics Echelle spectrograph with two full-Stokes polarimeters for the Large Binocular Telescope (LBT) in Arizona. Magnetic processes just like those seen on the Sun and in the space environment of the Earth are now well recognized in many astrophysical areas. The application to other stars opened up a new field of research that became widely known as the solar-stellar connection. Late-type stars with convective envelopes are all affected by magnetic processes which give rise to a rich variety of phenomena on their surface and are largely responsible for the heating of their outer atmospheres. Magnetic fields are likely to play a crucial role in the accretion process of T-Tauri stars as well as in the acceleration and collimation of jet-like flows in young stellar objects (YSOs). Another area is the physics of active galactic nucleii (AGNs) , where the magnetic activity of the accreting black hole is now believed to be responsible for most of the behavior of these objects, including their X-ray spectrum, their notoriously dramatic variability, and the powerful relativistic jets they produce. Another is the physics of the central engines of cosmic gamma-ray bursts, the most powerful explosions in the universe, for which the extreme apparent energy release are explained through the collimation of the released energy by magnetic fields. Virtually all the physics of magnetic fields exploited in astrophysics is somehow linked to our understanding of the Sun's and the star's magnetic fields.

  13. The third flight of the Colorado high-resolution echelle stellar spectrograph (CHESS): improvements, calibrations, and preliminary results

    Science.gov (United States)

    Kruczek, Nicholas; Nell, Nicholas; France, Kevin; Hoadley, Keri; Fleming, Brian; Kane, Robert; Ulrich, Stefan; Egan, Arika; Beatty, Dawson

    2017-08-01

    In this proceeding, we describe the scientific motivation and technical development of the Colorado HighResolution Echelle Stellar Spectrograph (CHESS), focusing on the hardware advancements and testing of components for the third launch of the payload (CHESS-3). CHESS is a far ultraviolet rocket-borne instrument designed to study the atomic-to-molecular transitions within translucent cloud regions in the interstellar medium. CHESS is an objective echelle spectrograph, which uses a mechanically-ruled echelle and a powered (f/12.4) crossdispersing grating, and is designed to achieve a resolving power R > 100,000 over the bandpass λλ 1000-1600 Å. Results from final efficiency and reflectivity measurements for the optical components of CHESS-3 are presented. An important role of sounding rocket experiments is the testing and verification of the space flight capabilities of experimental technologies. CHESS-3 utilizes a 40mm-diameter cross-strip anode microchannel plate detector fabricated by Sensor Sciences LLC, capable of achieving high spatial resolution and a high global count rate (˜1 MHz). We present pre-flight laboratory spectra and calibration results, including wavelength solution and resolving power of the instrument. The fourth launch of CHESS (CHESS-4) will demonstrate a δ-doped CCD, assembled in collaboration with the Microdevices Laboratory at JPL and Arizona State University. In support of CHESS-4, the CHESS-3 payload included a photomultiplier tube, used as a secondary confirmation of the optical alignment of the payload during flight. CHESS-3 launched on 26 June 2017 aboard NASA/CU sounding rocket mission 36.323 UG. We present initial flight results for the CHESS-3 observation of the β1 Scorpii sightline.

  14. Development of infrared Echelle spectrograph and mid-infrared heterodyne spectrometer on a small telescope at Haleakala, Hawaii for planetary observation

    Science.gov (United States)

    Sakanoi, Takeshi; Kasaba, Yasumasa; Kagitani, Masato; Nakagawa, Hiromu; Kuhn, Jeff; Okano, Shoichi

    2014-08-01

    We report the development of infrared Echelle spectrograph covering 1 - 4 micron and mid-infrared heterodyne spectrometer around 10 micron installed on the 60-cm telescope at the summit of Haleakala, Hawaii (alt.=3000m). It is essential to carry out continuous measurement of planetary atmosphere, such as the Jovian infrared aurora and the volcanoes on Jovian satellite Io, to understand its time and spatial variations. A compact and easy-to-use high resolution infrared spectrometer provide the good opportunity to investigate these objects continuously. We are developing an Echelle spectrograph called ESPRIT: Echelle Spectrograph for Planetary Research In Tohoku university. The main target of ESPRIT is to measure the Jovian H3+ fundamental line at 3.9 micron, and H2 nu=1 at 2.1 micron. The 256x256 pixel CRC463 InSb array is used. An appropriate Echelle grating is selected to optimize at 3.9 micron and 2.1 micron for the Jovian infrared auroral observations. The pixel scale corresponds to the atmospheric seeing (0.3 arcsec/pixel). This spectrograph is characterized by a long slit field-of-view of ~ 50 arcsec with a spectral resolution is over 20,000. In addition, we recently developed a heterodyne spectrometer called MILAHI on the 60 cm telescope. MILAHI is characterized by super high-resolving power (more than 1,500,000) covering from 7 - 13 microns. Its sensitivity is 2400 K at 9.6 micron with a MCT photo diode detector of which bandwidth of 3000 MHz. ESPRIT and MILAHI is planned to be installed on 60 cm telescope is planned in 2014.

  15. The re-flight of the Colorado high-resolution Echelle stellar spectrograph (CHESS): improvements, calibrations, and post-flight results

    Science.gov (United States)

    Hoadley, Keri; France, Kevin; Kruczek, Nicholas; Fleming, Brian; Nell, Nicholas; Kane, Robert; Swanson, Jack; Green, James; Erickson, Nicholas; Wilson, Jacob

    2016-07-01

    In this proceeding, we describe the scientific motivation and technical development of the Colorado High- resolution Echelle Stellar Spectrograph (CHESS), focusing on the hardware advancements and testing supporting the second flight of the payload (CHESS-2). CHESS is a far ultraviolet (FUV) rocket-borne instrument designed to study the atomic-to-molecular transitions within translucent cloud regions in the interstellar medium (ISM). CHESS is an objective f/12.4 echelle spectrograph with resolving power > 100,000 over the band pass 1000 - 1600 Å. The spectrograph was designed to employ an R2 echelle grating with "low" line density. We compare the FUV performance of experimental echelle etching processes (lithographically by LightSmyth, Inc. and etching via electron-beam technology by JPL Microdevices Laboratory) with traditional, mechanically-ruled gratings (Bach Research, Inc. and Richardson Gratings). The cross-dispersing grating, developed and ruled by Horiba Jobin-Yvon, is a holographically-ruled, "low" line density, powered optic with a toroidal surface curvature. Both gratings were coated with aluminum and lithium fluoride (Al+LiF) at Goddard Space Flight Center (GSFC). Results from final efficiency and reflectivity measurements for the optical components of CHESS-2 are presented. CHESS-2 utilizes a 40mm-diameter cross-strip anode readout microchannel plate (MCP) detector fabricated by Sensor Sciences, Inc., to achieve high spatial resolution with high count rate capabilities (global rates 1 MHz). We present pre-flight laboratory spectra and calibration results. CHESS-2 launched on 21 February 2016 aboard NASA/CU sounding rocket mission 36.297 UG. We observed the intervening ISM material along the sightline to epsilon Per and present initial characterization of the column densities, temperature, and kinematics of atomic and molecular species in the observation.

  16. VizieR Online Data Catalog: Abundances in the local region. II. F, G, and K dwarfs (Luck+, 2017)

    Science.gov (United States)

    Luck, R. E.

    2017-06-01

    The McDonald Observatory 2.1m Telescope and Sandiford Cassegrain Echelle Spectrograph provided much of the observational data for this study. High-resolution spectra were obtained during numerous observing runs, from 1996 to 2010. The spectra cover a continuous wavelength range from about 484 to 700nm, with a resolving power of about 60000. The wavelength range used demands two separate observations--one centered at about 520nm, and the other at about 630nm. Typical S/N values per pixel for the spectra are more than 150. Spectra of 57 dwarfs were obtained using the Hobby-Eberly telescope and High-Resolution Spectrograph. The spectra have a resolution of 30000, spanning the wavelength range of 400 to 785nm. They also have very high signal-to-noise ratios, >300 per resolution element in numerous cases. The last set of spectra were obtained from the ELODIE Archive (Moultaka et al. 2004PASP..116..693M). These spectra are fully processed, including order co-addition, and have a continuous wavelength span of 400 to 680nm and a resolution of 42000. The ELODIE spectra utilized here all have S/N>75 per pixel. (6 data files).

  17. From laboratory to the sky: Th-Ar wavelength standards for the cryogenic infrared echelle spectrograph (CRIRES)

    Energy Technology Data Exchange (ETDEWEB)

    Kerber, Florian; Bristow, Paul [European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching (Germany); Nave, Gillian; Sansonetti, Craig J [National Institute of Standards and Technology, Gaithersburg, MD (United States)], E-mail: fkerber@eso.org, E-mail: gillian.nave@nist.gov, E-mail: craig.sansonetti@nist.gov, E-mail: bristowp@eso.org

    2009-05-15

    We report on the collaborative effort of the European Southern Observatory (ESO) and the National Institute of Standards and Technology (NIST) to establish-through laboratory measurements-wavelength standards in the near-infrared (IR) emission line spectrum of a low current Th-Ar hollow cathode lamp. These standards are now routinely used for the wavelength calibration of the cryogenic infrared echelle spectrograph (CRIRES) operated at one of the unit telescopes of the very large telescope (VLT) at ESO's La Silla Paranal Observatory in Chile. The availability of highly accurate wavelength standards from a commercially available calibration source permits a shift to a new operational paradigm for high-resolution IR spectroscopy. Wavelength calibration no longer has to rely on atmospheric features but can make use of laboratory traceable reference data as is normally done in the ultraviolet and visible regions. This opens the door for more quantitative spectroscopic work in the near-IR. To illustrate the potential impact of this development, we briefly review the current state of affairs in IR astronomy and its projected future. With the advent of the next generation of extremely large ground-based telescopes the IR region will become the most powerful window on the universe within the next 10-15 years. We conclude with a short outlook on the contribution atomic physics can make to this evolution.

  18. Spectrometer system using a modular echelle spectrograph and a laser-driven continuum source for simultaneous multi-element determination by graphite furnace absorption spectrometry

    Energy Technology Data Exchange (ETDEWEB)

    Geisler, Sebastian; Okruss, Michael; Becker-Ross, Helmut; Huang, Mao Dong, E-mail: huang@isas.de; Esser, Norbert; Florek, Stefan

    2015-05-01

    A multi-element absorption spectrometer system has been developed based on a laser-driven xenon continuum source and a modular simultaneous echelle spectrograph (MOSES), which is characterized by a minimized number of optical components resulting in high optical throughput, high transmittance and high image quality. The main feature of the new optical design is the multifunction usage of a Littrow prism, which is attached on a rotation stage. It operates as an order-sorter for the echelle grating in a double-pass mode, as a fine positioning device moving the echelle spectrum on the detector, and as a forwarder to address different optical components, e.g., echelle gratings, in the setup. Using different prisms, which are mounted back to back on the rotation stage, a multitude of different spectroscopic modes like broad-range panorama observations, specific UV–VIS and NIR studies or high resolution zoom investigations of variable spectral channels can be realized. In the UV panorama mode applied in this work, MOSES has simultaneously detectable wavelength coverage from 193 nm to 390 nm with a spectral resolution λ/Δλ of 55,000 (3-pixel criterion). In the zoom mode the latter can be further increased by a factor of about two for a selectable section of the full wavelength range. The applicability and the analytical performance of the system were tested by simultaneous element determination in a graphite furnace, using eight different elements. Compared to an instrument operating in the optimized single line mode, the achieved analytical sensitivity using the panorama mode was typically a factor of two lower. Using the zoom mode for selected elements, comparable sensitivities were obtained. The results confirm the influence of the different spectral resolutions. - Highlights: • Echelle spectrometer with a full frame CCD array detector • High and variable spectral resolution from λ/Δλ of 55,000 to 95,000 • Laser-driven continuum light source

  19. Echelle observations of the spatially resolved kinematics of a region with high-speed motions in M17 (NGC 6618)-II

    International Nuclear Information System (INIS)

    Meaburn, J.; Clayton, C.A.

    1987-01-01

    In a previous paper the authors reported the discovery of a 'jet' of ionized gas ≅ 2 arcsec across emerging from a dark area of M17 with approaching speeds up to 115 km s -1 . The vicinity of this jet has now been observed in detail in the light of [O III] 5007 A with the Manchester echelle, with a five-element multi-slit, on the Isaac Newton Telescope. A variety of new high-speed phenomena has been discovered in the ionized gas. (author)

  20. Binary-induced magnetic activity?. Time-series echelle spectroscopy and photometry of HD 123351 = CZ CVn

    Science.gov (United States)

    Strassmeier, K. G.; Carroll, T. A.; Weber, M.; Granzer, T.; Bartus, J.; Oláh, K.; Rice, J. B.

    2011-11-01

    Context. Multi-wavelength time-series observations with high cadence and long duration are needed to resolve and understand the many variations of magnetically active late-type stars, which is an approach often used to observe the Sun. Aims: We present a first and detailed study of the bright and active K0IV-III star HD 123351. Methods: We acquired a total of 955 high-resolution STELLA echelle spectra during the years 2006-2010 and a total of 2260 photometric VIC data points during 1998-2010. These data are complemented by some spectra from CFHT and KPNO. Results: The star is found to be a single-lined spectroscopic binary with a period of 147.8919 ± 0.0003 days and a large eccentricity of e = 0.8086 ± 0.0001. The rms of the orbital solution is just 47 m s-1, making it the most precise orbit ever obtained for an active binary system. The rotation period is constrained from long-term photometry to be 58.32 ± 0.01 days. It shows that HD 123351 is a very asynchronous rotator, rotating five times slower than the expected pseudo-synchronous value. Two spotted regions persisted throughout the 12 years of our observations. We interpret them as active longitudes on a differentially rotating surface with a ΔP/P of 0.076. Four years of Hα, Ca ii H&K and He i D3 monitoring identifies the same main periodicity as the photometry but dynamic spectra also indicate that there is an intermittent dependence on the orbital period, in particular for Ca ii H&K in 2008. Line-profile inversions of a pair of Zeeman sensitive/insensitive iron lines yield an average surface magnetic-flux density of 542 ± 72 G. The time series for 2008 is modulated by the stellar rotation as well as the orbital motion, such that the magnetic flux is generally weaker during times of periastron and that the chromospheric emissions vary in anti-phase with the magnetic flux. We also identify a broad and asymmetric lithium line profile and measure an abundance of log n(Li) = 1.70 ± 0.05. The star

  1. The high-resolution cross-dispersed echelle white-pupil spectrometer of the McDonald Observatory 2.7-m telescope

    Science.gov (United States)

    Tull, Robert G.; Macqueen, Phillip J.; Sneden, Christopher; Lambert, David L.

    1995-01-01

    A new high-resolution cross-dispersed echelle spectrometer has been installed at the coude focus of the McDonald Observatory 2.7-m telescope. Its primary goal was simultaneously to gather spectra over as much of the spectral range 3400 A to 1 micrometer as practical, at a resolution R identical with lambda/Delta lambda which approximately = 60,000 with signal-to-noise ratio of approximately 100 for stars down to magnitude 11, using 1-h exposures. In the instrument as built, two exposures are all that are needed to cover the full range. Featuring a white-pupil design, fused silica prism cross disperser, and folded Schmidt camera with a Tektronix 2048x2048 CCD used at either of two foci, it has been in regularly scheduled operation since 1992 April. Design details and performance are described.

  2. NanoVipa: a miniaturized high-resolution echelle spectrometer, for the monitoring of young stars from a 6U Cubesat

    Science.gov (United States)

    Bourdarot, G.; Le Coarer, E.; Bonfils, X.; Alecian, E.; Rabou, P.; Magnard, Y.

    2017-12-01

    We introduce to astrophysical instrumentation and space optics the use of virtually imaged phased array (VIPA) to shrink échelle spectrometers and/or increase their resolution. Here, we report on both a concept of an echelle spectrometer with resolution R=50{,}000 (@653nm), which fits a 6U nanosatellite platform ({{1U= 10 cm × 10 cm × 10 cm}}), and on our laboratory tests on a R=200{,}000 demonstrator. The outline of our paper is as follows: Sect. 1 introduces our concept of a 6U payload comprising an échelle spectrometer based on the VIPA. We present also the science cases of monitoring young stars, and the wider science landscape amenable with larger telescopes. Section 2 gives a more detailed description of the VIPA and of its implementation in a cross-dispersed spectrometer. Section 3 shows the first results at R=200{,}000 we already achieved at the Institut de Planétologie et d'Astrophysique de Grenoble (IPAG). Finally, Sect. 4 is a discussion on the remaining technical points to study.

  3. Advanced statistical analysis of laser-induced breakdown spectroscopy data to discriminate sedimentary rocks based on Czerny–Turner and Echelle spectrometers

    International Nuclear Information System (INIS)

    Zhu, Xiaoqin; Xu, Tao; Lin, Qingyu; Liang, Long; Niu, Guanghui; Lai, Hongjun; Xu, Mingjun; Wang, Xu; Li, Hua; Duan, Yixiang

    2014-01-01

    The correct identification of rock types is critical for understanding the origins and history of any particular rock body. Laser-induced breakdown spectroscopy (LIBS) has developed into an excellent analytical tool for geological materials research because of its numerous technical advantages compared with traditional methods. The coupling of LIBS with advanced multivariate analysis has received increasing attention because it facilitates the rapid processing of spectral information to differentiate and classify samples. In this study, we collected LIBS datasets for 16 sedimentary rocks from Triassic strata in Sichuan Basin. We compared the performance of two types of spectrometers (Czerny–Turner and Echelle) for classification of rocks using two advanced multivariate statistical techniques, i.e., partial least squares discriminant analysis (PLS-DA) and support vector machines (SVMs). Comparable levels of performance were achievable when using the two systems in the best signal reception conditions. Our results also suggest that SVM outperformed PLS-DA in classification performance. Then, we compared the results obtained when using pre-selected wavelength variables and broadband LIBS spectra as variable inputs. They provided approximately equivalent levels of performance. In addition, the rock slab samples were also analyzed directly after being polished. This minimized the analysis time greatly and showed improvement of classification performance compared with the pressed pellets. - Highlights: • SVM and PLS-DA were compared using two spectrometers to classify sedimentary rocks. • SVM combined with LIBS improved the classification accuracy compared with PLS-DA. • Minimal difference using pre-selected and broadband spectra as variable inputs • Improved classification performance achievable using polished rock slab samples

  4. VizieR Online Data Catalog: Abundances for all seven stars in Latham 1 (O'Connell+, 2016)

    Science.gov (United States)

    O'Connell, J. E.; Martens, K.; Frinchaboy, P. M.

    2017-03-01

    Observations for all target stars were obtained at McDonald Observatory with the Otto Struve 2.1m telescope instrumented with the Sandiford Cass Echelle Spectrometer (SES; R=λ/Δλ~60000) in 2013 and 2014 June. The spectrograph setup was centered near 6175Å in 2013 and 6375Å in 2014 with wavelength coverage spanning from ~5350-6560Å and ~5560-6750Å, respectively (see Table2 for observation dates and exposure times). (3 data files).

  5. X-ray study of the structure of polyethylene at the scale of 100-200 Angstrom; Etude par rayons X dela structure du polyethylene a l'echelle de 100-200 Angstrom

    Energy Technology Data Exchange (ETDEWEB)

    Belbeoch nee Goldsztein, B [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1958-06-15

    Information on the structure of polyethylene is deduced from a comparison of the results obtained by central diffusion and by other X-ray methods. The structure depends on the thermal and mechanical treatment to which the samples are subjected, as well as on the observation temperature. The central diffusion due to the heterogeneity of the material at the scale of 100-200 Angstrom is bound up with the presence of both the amorphous and crystalline phases. Stretched polythene shows a more or less regular succession of orderly and disorderly regions. When released it has a structure of recrystallisation preceded by 'amorphization'. (author) [French] Les informations sur la structure du polyethylene sont deduites de la confrontation des resultats obtenus par la diffusion centrale et par d'autres methodes de rayons X. La structure depend des traitements thermiques et mecaniques subis par les echantillons ainsi que la temperature d'observation. La diffusion centrale due a l'existence d'heterogeneites de la matiere a l'echelle 100-200 Angstrom est lie a la presence des deux phases amorphe et cristallisee. Le polyethylene etire comporte une succession plus ou moins reguliere de domaines ordonnes et desordonnes. Le polyethylene relaxe a une structure de recristallisation precedee d'une 'amorphisation'. (auteur)

  6. Fast, remote read-off for binary scale counters; Lecture rapide a distance d'echelles binaires de comptage; Bystraya peredacha na rasstoyanie pokazanij binarnykh pereschetnykh ustrojstv; Lectura rapida, a distancia, de escalas binarias

    Energy Technology Data Exchange (ETDEWEB)

    Brun, J C; Antoine, P; Corbe, G; Schiller, J G; Victor, C [Faculte des Sciences de Paris, Orsay (France)

    1962-04-15

    The author describes a device for the rapid, remote transfer of the information contained in a 2{sup 20} scaler. Transformation of the parallel number to a series number of one microsecond duration. Application for non-destructive reading of a counter group connected to a scintillation detector with 30 simultaneous channels. (author) [French] L'auteur decrit un dispositif de transfert rapide a distance de l'information contenue dans une echelle de 2{sup 20}. Transformation du nombre parallele en nombre serie d'une microseconde de duree. Application a la lecture non destructive d'un groupe de comptage lie a un ensemble de detection par scintillation a 30 voies simultanees. (author) [Spanish] El autor describe un dispositivo para transferir rapidamente, a distancia, la informacion contenida en una escala de 2{sup 20}. Transformacion de la cifra paralela en cifra serie de un microsegundo de duracion. Aplicacion a la lectura no destructiva de un grupo de contaje unido a un conjunto de deteccion por centelleo de 30 canales simultaneos. (author) [Russian] Opisan apparat bystroj peredachi na rasstoyanie informatsii, soderzhashchejsya v pereschetnoj skheme 2{sup 20}. Prevrashchenie parallel'nogo chisla v serijnoe proiskhodit v techenie mikrosekundy. Primenenie pri normal'noj peredache schetnoj gruppy, svyazannoj s sistemoj detektirovaniya pri pomoshchi stsintillyatsii na 30 odnovremennykh kanalakh. (author)

  7. Incrementando la calidad de los espectros echelle

    Science.gov (United States)

    Pintado, O. I.; Adelman, S. J.

    For more than 10 years we have obtained spectra with the REOSC and EBASIM spectrograph at CASLEO. Usually we use IRAF to extract the spectra. Then we normalized the 1-d spectra and measured the lines with REDUCE. In this paper we compare the results obtained using each program in different parts of the spectrum measurements process. Wih EBASIM, or 4th magnitude stars and 120 minute exposures we obtain signal-to-noise ratios near 500 in the center of the orders

  8. VizieR Online Data Catalog: Solar neighborhood. XXXVII. RVs for M dwarfs (Benedict+, 2016)

    Science.gov (United States)

    Benedict, G. F.; Henry, T. J.; Franz, O. G.; McArthur, B. E.; Wasserman, L. H.; Jao, W.-C.; Cargile, P. A.; Dieterich, S. B.; Bradley, A. J.; Nelan, E. P.; Whipple, A. L.

    2017-05-01

    , National optical astronomy observatory (WIYN) 3.5m (Horch et al. 2012, Cat. J/AJ/143/10). Where available, we use astrometric observations from HST instruments other than the FGSs, including the Faint Object Camera (FOC; Barbieri et al. 1996A&A...315..418B), the Faint Object Spectrograph (FOS; Schultz et al. 1998PASP..110...31S), the Near-Infrared Camera and Multi-Object Spectrometer (NICMOS; Golimowski et al. 2004AJ....128.1733G), and the Wide-Field Planetary Camera 2 (WFPC2; Schroeder et al. 2000AJ....119..906S; Dieterich et al. 2012, Cat. J/AJ/144/64). Our radial velocity measurements, listed in table3, are from two sources. We obtained most radial velocity data with the McDonald 2.1m Struve telescope and the Sandiford Cassegrain Echelle spectrograph, hereafter CE. The CE delivers a dispersion equivalent to 2.5km/s/pix (R=λ/Δλ=60000) with a wavelength range of 5500{<=}λ{<=}6700Å spread across 26 orders (apertures). The McDonald data were collected during 33 observing runs from 1995 to 2009. Some GJ 623 AB velocities came from the Hobby-Eberly Telescope (HET) using the Tull Spectrograph. (3 data files).

  9. The development of a cell-assembly for the treatment of irradiated fuels on a semi-industrial scale; Etude concernant la realisation d'un ensemble de cellules destinees a des traitements de combustibles irradies a l'echelle semi-industrielle

    Energy Technology Data Exchange (ETDEWEB)

    Faugeras, P; Couture, J; Lefort, G [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1961-07-01

    The main studies and experiments involved in the development of a cell-assembly for the treatment of irradiated fuels on a semi-industrial scale are described. It must be possible to modify or transform each of these cells without interrupting the rest of the pilot. A full-scale prototype cell (3 x 4 x 6 m) has been built with an {alpha}-protection independent of the {gamma}-protection. It features all the main characteristics: tightness to {gamma} losses, dense glass lighting, ventilation. This cell has made possible trials on transfer, remote-controls and tele-dismantling, as well as the development of new methods of rapidly connecting hydraulic circuits. In conclusion the final form is given of the cells selected for the pilot. (author) [French] Il est decrit les principales etudes et experiences faites en vue de la realisation d'un ensemble de cellules destinees a des traitements de combustibles irradies a l'echelle semi-industrielle. Chacune de ces cellules doit pouvoir etre modifiee ou transformee sans interrompre le reste du pilote. Une cellule prototype vraie grandeur (3x4x6 m) est construite avec une protection {alpha} independante de la protection {gamma}. Elle comporte tous les elements importants: porte {gamma} etanche, eclairage verre dense, ventilation. Cette cellule a permis des experiences de transferts de telemanipulateurs et de teledemontages, ainsi que la mise au point de nouveaux procedes de jonction rapide pour des circuits hydrauliques. En conclusion, on indique la forme definitive des cellules retenues pour le pilote. (auteur)

  10. Application of the geometrical theory of diffraction to Cassegrain subreflectors with laterally defocused feeds

    DEFF Research Database (Denmark)

    Sørensen, O.; Rusch, W.

    1975-01-01

    The geometrical theory of diffraction (GTD) as formulated by R. G. Kouyoumjian has been applied to predict the radiation characteristics of hyperboloidal subreflectors with laterally defocused feeds. In caustic or multicaustic directions the scattered fields are determined using an equivalent ring...... current placed along the edge of the subreflector. The theoretical results are compared to measured amplitude and phase data. In order to improve the agreement, the blocking effects of the feed horn have been accounted for using the geometrical theory of diffraction. The calculated subreflector fields...... have been used to illuminate a paraboloid from which the scattered field is determined by physical optics. The results are compared to those obtained using a laterally defocused equivalent paraboloid....

  11. The Open Cluster Chemical Abundances and Mapping (OCCAM) Survey: Optical Extension for Neutron Capture Elements

    Science.gov (United States)

    Melendez, Matthew; O'Connell, Julia; Frinchaboy, Peter M.; Donor, John; Cunha, Katia M. L.; Shetrone, Matthew D.; Majewski, Steven R.; Zasowski, Gail; Pinsonneault, Marc H.; Roman-Lopes, Alexandre; Stassun, Keivan G.; APOGEE Team

    2017-01-01

    The Open Cluster Chemical Abundance & Mapping (OCCAM) survey is a systematic survey of Galactic open clusters using data primarily from the SDSS-III/APOGEE-1 survey. However, neutron capture elements are very limited in the IR region covered by APOGEE. In an effort to fully study detailed Galactic chemical evolution, we are conducting a high resolution (R~60,000) spectroscopic abundance analysis of neutron capture elements for OCCAM clusters in the optical regime to complement the APOGEE results. As part of this effort, we present Ba II, La II, Ce II and Eu II results for a few open clusters without previous abundance measurements using data obtained at McDonald Observatory with the 2.1m Otto Struve telescope and Sandiford Echelle Spectrograph.This work is supported by an NSF AAG grant AST-1311835.

  12. The Open Cluster Chemical Abundances and Mapping (OCCAM) Survey: Current Status

    Science.gov (United States)

    Frinchaboy, Peter; O'Connell, Julia; Donor, John; Cunha, Katia; Thompson, Benjamin; Melendez, Matthew; Shetrone, Matthew; Zasowski, Gail; Majewski, Steven R.; APOGEE TEAM

    2018-01-01

    The Open Cluster Chemical Analysis and Mapping (OCCAM) survey aims to produce a comprehensive, uniform, infrared-based data set forhundreds of open clusters, and constrain key Galactic dynamical and chemical parameters using the SDSS/APOGEE survey and follow-up from the McDonald Observatory Otto Struve 2.1-m telescope and Sandiford Cass Echelle Spectrograph (R ~ 60,000). We report on multi-element radial abundance gradients obtained from a sample of over 30 disk open clusters. The APOGEE chemical abundances were derived automatically by the ASPCAP pipeline and these are part of the SDSS IV Data Release 14, optical follow-up were analyzed using equivalent width analysis and spectral synthesis. We present the current open cluster sample that spans a significant range in age allowing exploration of the evolution of the Galactic abundance gradients. This work is supported by an NSF AAG grants AST-1311835 & AST-1715662.

  13. A Multi-Scaler Recording System and its Application to Radiometric ''Off-Line'' Analysis; Systeme d'Enregistrement a Echelles de Comptage Multiples et son Appucation aux Analyses Radlometriques Hors Circuit; Mul'tiskalyarnaya registriruyushchaya sistema i ee primenenie k radiometricheskim i ''vnelinejnym'' analizam; Un Sistema de Registro de Multiples Escalimetros y su Aplicacion al Analisis Radiometrico Discontinuo

    Energy Technology Data Exchange (ETDEWEB)

    Bisby, H. [Atomic Energy Research Establishment, Harwell, Berks. (United Kingdom)

    1966-02-15

    have been reviewed and an example demonstrates the value of unitized instrumentation and a comprehensive, flexible data recording system. Possible future developments have been mentioned in data processing which could lead to a completely automatic service becoming available. (author) [French] Dans les grandes usines de traitement extremement complexes, on a fait un gros effort au cours des dernieres annees pour incorporer un appareillage dans le circuit de fabrication pour l'analyse des caracteristiques et des teneurs des matieres pendant le traitement. Toutefois, les appareils en question jouent un role qualitatif plutot que quantitatif dans la gestion generale de l'installation. Les donnees quantitatives indispensables pour la gestion et la comptabilite sont obtenues grace a une utilisation efficace des methodes et appareils de laboratoire pour l'analyse precise d'echantillons representatifs preleves sur les matieres dans le circuit de traitement. Ces techniques, notamment celles qui utilisent des dispositifs de comptage a impulsions, peuvent etre rendues automatiques grace a un appareillage moderne, tel que celui qui est decrit dans le memoire et qui permet d'obtenir des donnees sous une forme numerique a l'aide de memoires electroniques (echelles de comptage). Une grande installation doit disposer de nombreux appareils de comptage distincts de ce genre, dont chacun est surveille independamment et fonctionne donc sans aucune correlation dans le temps avec les autres. Le systeme d'enregistrement automatique expose dans le memoire comporte un dispositif de lecture des donnees commun a plus de cinquante appareils de comptage fonctionnant independamment les uns des autres; ce systeme enregistre les donnees relevees par les echelles de comptage et permet, en outre, d'identifier les ensembles echantillons/appareil et le temps absolu de chaque lecture. Les donnees peuvent etre enregistrees sous une forme qui facilite leur traitement ulterieur dans un ordinateur, sur

  14. Who Is Chester Cook? The Story Behind the Plaques on the 16-inch f/18 Cassegrain Cook Memorial Telescope

    Science.gov (United States)

    Sudaric Hillier, Anna

    2010-01-01

    How did the public telescope on the mall become dedicated to Chester Sheldon Cook? He was a mulitfacted individual with qualities to be a musician and optician. His musical ablities went hand in hand with his optical work at Harvard College Observatory. His interactions with Donald Menzel and James G. Baker are explored in this oral presentation.

  15. Large Eddy simulations of jet in cross flow; Simulations aux grandes echelles: application au jet transverse

    Energy Technology Data Exchange (ETDEWEB)

    Priere, C

    2005-01-15

    Nowadays, environmental and economic constraints require considerable research efforts from the gas turbine industry. Objectives aim at lowering pollutants emissions and fuel consumption. These efforts take a primary importance to satisfy a continue growth of energy production and to obey to stringent environmental legislations. Recorded progresses are linked to mixing enhancement in combustors running at lean premixed operating point. Indeed, industry shows itself to be attentive in the mixing enhancement and during the last years, efforts are concentrated on fresh and burned gas dilution. The Jet In Cross Flow (JICF), which constitutes a representative case to further the research effort. It has been to be widely studied both in experimentally and numerically, and is particularly well suited for the evaluation of Large Eddy Simulations (LES). This approach, where large scale phenomena are naturally taken into account in the governing equation while the small scales are modelled, offers the means to well-predict such flows. The main objective of this work is to gauge and to enhance the quality of the LES predictions in JICF configurations by means of numerical tools developed in the compressible AVBP code. Physical and numerical parameters considered in the JICF modelization are taken into account and strategies that are able to enhance quality of LES results are proposed. Configurations studied in this work are the following: - Influences of the boundary conditions and jet injection system on a free JICF - Study of static mixing device in an industrial gas turbine chamber. - Study of a JICF configuration represented a dilution zone in low emissions combustors. (author)

  16. A leap in scale for computers; Un saut d`echelle pour les calculateurs

    Energy Technology Data Exchange (ETDEWEB)

    Barenco, A; Ekert, A; Macchiavello, Ch; Sanpera, A [Oxford Univ. (United Kingdom)

    1996-11-01

    The peculiar laws of quantum physics may lead to an upheaval in computing and information processing. Digital computers deal with bits 0 or 1. Quantum mechanics may provide in theory q-bits, a coherent superposition of both states 0 and 1. A set of N q-bits can represent concomitantly up to 2{sup N} states. This superposition allows massively parallel computing. The ``universal quantum computer`` from Deutsch was the first report mentioning this possibility. The first quantum algorithm shows how to factorize big numbers with quantum computer. This is a big theoretical issue for cryptography unachievable with digital computers. The technical difficulty is to implement a quantum computer. The main barriers are interference, decoherence and information retrieval. But recent experimental studies gives new hints to build quantum logic circuits. (O.M.). 4 refs.

  17. Doped spin ladders under magnetic field; Echelles de spins dopees sous champ magnetique

    Energy Technology Data Exchange (ETDEWEB)

    Roux, G

    2007-07-15

    This thesis deals with the physics of doped two-leg ladders which are a quasi one-dimensional and unconventional superconductor. We particularly focus on the properties under magnetic field. Models for strongly correlated electrons on ladders are studied using exact diagonalization and density-matrix renormalization group (DMRG). Results are also enlightened by using the bosonization technique. Taking into account a ring exchange it highlights the relation between the pairing of holes and the spin gap. Its influence on the dynamics of the magnetic fluctuations is also tackled. Afterwards, these excitations are probed by the magnetic field by coupling it to the spin degree of freedom of the electrons through Zeeman effect. We show the existence of doping-dependent magnetization plateaus and also the presence of an inhomogeneous superconducting phase (FFLO phase) associated with an exceeding of the Pauli limit. When a flux passes through the ladder, the magnetic field couples to the charge degree of freedom of the electrons via orbital effect. The diamagnetic response of the doped ladder probes the commensurate phases of the t-J model at low J/t. Algebraic transverse current fluctuations are also found once the field is turned on. Lastly, we report numerical evidences of a molecular superfluid phase in the 3/2-spin attractive Hubbard model: at a density low enough, bound states of four fermions, called quartets, acquire dominant superfluid fluctuations. The observed competition between the superfluid and density fluctuations is connected to the physics of doped ladders. (author)

  18. KiwiSpec: The Design and Performance of a High Resolution Echelle Spectrograph for Astronomy

    Science.gov (United States)

    Gibson, Steven Ross

    This document describes the design, analysis, construction and testing of KiwiSpec, a fibre-fed, high resolution astronomical spectrograph of an asymmetric white pupil design. The instrument employs an R4, 31.6 groove mm-1 échelle grating for primary dispersion and a 725 lines mm-1 volume phase holographic (VPH) based grism for cross-dispersion. Two versions of the prototype were designed and constructed: an 'in-air' prototype, and a prototype featuring a vacuum chamber (to increase the stability of the instrument). The KiwiSpec optical design is introduced, as well as a description of the theory behind a cross-dispersed échelle spectrograph. The results of tolerancing the optical design are reported for alignment, optical fabrication, and optical surface quality groups of parameters. The optical windows of an iodine cell are also toleranced. The opto-mechanical mounts of both prototypes are described in detail, as is the design of the vacuum chamber system. Given the goal of 1 m/s radial velocity stability, analyses were undertaken to determine the allowable amount of movement of the vacuum windows, and to determine the allowable changes in temperature and pressure within and outside of the vacuum chamber. The spectral efficiency of the instrument was estimated through a predictive model; this was calculated for the as-built instrument and also for an instrument with ideal, high-efficiency coatings. Measurements of the spectral efficiency of various components of the instrument are reported, as well as a description of the measurement system developed to test the efficiency of VPH gratings. On-sky efficiency measurements from use of KiwiSpec on the 1-m McLellan telescope at Mt John University Observatory are reported. Two possible exposure meter locations are explored via an efficiency model, and also through the measurement of the zero-order reflectivity of the échelle grating. Various stability aspects of the design are investigated. These include the stability of the optical mounts with temperature changes, and also the effect of the expansion and contraction of the supporting optical tables. As well, the stability of the in-air prototype was determined through measurement of the movement of thorium-argon emission lines within spectra as the temperature, atmospheric pressure and relative humidity (naturally) varied. Current and planned testing for determining the stability of the vacuum chamber prototype is discussed.

  19. Radiations: large scale monitoring in Japan; Radiations: suivi a grande echelle au Japon

    Energy Technology Data Exchange (ETDEWEB)

    Linton, M.; Khalatbari, A.

    2011-10-15

    As the consequences of radioactive leaks on their health are a matter of concern for Japanese people, a large scale epidemiological study has been launched by the Fukushima medical university. It concerns the two millions inhabitants of the Fukushima Prefecture. On the national level and with the support of public funds, medical care and follow-up, as well as systematic controls are foreseen, notably to check the thyroid of 360.000 young people less than 18 year old and of 20.000 pregnant women in the Fukushima Prefecture. Some measurements have already been performed on young children. Despite the sometimes rather low measures, and because they know that some parts of the area are at least as much contaminated as it was the case around Chernobyl, some people are reluctant to go back home

  20. Large eddy simulation and combustion instabilities; Simulation des grandes echelles et instabilites de combustion

    Energy Technology Data Exchange (ETDEWEB)

    Lartigue, G.

    2004-11-15

    The new european laws on pollutants emission impose more and more constraints to motorists. This is particularly true for gas turbines manufacturers, that must design motors operating with very fuel-lean mixtures. Doing so, pollutants formation is significantly reduced but the problem of combustion stability arises. Actually, combustion regimes that have a large excess of air are naturally more sensitive to combustion instabilities. Numerical predictions of these instabilities is thus a key issue for many industrial involved in energy production. This thesis work tries to show that recent numerical tools are now able to predict these combustion instabilities. Particularly, the Large Eddy Simulation method, when implemented in a compressible CFD code, is able to take into account the main processes involved in combustion instabilities, such as acoustics and flame/vortex interaction. This work describes a new formulation of a Large Eddy Simulation numerical code that enables to take into account very precisely thermodynamics and chemistry, that are essential in combustion phenomena. A validation of this work will be presented in a complex geometry (the PRECCINSTA burner). Our numerical results will be successfully compared with experimental data gathered at DLR Stuttgart (Germany). Moreover, a detailed analysis of the acoustics in this configuration will be presented, as well as its interaction with the combustion. For this acoustics analysis, another CERFACS code has been extensively used, the Helmholtz solver AVSP. (author)

  1. Mapping the Heiles Supershell GSH 90-28-17

    Science.gov (United States)

    Montgomery, Sharon Lynn; Beckey, Jacob Lucas; Welsh, Barry; Kuehne, John W.

    2017-01-01

    Large-diameter shells of neutral gas called superbubbles were first detected by the 21-cm radio surveys of Heiles (1979,1984) and are likely formed by stellar winds and supernova explosions. Some of these interstellar voids (including GSH 90-28-17) span more than 10 degrees of the sky. However, only a few studies have been able to identify the power source of a particular Heiles shell. The problem is that HI 21cm emission can arise at all distances along a given sight-line, so while we many know the speed at which neutral gas is moving, we do not know the distance of this gas. Indeed, a given line of sight may penetrate multiple shell walls making the interpretation of the radio data very challenging.Here we report on an absorption study of the interstellar absorption lines of NaI, CaII, CaI, CH and CH+ detected towards nine stellar continuum sources with sight-line distances increasing from 90 pc to >1kpc in the direction of the supershell GSH 90-28-17. Our observations, recorded with the Sandiford echelle spectrograph on the 2.1m telescope at the McDonald Observatory (Texas) in August 2016, reveal gas components with velocities between -10 and -50 km/s orginating from distances >400 pc that we can associate with the expansion of the GSH 90-28-17 shell.

  2. The Open Cluster Chemical Abundances and Mapping (OCCAM) Survey: Galactic Neutron CaptureAbundance Gradients

    Science.gov (United States)

    O'Connell, Julia; Frinchaboy, Peter M.; Shetrone, Matthew D.; Melendez, Matthew; Cunha, Katia; Majewski, Steven R.; Zasowski, Gail; APOGEE Team

    2017-06-01

    The evolution of elements, as a function or age, throughout the Milky Way disk provides a key constraint for galaxy evolution models. In an effort to provide these constraints, we have conducted an investigation into the r- and s- process elemental abundances for a large sample of open clusters as part of an optical follow-up to the SDSS-III/APOGEE-1 survey. Stars were identified as cluster members by the Open Cluster Chemical Abundance & Mapping (OCCAM) survey, which culls member candidates by radial velocity, metallicity and proper motion from the observed APOGEE sample. To obtain data for neutron capture elements in these clusters, we conducted a long-term observing campaign covering three years (2013-2016) using the McDonald Observatory Otto Struve 2.1-m telescope and Sandiford Cass Echelle Spectrograph (R ~ 60,000). We present Galactic neutron capture abundance gradients using 30+ clusters, within 6 kpc of the Sun, covering a range of ages from ~80 Myr to ~10 Gyr .

  3. Chemical Abundance Analysis of Moving Group W11450 (Latham 1)

    Science.gov (United States)

    O'Connell, Julia E.; Martens, Kylee; Frinchaboy, Peter M.

    2016-12-01

    We present elemental abundances for all seven stars in Moving Group W11450 (Latham 1) to determine if they may be chemically related. These stars appear to be both spatially and kinematically related, but no spectroscopic abundance analysis exists in literature. Abundances for eight elements were derived via equivalent width analyses of high-resolution (R ˜ 60,000), high-signal-to-noise ratio ( ˜ 100) spectra obtained with the Otto Struve 2.1 m telescope and the Sandiford Echelle Spectrograph at McDonald Observatory. The large star-to-star scatter in metallicity, -0.55 ≤ [Fe/H] ≤slant 0.06 dex (σ = 0.25), implies these stars were not produced from the same chemically homogeneous molecular cloud, and are therefore not part of a remnant or open cluster as previously proposed. Prior to this analysis, it was suggested that two stars in the group, W11449 and W11450, are possible wide binaries. The candidate wide binary pair show similar chemical abundance patterns with not only iron but with other elements analyzed in this study, suggesting the proposed connection between these two stars may be real.

  4. Nessie - A versatile multi-fiber feed on the KPNO Mayall 4-meter telescope

    Science.gov (United States)

    Barden, Samuel C.; Massey, Philip

    A multi-fiber instrument utilizing the KPNO 4-meter Lockheed Cassegrain Camera as plate holder for fiber-optic plugboards is described. Up to 49 fibers can be positioned on objects in a 40 arc-minute field of view with a minimum separation of 50 arc-seconds. The plugboards, made of Benalex, hold the fibers normal to the flat plane for better alignment with the telescope pupil, but at a depth which follows the curvature of the focal plane. Two 20 meter cables exist, one for optimal observations in the blue, the other for observations redward of 7000 A. These cables feed the light into the Cryocam, the RC spectrograph, or the Echelle which are located in the large coude room during the observations. Sample observations are presented along with some evaluation of the system stability due to the spectrograph being removed from the telescope. A review of the problems in the astrometry for the plates is also given.

  5. VizieR Online Data Catalog: The G+M eclipsing binary V530 Orionis photometry (Torres+, 2014)

    Science.gov (United States)

    Torres, G.; Lacy, C. H. S.; Pavlovski, K.; Feiden, G. A.; Sabby, J. A.; Bruntt, H.; Clausen, J. V.

    2017-08-01

    V530 Ori was monitored spectroscopically with three different instruments over a period of more than 17 yr. Observations began at the Harvard-Smithsonian Center for Astrophysics (CfA) in 1996 June with a Cassegrain-mounted echelle spectrograph ("Digital Speedometer", DS; Latham 1992ASPC...32..110L) attached to the 1.5 m Tillinghast reflector at the F. L. Whipple Observatory (Mount Hopkins, AZ). We gathered a further 30 spectra of V530 Ori at the Kitt Peak National Observatory (KPNO) from 1999 March to 2001 January, using the coude-feed telescope and the coude spectrometer. Finally, 41 additional observations were obtained at the CfA from 2009 November to 2014 March with the Tillinghast Reflector Echelle Spectrograph (TRES; Furesz 2008, PhD thesis , Univ. Szeged, Hungary) on the 1.5 m telescope mentioned earlier. Two sets of V-band images of V530 Ori were obtained with independent robotic telescopes operating at the University of Arkansas (URSA WebScope) and near Silver City, NM (NFO WebScope) from 2001 January to 2012 February. Differential photometric measurements of V530 Ori were also gathered with the Stromgren Automatic Telescope at ESO (La Silla, Chile), during several campaigns from 2001 January to 2006 February. (5 data files).

  6. Modelling of fractured reservoirs. Case of multi-scale media; Modelisation des reservoirs fractures. Cas des milieux multi-echelles

    Energy Technology Data Exchange (ETDEWEB)

    Henn, N.

    2000-12-13

    Some of the most productive oil and gas reservoirs are found in formations crossed by multi-scale fractures/faults. Among them, conductive faults may closely control reservoir performance. However, their modelling encounters numerical and physical difficulties linked with (a) the necessity to keep an explicit representation of faults through small-size grid blocks, (b) the modelling of multiphase flow exchanges between the fault and the neighbouring medium. In this thesis, we propose a physically-representative and numerically efficient modelling approach in order to incorporate sub-vertical conductive faults in single and dual-porosity simulators. To validate our approach and demonstrate its efficiency, simulation results of multiphase displacements in representative field sector models are presented. (author)

  7. Statewide evaluation of pay-for-use metering; Evaluation a l'echelle nationale du comptage en pre-paiement

    Energy Technology Data Exchange (ETDEWEB)

    D' Zurko, D C [New York Gas Group, (United States); Landsberg, D [Landsberg Engineering, P.C., (United States)

    2000-07-01

    To gain a better understanding of how best to deploy Pay-for-Use Metering technology in New York State, a consortium of eight natural gas and electric utilities conducted a feasibility study through their natural gas trade association, the New York Gas Group (NYGAS). As a result of the completed study and ongoing dialogue among utility service providers and regulators, benefits, challenges and test scenarios have been identified. During the transition to fully deregulated gas and electric industries, the regulated Local Distribution Companies (LDCs) must continue to provide service to the low-margin customers and those that are less profitable as the 'Supplier of Last Resort' (SOLR). PFU Metering has demonstrated that the consumer can save energy ranging from 5% to 20% based on the greater awareness of energy usage and associated costs. It can also turn a payment troubled customer into a good customer, making him attractive to all energy providers. For some residents who are no longer entitled to utility service due to default on deposit requirements or payment arrangements, it provides an alternative to receive energy that otherwise would not be possible. The goal of a multi-utility pilot test is to verify in varying conditions the reported benefits, change in consumer payment behavior, and projected economics. Based on evaluation during the pilot test and continuing interaction with the NYS regulators, it is likely that new procedures will be developed for full and successful implementation of PFU metering by regulated LDCs. (authors)

  8. Pages 524 - 529.pmd

    African Journals Online (AJOL)

    Administrator

    6):101-105. 12. Culei I. Methodology for the analysis of vegetable drugs: Practical Manual on the industrial. Utilisation of Medicinal and Aromatic Plants. 1st ed. Romania: Center Building, 1982. 13. Nayak SB, Sandiford S, Maxwell A. Evaluation.

  9. HARPS3 for a roboticized Isaac Newton Telescope

    Science.gov (United States)

    Thompson, Samantha J.; Queloz, Didier; Baraffe, Isabelle; Brake, Martyn; Dolgopolov, Andrey; Fisher, Martin; Fleury, Michel; Geelhoed, Joost; Hall, Richard; González Hernández, Jonay I.; ter Horst, Rik; Kragt, Jan; Navarro, Ramón; Naylor, Tim; Pepe, Francesco; Piskunov, Nikolai; Rebolo, Rafael; Sander, Louis; Ségransan, Damien; Seneta, Eugene; Sing, David; Snellen, Ignas; Snik, Frans; Spronck, Julien; Stempels, Eric; Sun, Xiaowei; Santana Tschudi, Samuel; Young, John

    2016-08-01

    We present a description of a new instrument development, HARPS3, planned to be installed on an upgraded and roboticized Isaac Newton Telescope by end-2018. HARPS3 will be a high resolution (R≃115,000) echelle spectrograph with a wavelength range from 380-690 nm. It is being built as part of the Terra Hunting Experiment - a future 10- year radial velocity measurement programme to discover Earth-like exoplanets. The instrument design is based on the successful HARPS spectrograph on the 3.6m ESO telescope and HARPS-N on the TNG telescope. The main changes to the design in HARPS3 will be: a customised fibre adapter at the Cassegrain focus providing a stabilised beam feed and on-sky fibre diameter ≍1:4 arcsec, the implementation of a new continuous ow cryostat to keep the CCD temperature very stable, detailed characterisation of the HARPS3 CCD to map the effective pixel positions and thus provide an improved accuracy wavelength solution, an optimised integrated polarimeter and the instrument integrated into a robotic operation. The robotic operation will optimise our programme which requires our target stars to be measured on a nightly basis. We present an overview of the entire project, including a description of our anticipated robotic operation.

  10. VizieR Online Data Catalog: Spectroscopic and photometric properties of Tombaugh 1 (Sales+, 2016)

    Science.gov (United States)

    Sales Silva, J. V.; Carraro, G.; Anthony-Twarog, B. J.; Moni Bidin, C.; Costa, E.; Twarog, B. A.

    2018-03-01

    Photometry for Tombaugh 1 was secured in 2010 December during a five-night run using the Cerro Tololo Inter-American Observatory 1.0 m telescope operated by the SMARTS consortium (http://www.astro.yale.edu/smarts). The telescope is equipped with an STA 4064x4064 CCD camera (http://www.astronomy.ohio-state.edu/Y4KCam/detector) with 15 μm pixels, yielding a scale of 0.289"/pixel and a field of view (FOV) of 20'x20' at the Cassegrain focus of the telescope. Over the night of 2010 January 5, we observed 10 potential cluster stars (nine clump stars and one Cepheid; see Section 4.1) with the Inamori-Magellan Areal Camera & Spectrograph (IMACS; Dressler et al. 2006SPIE.6269E..0FD) attached to the Magellan telescope (6.5 m) located at Las Campanas, Chile. The spectra were obtained using the Multi-Object Echelle (MOE) mode with two exposures, one of 900 s and the other of 1200 s. Our spectra have a resolution of R~20000, while the spectral coverage depends on the location of the star on the multislit mask, but it generally goes from 4200 to 9100 Å. The detector consists of a mosaic with eight CCDs with gaps of about 0.93 mm between the CCDs, causing small gaps in stellar spectra. (7 data files).

  11. Large scale simulation numerical study of transition to turbulence in jets; Etude numerique par simulation des grandes echelles de la transition a la turbulence dans les jets

    Energy Technology Data Exchange (ETDEWEB)

    Urbin, Gerald [Institut National Polytechnique, 38 - Grenoble (France)

    1998-02-02

    This study highlights the potentialities of the numerical technique of large scale simulation in describing and understanding the turbulent flows in a complex geometry. Particularly, it is focussed on flows of free jet, confined jets and multiple jets of high solidity grid. Spatial simulations of the circular zone close to a free jet, of high Reynolds number were performed. In spite of an evident sensitivity to upstream conditions good agreement between our statistical predictions and different experimental measurements was obtained. The multiple coherent vortical structures implied in the transition to turbulence of the jet were found. At the same time, helical or annular axisymmetric vortices were observed. Also, an original vortical arrangement was evidenced, resulting from the alternating inclination and local pairing of these rings. It could been forced through an ad-hoc excitation which modifies subsequently drastically the jet development. When an axisymmetric excitation is imposed after formation of annular structures, pairs of counter-rotative longitudinal vortices occur and generate lateral jets. Their nature and presence in case of a helical excitation are discussed. An efficient method for controlling their number is developed. Then, one is studied the very low frequency periodic phenomenon of backward-facing transition to turbulence which develops in the confined jet and grid multiple jets (a phenomenon generic in numerous flows). It was found to depend not only on the characteristic of the re-circulation (pre-transition) zones but also on the upstream flow (zone of post-transition stagnation, pressure effect). Large scale transversal motions of the fluid have been found beginning from the grid. An interpretation of this phenomenon is suggested 193 refs., 109 figs.

  12. Multi scale study of carbon deposits collected in Tore-Supra and TEXTOR tokamaks; Etude multi echelle des depots carbones collectes dans les tokamaks Tore Supra et TEXTOR

    Energy Technology Data Exchange (ETDEWEB)

    Richou, M

    2007-06-15

    Tokamaks are devices aimed at studying magnetic fusion. They operate with high temperature plasmas containing hydrogen, deuterium or tritium. One of the major issue is to control the plasma-wall interaction. The plasma facing components are most often in carbon. The major drawback of carbon is the existence of carbon deposits and dust, due to erosion. Dust is potentially reactive in case of an accidental opening of the device. These deposits also contain H, D or T and induce major safety problems when tritium is used, which will be the case in ITER. Therefore, the understanding of the deposit formation and structure has become a main issue for fusion researches. To clarify the role of the deposits in the retention phenomenon, we have done different complementary characterizations for deposits collected on similar places (neutralizers) in tokamaks Tore Supra (France) and TEXTOR (Germany). Accessible microporous volume and pore size distribution of deposits has been determined with the analysis of nitrogen and methane adsorption isotherms using the BET, Dubinin-Radushkevich and {alpha}{sub s} methods and the Density Functional Theory (DFT). To understand growth mechanisms, we have studied the deposit structure and morphology. We have shown using Transmission Electron Microscopy (TEM) and Raman micro-spectrometry that these deposits are non amorphous and disordered. We have also shown the presence of nano-particles (diameter between 4 and 70 nm) which are similar to carbon blacks: nano-particle growth occurs in homogeneous phase in the edge plasma. We have emphasised a dual growth process: a homogenous and a heterogeneous one. (author)

  13. Modeling of atmospheric pollution at the regional scale: application to the Esquif campaign; Modelisation a l'echelle regionale de la pollution atmospherique: application a la campagne Esquif

    Energy Technology Data Exchange (ETDEWEB)

    Sarrat, C

    2003-06-01

    The Esquif experimental campaign (study and simulation of air quality in Ile-de-France (Paris region, France)) took place between 1998 and 2000 with the aim of better understanding the dynamical and chemical processes leading to atmospheric pollution peaks in Paris. The construction of a rich and diversified database (12 periods of intensive monitoring (PIM)) has been implemented with the aim of improving the existing chemical-transport models in general and air quality forecasting models in particular. In the framework of this study, the data collected during PIM 2 and 6 were used for the validation and analysis of situations of intensive pollution, simulated with the meso-scale numerical meteorological and chemical model Meso-NHC. The validation of both the dynamic fields (temperature and potential temperature, wind, height of the boundary layer) and the chemical fields (mainly O{sub 3}, NO{sub x}, NO{sub y}, PAN, isoprene) of the model allows to discuss some of the parameters of the model such as the initialization, the boundary forcing and the resolution. Then, a study of the dynamical processes allows to analyze the formation and reinforcement of the pollution conditions. Stress is put on the interaction of the regional scale processes with the photochemical pollution events. In this framework, the dynamical-chemical interaction processes are analyzed in detail, in particular when pollution levels are reinforced by the intrusion of residual ozone inside the convective boundary layer, dragged by the turbulence. Also, the impact of the urban hot island and of the urban wind on the redistribution of primary and secondary pollutants are considered. An analysis of the impact of hydrocarbons of biogenic origin on the ozone concentrations with respect to the temperature and to the presence of primary compounds has been performed for the PIM 2 and 6 of the Esquif campaign. (J.S.)

  14. Transport of particles in liquid foams: a multi-scale approach; Etude multi-echelles du transport de particules dans les mousses liquides

    Energy Technology Data Exchange (ETDEWEB)

    Louvet, N.

    2009-11-15

    Foam is used for the decontamination of radioactive tanks since foam is a system that has a large surface for a low amount of liquid and as a consequence requires less water to be decontaminated. We study experimentally different particle transport configurations in fluid micro-channels network (Plateau borders) of aqueous foam. At first, foam permeability is measured at the scale of a single channel and of the whole foam network for 2 soap solutions known for their significant different interface mobility. Experimental data are well described by a model that takes into account the real geometry of the foam and by considering a constant value of the Boussinesq number of each soap solutions. Secondly, the velocity of one particle convected in a single foam channel is measured for different particle/channel aspect ratio. For small aspect ratio, a counterflow that is taking place at the channel's corners slows down the particle. A recirculation model in the channel foam films is developed to describe this effect. To do this, the Gibbs elasticity is introduced. Then, the threshold between trapped and released of one particle in liquid foam are carried out. This threshold is deduced from hydrodynamic and capillary forces equilibrium. Finally, the case of a clog foam node is addressed. (author)

  15. Greenhouse gases regional fluxes estimated from atmospheric measurements; Estimation des flux de gaz a effet de serre a l'echelle regionale a partir de mesures atmospheriques

    Energy Technology Data Exchange (ETDEWEB)

    Messager, C

    2007-07-15

    build up a new system to measure continuously CO{sub 2} (or CO), CH{sub 4}, N{sub 2}O and SF{sub 6} mixing ratios. It is based on a commercial gas chromatograph (Agilent 6890N) which have been modified to reach better precision. Reproducibility computed with a target gas on a 24 hours time step gives: 0.06 ppm for CO{sub 2}, 1.4 ppb for CO, 0.7 ppb for CH{sub 4}, 0.2 ppb for N{sub 2}O and 0.05 ppt for SF{sub 6}. The instrument's run is fully automated, an air sample analysis takes about 5 minutes. In July 2006, I install instrumentation on a telecommunication tall tower (200 m) situated near Orleans forest in Trainou, to monitor continuously greenhouse gases (CO{sub 2}, CH{sub 4}, N{sub 2}O, SF{sub 6}), atmospheric tracers (CO, Radon-222) and meteorological parameters. Intake lines were installed at 3 levels (50, 100 and 180 m) and allow us to sample air masses along the vertical. Continuous measurement started in January 2007. I used Mace Head (Ireland) and Gif-sur-Yvette continuous measurements to estimate major greenhouse gases emission fluxes at regional scale. To make the link between atmospheric measurements and surface fluxes, we need to quantify dilution due to atmospheric transport. I used Radon-222 as tracer (radon tracer method) and planetary boundary layer heights estimates from ECMWF model (boundary layer budget method) to parameterize atmospheric transport. In both cases I compared results to available emission inventories. (author)

  16. Up scaling two-phase flow in heterogeneous porous media; Mise a l'echelle des ecoulements diphasiques dans les milieux poreux heterogenes

    Energy Technology Data Exchange (ETDEWEB)

    Artus, V.

    2003-11-01

    For two-phase flow in heterogeneous media, the emergence of different flow regimes at large-scale is driven by local interactions between the viscous coupling and the heterogeneity. In particular, when the viscosity ratio is favorable, viscous effects induce a transverse flow that stabilizes the front while flooding. However, most of recent stochastic models neglect the influence of the viscous coupling. We developed a stochastic model for the dynamics of the front, taking the viscous coupling into account. For stable cases, this model relates the statistical properties of the front to the statistical properties of the permeability field. For stable flow in stratified media, we show that the front is stationary by parts in the reservoir. These parts can be identified as large-scale hydrodynamic layers and separately coarsened in the large-scale simulation model. For flows with favorable viscosity ratios in isotropic reservoirs, we show that a stationary front occurs, in a statistical sense. For unfavorable viscosity ratios, the flow is driven by the development of viscous fingering. These different regimes lead to different large-scale saturation profiles that can be matched with a macro-dispersion equation, if the effective convective flux is modified to take into account stabilizing or destabilizing viscous effects. (author)

  17. Greenhouse gases regional fluxes estimated from atmospheric measurements; Estimation des flux de gaz a effet de serre a l'echelle regionale a partir de mesures atmospheriques

    Energy Technology Data Exchange (ETDEWEB)

    Messager, C

    2007-07-15

    build up a new system to measure continuously CO{sub 2} (or CO), CH{sub 4}, N{sub 2}O and SF{sub 6} mixing ratios. It is based on a commercial gas chromatograph (Agilent 6890N) which have been modified to reach better precision. Reproducibility computed with a target gas on a 24 hours time step gives: 0.06 ppm for CO{sub 2}, 1.4 ppb for CO, 0.7 ppb for CH{sub 4}, 0.2 ppb for N{sub 2}O and 0.05 ppt for SF{sub 6}. The instrument's run is fully automated, an air sample analysis takes about 5 minutes. In July 2006, I install instrumentation on a telecommunication tall tower (200 m) situated near Orleans forest in Trainou, to monitor continuously greenhouse gases (CO{sub 2}, CH{sub 4}, N{sub 2}O, SF{sub 6}), atmospheric tracers (CO, Radon-222) and meteorological parameters. Intake lines were installed at 3 levels (50, 100 and 180 m) and allow us to sample air masses along the vertical. Continuous measurement started in January 2007. I used Mace Head (Ireland) and Gif-sur-Yvette continuous measurements to estimate major greenhouse gases emission fluxes at regional scale. To make the link between atmospheric measurements and surface fluxes, we need to quantify dilution due to atmospheric transport. I used Radon-222 as tracer (radon tracer method) and planetary boundary layer heights estimates from ECMWF model (boundary layer budget method) to parameterize atmospheric transport. In both cases I compared results to available emission inventories. (author)

  18. Turbulent viscosity and scale laws in turbulent jets with variable density; Viscosite turbulente et lois d`echelles dans les jets turbulents a masse volumique variable

    Energy Technology Data Exchange (ETDEWEB)

    Pietri, L.; Amielh, M.; Anselmet, F.; Fulachier, L. [Institut de Recherche sur les Phinomenes Hors Equilibre Equipe Turbulence, 13 - Marseille (France)

    1997-12-31

    Turbulent flows with strong density variations, like helium jets in the ambient air, have specific properties linked with the difference of gas densities. This paper presents some experimental results of turbulence properties inside such flows: the Reynolds tensions and the associated turbulent viscosity, and some characteristics linked with the statistical properties of the different turbulence scales. These last results allows to show the complexity of such flows characterized by the influence of external parameters (Reynolds number, initial density ratio, initial momentum flux) that govern the evolution of these parameters inside the jet from the nozzle up to regions where similarity properties are reached. (J.S.) 12 refs.

  19. Study of the permeability up-scaling by direct filtering of geostatistical model; Etude du changement d'echelle des permeabilites par filtrage direct du modele geostatistique

    Energy Technology Data Exchange (ETDEWEB)

    Zargar, G

    2005-10-15

    In this thesis, we present a new approach, which consists in directly up-scaling the geostatistical permeability distribution rather than the individual realizations. Practically, filtering techniques based on. the FFT (Fast Fourier Transform), allows us to generate geostatistical images, which sample the up-scaled distributions. In the log normal case, an equivalence hydraulic criterion is proposed, allowing to re-estimate the geometric mean of the permeabilities. In the anisotropic case, the effective geometric mean becomes a tensor which depends on the level of filtering used and it can be calculated by a method of renormalisation. Then, the method was generalized for the categorial model. Numerical tests of the method were set up for isotropic, anisotropic and categorial models, which shows good agreement with theory. (author)

  20. Statewide evaluation of pay-for-use metering; Evaluation a l'echelle nationale du comptage en pre-paiement

    Energy Technology Data Exchange (ETDEWEB)

    D' Zurko, D.C. [New York Gas Group, (United States); Landsberg, D. [Landsberg Engineering, P.C., (United States)

    2000-07-01

    To gain a better understanding of how best to deploy Pay-for-Use Metering technology in New York State, a consortium of eight natural gas and electric utilities conducted a feasibility study through their natural gas trade association, the New York Gas Group (NYGAS). As a result of the completed study and ongoing dialogue among utility service providers and regulators, benefits, challenges and test scenarios have been identified. During the transition to fully deregulated gas and electric industries, the regulated Local Distribution Companies (LDCs) must continue to provide service to the low-margin customers and those that are less profitable as the 'Supplier of Last Resort' (SOLR). PFU Metering has demonstrated that the consumer can save energy ranging from 5% to 20% based on the greater awareness of energy usage and associated costs. It can also turn a payment troubled customer into a good customer, making him attractive to all energy providers. For some residents who are no longer entitled to utility service due to default on deposit requirements or payment arrangements, it provides an alternative to receive energy that otherwise would not be possible. The goal of a multi-utility pilot test is to verify in varying conditions the reported benefits, change in consumer payment behavior, and projected economics. Based on evaluation during the pilot test and continuing interaction with the NYS regulators, it is likely that new procedures will be developed for full and successful implementation of PFU metering by regulated LDCs. (authors)

  1. Echelles de temps et échelles d’objets dans l’histoire de la grammaire française

    Directory of Open Access Journals (Sweden)

    Auroux Sylvain

    2012-07-01

    Full Text Available Les historiens ont coutume d’enraciner leur discipline dans le « récit » et, par conséquent, d’admettre que la « ligne » de l’histoire est celle d’une temporalité linéaire à quoi se résume la chronologie. Les historiens des sciences ont le plus souvent suivi cette tendance générale, et, cela, pour deux raisons principales. D’abord, ils ont suivi la tentation d’une « histoire » des grands hommes de science et, donc, de la suite des générations. Ensuite, la science est un processus dont on attend non seulement un résultat, mais une suite de résultats. Comme « science » nous n’aurions pas la même représentation de la physique si nous n’étions pas capables de faire une liste de « découvertes ». Je ne connais pas une science humaine qui dispose d’une pareille représentation, même si, sur de courtes périodes, et sur des objets précis on peut en approcher (par exemple en linguistique avec les lois de la grammaire comparée. Quand on se trouve devant une « histoire-récit » de la grammaire française, on se trouve le plus souvent confronté à une série (plus ou moins complète d’auteurs et d’ouvrages. Même si on peut parfois l’inférer à la lecture du texte on ne trouve guère de datation, et surtout pas de listes d’ « inventions » ; on ne suit pas des thématiques qui évolueraient comme dans la physique. Tout ce que l’on admet généralement, c’est le progrès quantitatif des phénomènes abordés et des règles, ou de grands changements théoriques qui rendraient caduques les études antérieures. La grammaire française serait-elle une discipline chaotique qui ne relève d’aucun processus de cumulation ? Nous nous proposons, plutôt que de juger une discipline en tirant des conclusions qui relèvent clairement du choix d’un modèle particulier (le « récit » pour l’histoire, d’interroger ce modèle à partir d’une étude des propriétés de notre objet, la grammaire française.

  2. ORIENTATION RELATIONNELLE VERSUS TRANSACTIONNELLE DU CLIENT : DEVELOPPEMENT D'UNE ECHELLE DANS LE SECTEUR BANCAIRE FRANÇAIS. UNE ETUDE EXPLORATOIRE

    OpenAIRE

    Benamour , Yasmine; Prim-Allaz , Isabelle

    2000-01-01

    International audience; The authors conduct an exploratory study in order to develop a measurement scale of customers transactional/relational orientation. The study is implemented in the context of French banking industry in both B.-to-C. and B.-to-B. environments. The results show that a different scale is needed for each context.; Les auteurs mettent en place une étude exploratoire dans le but de développer une échelle de mesure de l'orientation transactionnelle/relationnelle du client. Ce...

  3. Point defects and irradiation in oxides: simulations at the atomic scale; Defauts ponctuels et irradiation dans les oxydes: simulation a l'echelle atomique

    Energy Technology Data Exchange (ETDEWEB)

    Crocombette, J.P

    2005-12-15

    The studies done by Jean-Paul Crocombette between 1996 and 2005 in the Service de Recherches de Metallurgie Physique of the Direction de l'Energie Nucleaire in Saclay are presented in this Habilitation thesis. These works were part of the material science researches on the ageing, especially under irradiation, of oxides of interest for the nuclear industry. In this context simulation studies at the atomic scale were performed on two elementary components of ageing under irradiation : point defects and displacement cascades ; using two complementary simulation techniques : ab initio electronic structure calculations and empirical potential molecular dynamics. The first part deals with point defects : self defects (vacancies or interstitials) or hetero-atomic dopants. One first recalls the energetics of such defects in oxides, the specific features of defects calculations and the expected accuracy of these calculations. Then one presents the results obtained on uranium dioxide, oxygen in silver and amorphous silica. The second part tackles the modelling of disintegration recoil nuclei in various?displacement cascades created by crystalline matrices for actinide waste disposal. Cascade calculations give access to the amorphization mechanisms under irradiation of these materials. One thus predicts that the amorphization in zircon takes place directly in the tracks whereas in lanthanum zirconate, the amorphization proceeds through the accumulation of point defects. Finally the prospects of these studies are discussed. (author)

  4. Towards Eulerian-Eulerian large eddy simulation of reactive two-phase plows; Vers la simulation des grandes echelles en formulation Euler-Euler des ecoulements reactifs diphasiques

    Energy Technology Data Exchange (ETDEWEB)

    Kaufmann, A.

    2004-03-15

    Particle laden flows occur in industrial applications ranging from droplets in gas turbines to fluidized bed in chemical industry. Prediction of the dispersed phase properties such as concentration and dynamics are crucial for the design of more efficient devices that meet the new pollutant regulations of the European community. Numerical simulation coupling Lagrangian tracking of discrete particles with DNS or LES of the carrier phase provide a well established powerful tool to investigate particle laden flows. Such numerical methods have the drawback of being numerically very expensive for practical applications. Numerical simulations based on separate Eulerian balance equations for both phases, coupled through inter-phase exchange terms might be an effective alternative approach. This approach has been validated for the case of tracer particles with very low inertia that follow the carrier phase almost instantaneously due to their small response time compared with the micro-scale time scales of the carrier phase. Objective of this thesis is to extend this approach to more inertial particles that occur in practical applications such as fuel droplets in gas turbine combustors. Existing results suggest a separation of the dispersed phase velocity into a correlated and an uncorrelated component. The energy related to the uncorrelated component is about 30% of the total particle kinetic energy when the particle relaxation time is comparable to the Lagrangian integral time scale. The presence of this uncorrelated motion leads to stress terms in the Eulerian balance equation for the particle momentum. Models for this stress terms are proposed and tested. Numerical simulations in the Eulerian framework are validated by comparison with simulations using Lagrangian particle tracking. Additionally coupling of the Eulerian transport equations for the particles to combustion models is tested. (author)

  5. Thermo-mechanical behaviour modelling of particle fuels using a multi-scale approach; Modelisation du comportement thermomecanique des combustibles a particules par une approche multi-echelle

    Energy Technology Data Exchange (ETDEWEB)

    Blanc, V.

    2009-12-15

    Particle fuels are made of a few thousand spheres, one millimeter diameter large, compound of uranium oxide coated by confinement layers which are embedded in a graphite matrix to form the fuel element. The aim of this study is to develop a new simulation tool for thermo-mechanical behaviour of those fuels under radiations which is able to predict finely local loadings on the particles. We choose to use the square finite element method, in which two different discretization scales are used: a macroscopic homogeneous structure whose properties in each integration point are computed on a second heterogeneous microstructure, the Representative Volume Element (RVE). First part of this works is concerned by the definition of this RVE. A morphological indicator based in the minimal distance between spheres centers permit to select random sets of microstructures. The elastic macroscopic response of RVE, computed by finite element has been compared to an analytical model. Thermal and mechanical representativeness indicators of local loadings has been built from the particle failure modes. A statistical study of those criteria on a hundred of RVE showed the significance of choose a representative microstructure. In this perspective, a empirical model binding morphological indicator to mechanical indicator has been developed. Second part of the work deals with the two transition scale method which are based on the periodic homogenization. Considering a linear thermal problem with heat source in permanent condition, one showed that the heterogeneity of the heat source involve to use a second order method to localized finely the thermal field. The mechanical non-linear problem has been treats by using the iterative Cast3M algorithm, substituting to integration of the behavior law a finite element computation on the RVE. This algorithm has been validated, and coupled with thermal resolution in order to compute a radiation loading. A computation on a complete fuel element reflect a strong interaction between the two scales, that confirm the interest of a such model to compute the behaviour of those fuels. (author)

  6. Large Eddy Simulations of turbulent flows with heat transfer; Simulation des grandes echelles d'ecoulements turbulents avec transferts de chaleur

    Energy Technology Data Exchange (ETDEWEB)

    Chatelain, A.

    2004-09-15

    LES of turbulent flows with heat transfer was used within the framework of conjugate heat transfer problems. The objective of this work lies not only in identifying the various elements likely to impair temperature fluctuations estimations at the fluid/solid interface but also to introduce adequate wall modeling. The choice of a proper convection scheme for the transport of passive scalars led to the adoption of a high order upwind scheme with slope limiter. The use of classical wall models having shown some weaknesses as for the estimation of parietal temperature fluctuations, two new approaches are proposed and tested. The first one relies on a complete resolution of the Navier-Stokes equations on a refined grid close to the wall making it possible to rebuild the temperature fluctuations near the wall. The second one relies on the simultaneous and one dimensional resolution of a turbulent boundary layer equation and a variance transport equation near the wall. (author)

  7. Modeling of the air pollution on various scales; Modelisation de la pollution atmospherique a differentes echelles. confrontations simulations/mesures pour la preparation d'Escompte 2001

    Energy Technology Data Exchange (ETDEWEB)

    Meleux, F.

    2002-11-15

    On June and July 2001, the campaign ESCOMPTE took place in the Marseille area in southern of France, with the aim of generating a detailed 3-D data base for the study of dynamics and chemistry of high pollution events so as to validate and improve air quality models. Previous to this field experiment, a pre-modelling exercise has been performed to document the dynamic interactions between sea and land breezes and orographic flows over this complex topographical area. This study was carried out using a nesting procedure at local and regional scales using the MESO-NH model (jointly developed by Laboratoire d'Aerologie and Meteofrance at Toulouse). Tracers emitted at various locations in the Marseille and Etang de Berre areas were first followed, then in a second step, full chemistry simulations have been run for two selected periods on June and July 1999, quite similar to the meteorological situations met during the IOP2a and the IOP4 in the 2001 campaign. The performance of the model has been assessed by comparing measured data with simulated data for meteorological parameters and ozone. The general ability of the model to correctly simulate these two situations allows to further study ozone plume developments. In particular, these studies bear upon the relative roles of O{sub 3} transport versus O{sub 3} chemical production, as a function of distance within the plume to anthropogenic emissions and biogenic emissions, together with ozone daily variations and peak values observed at rural sites. After that, ozone chemical production sensitivity is analysed in regards to its precursors. (author)

  8. Marine and fluvial facies modelling at petroleum reservoir scale; Modelisation des heterogeneites lithologiques a l'echelle du reservoir petrolier en milieu marin et fluviatile

    Energy Technology Data Exchange (ETDEWEB)

    Leflon, B.

    2005-10-15

    When modelling a petroleum reservoir, well data are very useful to model properties at a sub-seismic scale. Petrophysical properties like porosity or permeability are linked to the rock-type. Two methods based on well data have been developed to model facies. The first one is used to model marine carbonates deposits. The geometry of sedimentary layers is modelled through a special parameterization of the reservoir similar to Wheeler space. The time parameter is defined along the well paths thanks to correlations. The layer thickness is then extrapolated between wells. A given relationship between facies and bathymetry of sedimentation makes it possible to compute bathymetry along the well paths. Bathymetry is then extrapolated from wells and a reference map using the concept of accommodation. The model created this way is stratigraphically consistent. Facies simulation can then be constrained by the computed bathymetry. The second method describes a novel approach to fluvial reservoirs modelling. The core of the method lies in the association of a fairway with the channels to be simulated. Fairways are positioned so that all data are taken in account; they can be stochastic if unknown or explicitly entered if identified on seismic data. A potential field is defined within the fairway. Specifying a transfer function to map this potential field to thickness results in generating a channel inside the fairway. A residual component is stochastically simulated and added to the potential field creating realistic channel geometries. Conditioning to well data is obtained by applying the inverse transfer function at the data location to derive thickness values that will constrain the simulation of residuals. (author)

  9. Proposed classification scale for radiological incidents and accidents; Elaboration d'une echelle de classement des incidents et accidents radiologiques

    Energy Technology Data Exchange (ETDEWEB)

    NONE

    2003-04-15

    The scale proposed in this report is intended to facilitate communication concerning the severity of incidents and accidents involving the exposure of human beings to ionising radiations. Like the INES, it comprises eight levels of severity and uses the same terms (accident, incident, anomaly, serious and major) for keeping the public and the media informed. In a radiological protection context, the severity of an event is considered as being directly proportional to the risk run by an individual (the probability of developing fatal or non-fatal health effects) following exposure to ionising radiation in an incident or accident situation. However for society, other factors have to be taken into account to determine severity. The severity scale proposed is therefore based on assessment of the individual radiological risk. A severity level corresponding to exposure of a member of the public in an incident or accident situation is determined on the basis of risk assessment concepts and methods derived from international consensus on dose/effect relationships for both stochastic and deterministic effects. The severity of all the possible exposure situations - worker exposure, collective exposure, potential exposure - is determined using a system of weighting in relation to situations involving members of the public. In the case of this scale, to indicate the severity of an event, it is proposed to make use of the most penalizing level of severity, comparing: - the severity associated with the probability of occurrence of deterministic effects and the severity associated with the probability of occurrence of stochastic effects, when the event gives rise to both types of risk; - the severity for members of the public and the severity for exposed workers, when both categories of individuals are involved; - the severity on the proposed radiological protection scale and that obtained using the INES, when radiological protection and nuclear safety aspects are associated with the event in question. (author)

  10. Large Eddy simulations of flame/acoustics interactions in a swirl flow; Simulation aux grandes echelles des interactions flamme / acoustique dans un ecoulement vrille

    Energy Technology Data Exchange (ETDEWEB)

    Selle, L.

    2004-01-15

    Swirl flows exhibit a large variety of topologies, depending on the ratio of the flux axial momentum to the axial flux of tangential momentum: this ratio is called swirl number. Above a given critical value for the swirl number, the pressure gradient reverses the flow on the axis of rotation. This central recirculation zone is used in turbines for flame stabilization. And yet, reacting-swirled flows can exhibit combustion instabilities resulting from the coupling between acoustics and unsteady heat release. Combustion instabilities can lead to loss of control or even complete destruction of the system. Their prediction is impossible with standard engineering tools. The work presented here investigates the capabilities of numerical research tools for the prediction of combustion instabilities. Large-Eddy Simulation (LES) is implemented in a code solving the Navier-Stokes equations for compressible-multi-components fluids (code AVBP developed at CERFACS). This method takes into account for the major ingredients of combustion instabilities such as acoustics and flame / vortex interaction. The LES methodology is validated in the swirled flow from a complex industrial burner (SIEMENS PG). Both reactive and non-reactive regimes are successfully compared with experimental data in terms of mean temperature and mean and RMS velocities. Experimental measurements were performed at the university of Karlsruhe (Germany). A detailed analysis of the acoustics and its interaction with the flame front is performed with the code AVSP, also developed at CERFACS. (author)

  11. La lévitation Diamagnétique à l'Echelle Micrométrique: Applications et Possibilités

    OpenAIRE

    Pigot , Christian

    2008-01-01

    Levitation is a fascinating way to compensate the action of gravity. Diamagnetism is the only physical phenomenon that allows a stable, static and passive levitation at room temperature. However, this magnetic effet is mostly insignificant at ordinary scales. Among the different means to improve the amplitude of this phenomenon, scale reduction is promishing. The present work contributes to the exploration of the possibilities and the potentialities of levitation in the microsystems. The redu...

  12. Software framework and jet energy scale calibration in the ATLAS experiment; Environnement logiciel et etalonnage de l'echelle en energie des jets dans l'experience ATLAS

    Energy Technology Data Exchange (ETDEWEB)

    Binet, Sebastien [Laboratoire de Physique Corpusculaire, Universite Blaise Pascal - CNRS/IN2P3, 63000 Aubiere Cedex (France)

    2006-07-01

    This thesis presents the work achieved to instrument the ATLAS software framework, ATHENA, with a library of tools and utensils for the physics analysis as well as the extraction of the jet energy scale using physics events (in-situ calibration). The software part presents the various components of the ATHENA framework which handles the simulated and reconstructed data flow as well as the different stages of this process, before and during the data taking. The building of a library of tools easing the reconstruction of physics objects, their association with Monte-Carlo particles and their API is then explained. The need for common language and collaboration-wide utensils is emphasised as it allows to share the workload of validating these tools and to get reproducible physics results. The analysis part deals with the implementation of a light jet energy scale calibration algorithm within the C++ framework. This calibration algorithm makes use of W bosons decaying into light jets within semileptonic t t-bar events. From the processing of fast and full simulation data with this algorithm, it seems possible to reach a percent level knowledge of the light jet energy scale. Finally, the feasibility study of the b-jet energy scale calibration using {gamma}Z{sup 0} {yields} {gamma}b b-bar events is presented. It is shown that a purely sequential approach is not sufficient to extract the signal nor to collect a sufficient amount of Z{sup 0} to calibrate the b-jet energy scale. (author)

  13. Study of the permeability up-scaling by direct filtering of geostatistical model; Etude du changement d'echelle des permeabilites par filtrage direct du modele geostatistique

    Energy Technology Data Exchange (ETDEWEB)

    Zargar, G.

    2005-10-15

    In this thesis, we present a new approach, which consists in directly up-scaling the geostatistical permeability distribution rather than the individual realizations. Practically, filtering techniques based on. the FFT (Fast Fourier Transform), allows us to generate geostatistical images, which sample the up-scaled distributions. In the log normal case, an equivalence hydraulic criterion is proposed, allowing to re-estimate the geometric mean of the permeabilities. In the anisotropic case, the effective geometric mean becomes a tensor which depends on the level of filtering used and it can be calculated by a method of renormalisation. Then, the method was generalized for the categorial model. Numerical tests of the method were set up for isotropic, anisotropic and categorial models, which shows good agreement with theory. (author)

  14. Numerical analysis of scaling laws for capillary rise in soils; Lois d'echelle pour l'ascension capillaire dans les sols: analyse numerique

    Energy Technology Data Exchange (ETDEWEB)

    Rezzoug, A.; Konig, D.; Triantafyllidis, Th. [Ruhr Bochum Univ. (Germany); Coumoulos, H.; Soga, K. [Cambridge Univ. (United Kingdom)

    2000-07-01

    The capillary movement of water through soils is of interest in many practical environmental engineering problems, especially problems concerning pollutant transport in soils. The potential use of the geotechnical centrifuge to study the capillary phenomena in soils has been proposed and some results have been reported. The main issue in relation is the verification of the scaling laws for the capillary phenomena in soils. However, the theoretical aspect of the capillary rise in relation to the accelerated gravity effect is still poorly understood; further investigation is required on the gravity effect on the capillary pressure, the meniscus form, the scaling of the capillary height and the scaling of the time. A theoretical analysis of the movement in capillary tube, representing soil, is presented. Scaling laws for the capillary height and the time are proposed. The effect of the contact angle changes on the scaling laws is also considered. (authors)

  15. Spectroscopic Analyses of Neutron Capture Elements in Open Clusters

    Science.gov (United States)

    O'Connell, Julia E.

    The evolution of elements as a function or age throughout the Milky Way disk provides strong constraints for galaxy evolution models, and on star formation epochs. In an effort to provide such constraints, we conducted an investigation into r- and s-process elemental abundances for a large sample of open clusters as part of an optical follow-up to the SDSS-III/APOGEE-1 near infrared survey. To obtain data for neutron capture abundance analysis, we conducted a long-term observing campaign spanning three years (2013-2016) using the McDonald Observatory Otto Struve 2.1-meter telescope and Sandiford Cass Echelle Spectrograph (SES, R(lambda/Deltalambda) ˜60,000). The SES provides a wavelength range of ˜1400 A, making it uniquely suited to investigate a number of other important chemical abundances as well as the neutron capture elements. For this study, we derive abundances for 18 elements covering four nucleosynthetic families- light, iron-peak, neutron capture and alpha-elements- for ˜30 open clusters within 6 kpc of the Sun with ages ranging from ˜80 Myr to ˜10 Gyr. Both equivalent width (EW) measurements and spectral synthesis methods were employed to derive abundances for all elements. Initial estimates for model stellar atmospheres- effective temperature and surface gravity- were provided by the APOGEE data set, and then re-derived for our optical spectra by removing abundance trends as a function of excitation potential and reduced width log(EW/lambda). With the exception of Ba II and Zr I, abundance analyses for all neutron capture elements were performed by generating synthetic spectra from the new stellar parameters. In order to remove molecular contamination, or blending from nearby atomic features, the synthetic spectra were modeled by a best-fit Gaussian to the observed data. Nd II shows a slight enhancement in all cluster stars, while other neutron capture elements follow solar abundance trends. Ba II shows a large cluster-to-cluster abundance spread

  16. Role of mesoscale eddies in the global ocean uptake of anthropogenic CO{sub 2}; Role des tourbillons de meso-echelle oceaniques dans la distribution et les flux air-mer de CO{sub 2} anthropique a l'echelle globale

    Energy Technology Data Exchange (ETDEWEB)

    Zouhair, Lachkar

    2007-02-15

    Mesoscale eddies play a fundamental role in ocean dynamics particularly in the Southern Ocean. Global-scale tracer simulations are typically made at coarse resolution without explicitly modeling eddies. Here we ask what role do eddies play in ocean uptake, storage, and meridional transport of anthropogenic CO{sub 2}, CFC-11 and bomb {delta}{sup 14}C. We made global anthropogenic transient tracer simulations in coarse-resolution, ORCA2, and eddy-permitting, ORCA05 and ORCA025, versions of the ocean modelling system NEMO. We focus on the Southern Ocean where tracer air-sea fluxes are largest. Eddies have little effect on bomb {delta}{sup 14}C uptake and storage. Yet for CFC-11 and anthropogenic CO{sub 2}, increased eddy activity reduces southern extra-tropical uptake by 28% and 25% respectively, thereby providing better agreement with observations. It is shown that the discrepancies in the equilibration times between the three tracers determine their respective sensitivities to the model horizontal resolution. Applying Gent and McWilliams (1990) (GM) parameterization of eddies in the non-eddying version of the model does improve results, but not enough. An in-depth investigation of the mechanisms by which eddies affect the uptake of the transient tracers shows that including mesoscale eddies leads to an overall reduction in the Antarctic Intermediate Water (AAIW) ventilation, and modifies substantially the spatial distribution of their source regions. This investigation reveals also that the GM parameterization still overestimates the ventilation and the subduction of AAIW in the Indian Ocean where the simulated mixed layer is particularly deep during the winter. This work suggests that most current coarse-resolution models may overestimate the ventilation of AAIW in the Indian sector of the Southern Ocean. This study shows also that the use of the GM parameterization may be of limited utility where mixed layer is relatively deep and confirms the general need for a more adequate parameterization that represents both the effects of eddies in the ocean interior and in the mixed layer. Finally,we attempt to evaluate the contribution of mesoscale eddies to the meridional transport of anthropogenic CO{sub 2} and CFC-11 at the global scale. The mesoscale variability is found to little affect the annual-mean transport and its traditional hydrographic-based estimates except between the tropics and in the Southern Ocean. In these regions, the meridional distribution of the 'rectified' eddy transport of CFC-11 and anthropogenic CO{sub 2} shows large discrepancies. (author)

  17. Role of mesoscale eddies in the global ocean uptake of anthropogenic CO{sub 2}; Role des tourbillons de meso-echelle oceaniques dans la distribution et les flux air-mer de CO{sub 2} anthropique a l'echelle globale

    Energy Technology Data Exchange (ETDEWEB)

    Zouhair, Lachkar

    2007-02-15

    Mesoscale eddies play a fundamental role in ocean dynamics particularly in the Southern Ocean. Global-scale tracer simulations are typically made at coarse resolution without explicitly modeling eddies. Here we ask what role do eddies play in ocean uptake, storage, and meridional transport of anthropogenic CO{sub 2}, CFC-11 and bomb {delta}{sup 14}C. We made global anthropogenic transient tracer simulations in coarse-resolution, ORCA2, and eddy-permitting, ORCA05 and ORCA025, versions of the ocean modelling system NEMO. We focus on the Southern Ocean where tracer air-sea fluxes are largest. Eddies have little effect on bomb {delta}{sup 14}C uptake and storage. Yet for CFC-11 and anthropogenic CO{sub 2}, increased eddy activity reduces southern extra-tropical uptake by 28% and 25% respectively, thereby providing better agreement with observations. It is shown that the discrepancies in the equilibration times between the three tracers determine their respective sensitivities to the model horizontal resolution. Applying Gent and McWilliams (1990) (GM) parameterization of eddies in the non-eddying version of the model does improve results, but not enough. An in-depth investigation of the mechanisms by which eddies affect the uptake of the transient tracers shows that including mesoscale eddies leads to an overall reduction in the Antarctic Intermediate Water (AAIW) ventilation, and modifies substantially the spatial distribution of their source regions. This investigation reveals also that the GM parameterization still overestimates the ventilation and the subduction of AAIW in the Indian Ocean where the simulated mixed layer is particularly deep during the winter. This work suggests that most current coarse-resolution models may overestimate the ventilation of AAIW in the Indian sector of the Southern Ocean. This study shows also that the use of the GM parameterization may be of limited utility where mixed layer is relatively deep and confirms the general need for a more adequate parameterization that represents both the effects of eddies in the ocean interior and in the mixed layer. Finally,we attempt to evaluate the contribution of mesoscale eddies to the meridional transport of anthropogenic CO{sub 2} and CFC-11 at the global scale. The mesoscale variability is found to little affect the annual-mean transport and its traditional hydrographic-based estimates except between the tropics and in the Southern Ocean. In these regions, the meridional distribution of the 'rectified' eddy transport of CFC-11 and anthropogenic CO{sub 2} shows large discrepancies. (author)

  18. VizieR Online Data Catalog: Photometry and spectroscopy of NP Per (Lacy+, 2016)

    Science.gov (United States)

    Lacy, C. H. S.; Fekel, F. C.; Pavlovski, K.; Torres, G.; Muterspaugh, M. W.

    2016-09-01

    From 2011 November through 2014 November, we acquired 56 high-quality spectra of NP Per with the Tennessee State University 2m Automatic Spectroscopic Telescope (AST) and a fiber-fed echelle spectrograph at Fairborn Observatory in southeast Arizona. Of these spectra, 55 were suitable for radial velocity measurements (see Table1). The detector for these observations was a Fairchild 486 CCD, having 4096*4096 15μ pixels. While the spectrograms have 48 orders ranging from 3800 to 8260Å, we have used just the orders that cover the wavelength region from 4920 to 7100Å. We made our observations with a fiber that produced a spectral resolution of 0.4Å, corresponding to a resolving power of 15000 at 6000Å. Our spectra have typical signal-to-noise ratios (S/Ns) of 40 at 6000Å. We began V-band photometric observations of NP Per with the URSA WebScope on 2003 December 2. URSA is a 10inch Schmidt-Cassegrain telescope made by Meade Instruments Corp., equipped with a V-band filter and a Santa Barbara Instruments Group ST8 CCD camera, housed in a Technical Innovations RoboDome, all controlled by a Macintosh computer in a control room under the observing deck of Kimpel Hall on the University of Arkansas campus at Fayetteville. A larger telescope, the NFO WebScope, was brought to bear on 2005 February 27. Nearly all the observations after this date were obtained with the NFO, which is a robotic 24inch Cassegrain reflector located near Silver City, NM, USA. Both telescopes used Bessel V filters consisting of 2.0mm of GG495 and 3.0mm of BG 39. Exposures were 120 seconds long for both telescopes, and the cadence was typically 150 seconds per image. The images contained the variable star (TYC 2371-0390-1=BD +31 0729) and 2 comparison stars (TYC 2371-156-1 and TYC 2371-1034-1) of approximately the same brightness and color as the variable star. The observations are given in Table6 for the URSA WebScope and in Table7 for the NFO WebScope. Dates of eclipses obtained from the

  19. DFT studies of fluid-minerals interactions at the molecular level: examples and perspectives; Etudes DFT des interactions fluides-mineraux a l'echelle moleculaire: exemples et perspectives

    Energy Technology Data Exchange (ETDEWEB)

    Toulhoat, H.; Digne, M.; Arrouvel, C.; Raybaud, P. [Institut Francais du Petrole (IFP), 92 - Rueil-Malmaison (France)

    2005-03-15

    The scope of applications of first-principle theoretical chemistry methods has been vastly expanded over the past years due to the combination of improved methods and algorithms for solving the poly-electronic Schroedinger equation with exponential growth of computer power available at constant cost (the so-called 'Moore law'). In particular, atomistic studies of solid-fluid interfaces are now routinely producing new qualitative and quantitative insights into adsorption, surface speciation as a function of the prevailing chemical potentials, and reactivity of surface species. This approach is currently widely exploited in the fields of heterogeneous catalysis and surface physics, and so far to a lesser extent for geochemical purposes, although the situation is rapidly evolving. Many fundamental issues of fluid-minerals interaction phenomena can indeed be addressed ab initio with atomistic 3D periodic models of fluid-solid interfaces involving up to 200-300 un-equivalent atoms. We illustrate this proposal with recent IFP results, some of which are of primary interest with respect to the manufacture of catalysts supports, but which also show some relevance for inorganic geochemical issues in the context of the sequestration of acid gases in subsurface porous rocks: - reactive wetting of boehmite AlOOH and morphology prediction; - acid-basic surface properties of a transition alumina; - hydroxylation and sulfhydrylation of anatase TiO{sub 2} surfaces. Through these examples, the performances of DFT and a variety of up-to-date modeling techniques and strategies are discussed. (authors)

  20. Multi-scale structuration of the electrode-electrolyte interface for applications in bio-electro-catalysis; Structuration multi-echelle de l'interface electrode-electrolyte pour des applications en bioelectrocatalyse

    Energy Technology Data Exchange (ETDEWEB)

    Kuhn, A. [Bordeaux-1 Univ., LACReM, ENSCPB, 33 - Pessac (France)

    2006-07-01

    In this work, two approaches have been combined to elaborate bio-functionalized interfaces having an original structure and well defined at several characteristic scales. These two approaches are 1)the growth of conducting or non conducting materials through organized structures and 2)the chemistry of non-covalent intermolecular bonds leading to the assembling of molecules towards interfacial structures having greatest size. With a deep physico-chemical characterization, it has been possible to understand the properties of these multi-scale structures and to propose different applications fields as for instance bio-electro-catalysis or photovoltaic cells. (O.M.)

  1. Theoretical study of silicon carbide under irradiation at the nano scale: classical and ab initio modelling; Etude theorique a l'echelle nanometrique du carbure de silicium sous irradiation: modelisation classique et ab initio

    Energy Technology Data Exchange (ETDEWEB)

    Lucas, G

    2006-10-15

    The behaviour of silicon carbide under irradiation has been studied using classical and ab initio simulations, focusing on the nano scale elementary processes. First, we have been interested in the calculation of threshold displacement energies, which are difficult to determine both experimentally and theoretically, and also the associated Frenkel pairs. In the framework of this thesis, we have carried out simulations in classical and ab initio molecular dynamics. For the classical approach, two types of potentials have been used: the Tersoff potential, which led to non satisfactory results, and a new one which has been developed during this thesis. This potential allows a better modelling of SiC under irradiation than most of the empirical potentials available for SiC. It is based on the EDIP potential, initially developed to describe defects in silicon, that we have generalized to SiC. For the ab initio approach, the feasibility of the calculations has been validated and average energies of 19 eV for the C and 38 eV for the Si sublattices have been determined, close to the values empirically used in the fusion community. The results obtained with the new potential EDIP are globally in agreement with those values. Finally, the elementary processes involved in the crystal recovery have been studied by calculating the stability of the created Frenkel pairs and determining possible recombination mechanisms with the nudged elastic band method. (author)

  2. Hydration of swelling clays: multi-scale sequence of hydration and determination of macroscopic energies from microscopic properties; Hydratation des argiles gonflantes: sequence d'hydratation multi-echelle determination des energies macroscopiques a partir des proprietes microscopiques

    Energy Technology Data Exchange (ETDEWEB)

    Salles, F

    2006-10-15

    Smectites have interesting properties which make them potential candidates for engineered barriers in deep geological nuclear waste repository: low permeability, swelling and cations retention. The subject of this thesis consists in the determination of the relationship between hydration properties, swelling properties and cations mobility in relation with confinement properties of clayey materials. The aim is to understand and to predict the behaviour of water in smectites, following two research orientations: the mechanistic aspects and the energetic aspects of the hydration of smectites. We worked on the Na-Ca montmorillonite contained in the MX80 bentonite, with the exchanged homo ionic structure (saturated with alkaline cations and calcium cations). The approach crosses the various scales (microscopic, mesoscopic and macroscopic) and implied the study of the various components of the system (layer-cation-water), by using original experimental methods (thermo-poro-metry and electric conductivity for various relative humidities (RH) and electrostatic calculations. Initially, the dry state is defined by SCTA (scanning calorimetry thermal analysis). Then a classical characterization of the smectite porosity for the dry state is carried out using mercury intrusion and nitrogen adsorption. We evidenced the existence of a meso-porosity which radius varies from 2 to 10 nm depending on the compensating cation. The thermo-poro-metry and conductivity experiments performed at various hydration states made it possible to follow the increase in the pore sizes and the cations mobility as a function of the hydration state. We highlight in particular the existence of an osmotic mesoscopic swelling for low RH (approximately 50-60%RH for Li and Na). By combining the results of thermo-poro-metry, X-ray diffraction and electric conductivity, we are able to propose a complete hydration sequence for each cation, showing the crucial role of the compensating cation in the hydration of smectites: it is responsible for the structure of porosity in a dry state and of the evolution of the pore sizes as a function of the RH and it modifies the hydration sequence by its mobility inside the interlayer space. The distinction between various types of water in the smectite structure is also achieved by thermo-poro-metry at different RH: water bound to the cations and surfaces, water structured by porosity and free water. This distinction is important to understand the behaviour of smectite and in particular the diffusion properties in clayey materials. The importance of the cation nature is also highlighted by the energetic model. Electrostatic calculations using the PACHA formalism (Electronegativities Equalization method) show that, for the small cations, the hydration energy of the layers is predominant. To obtain these results, we determine the surface enthalpies for the dry state, which show a coherent evolution as a function of the cation partial charge with the increase of pore sizes and thus with particle sizes. Then, using a theoretical model, we calculated swelling energies, surface hydration energies and cation hydration energies. The behaviour of mixed purified clay displays a behaviour closer to that of a calcic clay for the experiments carried out, in contradiction with the fact that the Na cation is the most abundant. This observation implies results on the clay properties, different from that expected for hydration properties, swelling and interlayer cation mobility within the framework of the radioactive waste. (author)

  3. Dislocation glide in Ni-Al solid solutions from the atomic scale up: a molecular dynamics study; Etude du glissement des dislocations dans la solution solide Ni-Al par simulation a l'echelle atomique

    Energy Technology Data Exchange (ETDEWEB)

    Rodary, E

    2003-01-01

    The glide of an edge dislocation in solid solutions is studied by molecular dynamics, at fixed temperature and imposed external stress. We have optimized an EAM potential for Ni(1 a 8% A1): it well reproduces the lattice expansion, local atomic order, stacking fault energy as a function of composition, as well as the elastic properties of the {gamma}' phase with L1{sub 2} structure. On increasing the stress, the dislocation is first immobile, then glides with a velocity proportional to the stress and the velocity saturates on reaching the transverse sound velocity. However, only beyond a static threshold stress, {sigma}{sub s}, does the dislocation glide a distance large enough to allow macroscopic shear; the linear part of the velocity-stress curve extrapolates to zero at a dynamical threshold stress, {sigma}{sub d}, The friction coefficient, and the threshold stresses ({sigma}{sub s} and {sigma}{sub d}), increase with the A1 concentration and decrease with temperature (300 and 500 K). Close to the critical shear stress, {sigma}{sub s}, the dislocation glide is analysed with a 'stop and go' model. The latter yields the flight velocity between obstacles, the mean obstacle density and the distribution of the waiting time on each obstacle as a function of stress, composition and temperature. The obstacle to the glide is proposed to be the strong repulsion between Al atoms brought into nearest neighbour position by the glide process, and not the dislocation-solute interaction. The microscopic parameters so defined are introduced into a micro-mechanical model, which well reproduces the known behaviour of nickel base solid solutions. (author)

  4. Thermally accurate LES of the stability-emission performance of staged gas-turbine combustion; Simulation aux grandes echelles de la combustion etagee dans les turbines a gaz et son interaction stabilite-polluants-thermique

    Energy Technology Data Exchange (ETDEWEB)

    Schmitt, P.

    2005-06-15

    Modern gas turbines use turbulent lean partially premixed combustion in order to minimise nitrous oxide (NO{sub X}) emissions while ensuring flashback safety. The Large-Eddy Simulation (LES) of such a device is the goal of this work. Focus is laid on correctly predicting the NO{sub X} emissions, which are influenced by four factors: heat transfer, mixing quality, combustion modelling and thermo-acoustic stability. As NO{sub X} reaction rates are strongly influenced by temperature, heat transfer by radiation and convection is included. Radiation is predicted by a model, which assumes that the gases are optically thin. Convective heat transfer is included via a newly developed and validated wall-function approach based on the logarithmic law of the wall for temperature. An optimised 2-step reduced chemical reaction scheme for lean methane combustion is presented. This scheme is used for the LES in conjunction with an additional third reaction, fitted to produce the same NO{sub X} reaction rates as in the complete reaction mechanism. Turbulence is accounted for with the thickened flame model in a form, which is optimised for changing equivalence ratios and mesh-resolutions. Mixing is essential not only for predicting flame stabilisation, but also for pollutant emissions as NO{sub X} reaction rates depend exponentially on equivalence ratio. Therefore the full burner geometry, including 16 fuel injections is resolved in LES. Additionally, effusion cooling and film cooling is accounted for in a simplified manner. The non-reacting flow is extensively validated with experimental results. As mixture-fraction fluctuations do not only arise from turbulence, but also from thermo-acoustic instabilities, care was taken to provide acoustic boundary conditions that come close to reality. The resulting LES shows a strong thermo-acoustic instability, comparing well with experimental observations. By making the boundaries completely anechoic it is shown that when the instability disappears, the NO{sub X} levels are reduced by 75%. Additionally, neglecting all heat transfer, effusion and film cooling, the NO{sub X} levels are increased again by one order of magnitude. (author)

  5. Inverse modeling for the optimization of primary sources of atmospheric pollution at a regional scale; Modelisation inverse pour l'optimisation des sources primaires de pollution atmospherique a l'echelle regionale

    Energy Technology Data Exchange (ETDEWEB)

    Pison, I

    2005-12-15

    Atmospheric pollution at a regional scale is the result of various interacting processes: emissions, chemistry, transport, mixing and deposition of gaseous species. The forecast of air quality is then performed by models, in which the emissions are taken into account through inventories. The simulated pollutant concentrations depend highly on the emissions that are used. Now inventories that represent them have large uncertainties. Since it would be difficult today to improve their building methodologies, there remains the possibility of adding information to existing inventories. The optimization of emissions uses the information that is available in measurements to get the inventory that minimizes the difference between simulated and measured concentrations. A method for the inversion of anthropogenic emissions at a regional scale, using network measurements and based on the CHIMERE model and its adjoint, was developed and validated. A kriging technique allows us to optimize the use of the information available in the concentration space. Repeated kriging-optimization cycles increase the quality of the results. A dynamical spatial aggregation technique makes it possible to further reduce the size of the problem. The NO{sub x} emissions from the inventory elaborated by AIRPARIF for the Paris area were inverted during the summers of 1998 and 1999, the events of the ESQUIF campaign being studied in detail. The optimization reduces large differences between simulated and measured concentrations. Generally, however, the confidence level of the results decreases with the density of the measurement network. Therefore, the results with the higher confidence level correspond to the most intense emission fluxes of the Paris area. On the whole domain, the corrections to the average emitted mass and to the matching time profiles are consistent with the estimate of 15% obtained during the ESQUIF campaign. (author)

  6. Study of vibrations and stabilization of linear collider final doublets at the sub-nanometer scale; Etude des vibrations et de la stabilisation a l'echelle sous-nanometrique des doublets finaux d'un collisionneur lineaire

    Energy Technology Data Exchange (ETDEWEB)

    Bolzon, B

    2007-11-15

    CLIC is one of the current projects of high energy linear colliders. Vertical beam sizes of 0.7 nm at the time of the collision and fast ground motion of a few nanometers impose an active stabilization of the final doublets at a fifth of nanometer above 4 Hz. The majority of my work concerned vibrations and active stabilization study of cantilever and slim beams in order to be representative of the final doublets of CLIC. In a first part, measured performances of different types of vibration sensors associated to an appropriate instrumentation showed that accurate measurements of ground motion are possible from 0.1 Hz up to 2000 Hz on a quiet site. Also, electrochemical sensors answering a priori the specifications of CLIC can be incorporated in the active stabilization at a fifth of nanometer. In a second part, an experimental and numerical study of beam vibrations enabled to validate the efficiency of the numerical prediction incorporated then in the simulation of the active stabilization. Also, a study of the impact of ground motion and of acoustic noise on beam vibrations showed that an active stabilization is necessary at least up to 1000 Hz. In a third part, results on the active stabilization of a beam at its two first resonances are shown down to amplitudes of a tenth of nanometer above 4 Hz by using in parallel a commercial system performing passive and active stabilization of the clamping. The last part is related to a study of a support for the final doublets of a linear collider prototype in phase of finalization, the ATF2 prototype. This work showed that relative motion between this support and the ground is below imposed tolerances (6 nm above 0.1 Hz) with appropriate boundary conditions. (author)

  7. Software framework and jet energy scale calibration in the ATLAS experiment; Environnement logiciel et etalonnage de l'echelle en energie des jets dans l'experience ATLAS

    Energy Technology Data Exchange (ETDEWEB)

    Binet, Sebastien [Laboratoire de Physique Corpusculaire, Universite Blaise Pascal - CNRS/IN2P3, 63000 Aubiere Cedex (France)

    2006-07-01

    This thesis presents the work achieved to instrument the ATLAS software framework, ATHENA, with a library of tools and utensils for the physics analysis as well as the extraction of the jet energy scale using physics events (in-situ calibration). The software part presents the various components of the ATHENA framework which handles the simulated and reconstructed data flow as well as the different stages of this process, before and during the data taking. The building of a library of tools easing the reconstruction of physics objects, their association with Monte-Carlo particles and their API is then explained. The need for common language and collaboration-wide utensils is emphasised as it allows to share the workload of validating these tools and to get reproducible physics results. The analysis part deals with the implementation of a light jet energy scale calibration algorithm within the C++ framework. This calibration algorithm makes use of W bosons decaying into light jets within semileptonic t t-bar events. From the processing of fast and full simulation data with this algorithm, it seems possible to reach a percent level knowledge of the light jet energy scale. Finally, the feasibility study of the b-jet energy scale calibration using {gamma}Z{sup 0} {yields} {gamma}b b-bar events is presented. It is shown that a purely sequential approach is not sufficient to extract the signal nor to collect a sufficient amount of Z{sup 0} to calibrate the b-jet energy scale. (author)

  8. Dislocations and elementary processes of plasticity in FCC metals: atomic scale simulations; Dislocations et processus elementaires de la plasticite dans les metaux CFC: apports des simulations a l'echelle atomique

    Energy Technology Data Exchange (ETDEWEB)

    Rodney, D

    2000-07-01

    We present atomic-scale simulations of two elementary processes of FCC crystal plasticity. The first study consists in the simulation by molecular dynamics, in a nickel crystal, of the interactions between an edge dislocation and glissile interstitial loops of the type that form under irradiation in displacement cascades. The simulations show various atomic-scale interaction processes leading to the absorption and drag of the loops by the dislocation. These reactions certainly contribute to the formation of the 'clear bands' observed in deformed irradiated materials. The simulations also allow to study quantitatively the role of the glissile loops in irradiation hardening. In particular, dislocation unpinning stresses for certain pinning mechanisms are evaluated from the simulations. The second study consists first in the generalization in three dimensions of the quasi-continuum method (QCM), a multi-scale simulation method which couples atomistic techniques and the finite element method. In the QCM, regions close to dislocation cores are simulated at the atomic-scale while the rest of the crystal is simulated with a lower resolution by means of a discretization of the displacement fields using the finite element method. The QCM is then tested on the simulation of the formation and breaking of dislocation junctions in an aluminum crystal. Comparison of the simulations with an elastic model of dislocation junctions shows that the structure and strength of the junctions are dominated by elastic line tension effects, as is assumed in classical theories. (author)

  9. Heat and mass transfer in multi-scale porous structures: application to Diesel particulate filters modelling; Transferts de chaleur et de masse dans des structures poreuses multi-echelles: application a l'etude des filtres a particules Diesel

    Energy Technology Data Exchange (ETDEWEB)

    Oxarango, L.

    2004-09-15

    Ceramic filters appear to be the most promising solution to deal with the future emission standard requirements for diesel powered vehicles. Indeed, this type of Diesel Particulate Filters provides suitable characteristics for high efficiency soot collection. However, this filtration process is characterised by a dramatic increase of the pressure drop imposed in the exhaust line. Thus, the filter has to be cleaned periodically to insure the proper engine operating conditions. This regeneration phase is based on the oxidation of the carbon particles within the apparatus. This complex thermal process is critical for the safety working of Diesel Particulate Filters. Indeed, thermal stresses induced by the heat released during soot oxidation are involved in most of the filter breaking scenario. Numerous geometrical parameters defining the complex multi-scale structure of the apparatus could influence its thermal response. Thus, the geometrical optimization of these filters is a major problematic for the development of new products. This study aims at modelling heat and mass transfer phenomenon within Diesel Particulate Filters. The studied geometrical configuration is based on a ceramic honeycomb with porous walls and alternately plugged channel known as wall-flow DPF. In a first part, the gas flow, particles transport and collection are considered. Given the apparatus particular structure, the problem has to be treated considering various spatial length-scales. The filtering walls are characterised by a micrometric porous structure. The flow modelling with the Darcy law requires determining a particular effective permeability. The laminar flow problem in millimetric channels with wall suction (or injection) is studied. The asymptotic solution for flow in two-dimensional channels is used to derive a one-dimensional system preserving mass and momentum balances. This approach is then extended to the square channel configuration using direct numerical simulations. The particle collection process is modelled as a simple cake layer formation with respect to the gas flow properties. A parametric study carried out on periodic representative cells evidence the heterogeneous distribution of soot along the filter channel. Then, the non-periodic multi-channel case is considered. The particle loading appears to be weakly sensitive to local heterogeneities imposed in a single channel. Finally, the mass and momentum equations are expressed under a macroscopic form. The filtration process could then be simulated in the whole apparatus. During this study, a particular care has been taken to validate each model against experiment. In a second part, the thermal problem is considered. The phenomena occurring at the micrometric scale are taken into account. However, the study focuses more particularly on the scale change allowing describing the honeycomb as an equivalent homogeneous media. The analysis is base on the volume averaging theory. A thermal-equilibrium assumption is considered to express a macroscopic one-equation model including all the thermal exchanges. The local contributions to the macroscopic balance equation are taken into account defining closure problems. These closure problems are computed numerically on a periodic representative cell of the filter to obtain an effective thermal conductivity tensor. The particles oxidation reaction is taken into account as a source term in the macroscopic equation. It includes a global reaction kinetic model. The oxygen transport through the soot layer appears to play a limiting role for the chemical reaction. The complete macroscopic energy balance model is solved numerically with a finite volume method. The measurements obtained from two different experimental apparatus are used to validate the approach. Finally, the influence of some geometrical parameters on the thermal behaviour during regeneration is discussed. (author)

  10. Transfer of reactive solutes in the unsaturated zone of soils at several observation scales; Transfert de solutes reactifs dans la zone non-saturee des sols a differentes echelles d'observation

    Energy Technology Data Exchange (ETDEWEB)

    Limousin, G

    2006-10-15

    The transfer of contaminants in the unsaturated zone of soils is driven by numerous mechanisms. Field studies are sometimes difficult to set up, and so the question is raised about the reliability of laboratory measurements for describing a field situation. The nuclear power plant at Brennilis (Finistere, France) has been chosen to study the transfer of strontium, cobalt and inert tracers in the soil of this industrial site. Several observation scales have been tested (batch, stirred flow-through reactor, sieved-soil column, un-repacked or repacked soil-core lysimeter, field experiments) in order to determine, at each scale, the factors that influence the transfer of these contaminants, then to verify the adequacy between the different observation scales and their field representativeness. Regarding the soil hydrodynamic properties, the porosity, the water content in the field, the pore water velocity at the water content in the field, the saturation hydraulic conductivity and the dispersion coefficient of this embanked soil are spatially less heterogeneous than those of agricultural or non-anthropic soils. The results obtained with lysimeter and field experiments suggest that hydrodynamics of this unstructured soil can be studied on a repacked sample if the volume is high compared to the rare big-size stones. Regarding the chemical soil-contaminant interactions, cobalt and strontium isotherms are non-linear at concentration higher than 10{sup -4} mol.L{sup -1}, cobalt adsorption and desorption are fast and independent on pH. On the contrary, at concentration lower than 3.5 x 10{sup -6} mol.L{sup -1}, cobalt and strontium isotherms are linear, cobalt desorption is markedly slower than adsorption and both cobalt partition coefficient at equilibrium and its reaction kinetics are highly pH-dependent. For both elements, the results obtained with batch, stirred flow-through reactor and sieved-soil column are in adequacy. However, strontium batch adsorption measurements at equilibrium do not make possible to describe the results of field transfer experiments. (author)

  11. Multi-scales analysis of the global change impact on the diversity of the aphid communities; Analyse multi-echelle de l'impact du changement global sur la diversite des communautes aphidiennes

    Energy Technology Data Exchange (ETDEWEB)

    Hulle, M

    2007-07-01

    The primary objective of this project is to investigate the effects of global change on the biodiversity of aphid communities in Western Europe. Biodiversity has been examined at 3 levels: total number of species, phenology and reproductive strategy. Data were provided by EXAMINE, the European suction traps network which has been now operating for 35 years. 392 different species have been identified. At each location, total number of species has been regularly increasing, one additional species being caught every 1 or 2 years depending on location. This is due to introduced species but also to warming which favours rare species. No general trend of increasing density has been detected, but phenological earliness of almost all species (annual date of first appearance in suction traps) is strongly correlated with temperature and especially with mean daily temperature (during more or less long periods of time lying principally in February and March) or number of days below 0 C. Strong relationships between aphid phenology and environmental variables have been found and there is strong discrimination between species with different life cycle strategies, and between species feeding on herbs and trees, suggesting the possible value of trait-based groupings in predicting responses to environmental changes. These preliminary results suggest that 1) biodiversity has increased during the last decades; 2) there is a pool of species among which some of them reach a detectable density only during years where temperatures are high enough; 3) a set of newly introduced species succeed in settling being favoured by warming and 4) phenology of aphids is expected to advance and their abundance to increase with temperature, and the possible role of natural enemies to regulate abundant species is discussed. (author)

  12. Grain scale stresses and strains determination by X-ray diffraction; Contribution a l'analyse par diffractometrie X des deformations et des contraintes a l'echelle des grains

    Energy Technology Data Exchange (ETDEWEB)

    Huang, W

    2007-03-15

    A new methodology for strain and stress analysis by X ray diffraction (XRD) in single crystal was developed. It can be applied to determine the second order stress (in grain scale) in single and multi-crystal material with non-cubic lattice. This method is based on the method Ortner I. It has introduced the metric tensor G which is deduced from the lattice space measured by XRD. In the developed method, when the crystal reference is non-orthonormal, an orthonormal reference associated with the crystal basis is defined, so all calculation could be done with usual calculation laws. The use of the least square method allows the acquisition of many more measurements than the six absolute necessary. Then a better metric tensor G is calculated and the statistical error is obtained. This developed method was applied in a bi crystal copper. The experimental results have shown that this method is also effective. The second order residuals stresses for coarse Zn grains in a galvanized coating were determined after annealing. The four coarse grains with different orientations were also characterized and demonstrated the elastic and plastic deformation mechanism in a grain or between the grains during in situ tensile loading. So this method is well able to determine the strains and stresses in grain scale in a mono crystal or multi crystal with any crystalline structure. (author)

  13. Macro-scale turbulence modelling for flows in porous media; Modelisation a l'echelle macroscopique d'un ecoulement turbulent au sein d'un milieu poreux

    Energy Technology Data Exchange (ETDEWEB)

    Pinson, F

    2006-03-15

    - This work deals with the macroscopic modeling of turbulence in porous media. It concerns heat exchangers, nuclear reactors as well as urban flows, etc. The objective of this study is to describe in an homogenized way, by the mean of a spatial average operator, turbulent flows in a solid matrix. In addition to this first operator, the use of a statistical average operator permits to handle the pseudo-aleatory character of turbulence. The successive application of both operators allows us to derive the balance equations of the kind of flows under study. Two major issues are then highlighted, the modeling of dispersion induced by the solid matrix and the turbulence modeling at a macroscopic scale (Reynolds tensor and turbulent dispersion). To this aim, we lean on the local modeling of turbulence and more precisely on the k - {epsilon} RANS models. The methodology of dispersion study, derived thanks to the volume averaging theory, is extended to turbulent flows. Its application includes the simulation, at a microscopic scale, of turbulent flows within a representative elementary volume of the porous media. Applied to channel flows, this analysis shows that even within the turbulent regime, dispersion remains one of the dominating phenomena within the macro-scale modeling framework. A two-scale analysis of the flow allows us to understand the dominating role of the drag force in the kinetic energy transfers between scales. Transfers between the mean part and the turbulent part of the flow are formally derived. This description significantly improves our understanding of the issue of macroscopic modeling of turbulence and leads us to define the sub-filter production and the wake dissipation. A f - <{epsilon}>f - <{epsilon}{sub w}>f model is derived. It is based on three balance equations for the turbulent kinetic energy, the viscous dissipation and the wake dissipation. Furthermore, a dynamical predictor for the friction coefficient is proposed. This model is then successfully applied to the study of turbulent channel flows. (author)

  14. Tokamak electron heat transport by direct numerical simulation of small scale turbulence; Transport de chaleur electronique dans un tokamak par simulation numerique directe d'une turbulence de petite echelle

    Energy Technology Data Exchange (ETDEWEB)

    Labit, B

    2002-10-01

    In a fusion machine, understanding plasma turbulence, which causes a degradation of the measured energy confinement time, would constitute a major progress in this field. In tokamaks, the measured ion and electron thermal conductivities are of comparable magnitude. The possible sources of turbulence are the temperature and density gradients occurring in a fusion plasma. Whereas the heat losses in the ion channel are reasonably well understood, the origin of the electron losses is more uncertain. In addition to the radial velocity associated to the fluctuations of the electric field, electrons are more affected than ions by the magnetic field fluctuations. In experiments, the confinement time can be conveniently expressed in terms of dimensionless parameters. Although still somewhat too imprecise, these scaling laws exhibit strong dependencies on the normalized pressure {beta} or the normalized Larmor radius, {rho}{sub *}. The present thesis assesses whether a tridimensional, electromagnetic, nonlinear fluid model of plasma turbulence driven by a specific instability can reproduce the dependence of the experimental electron heat losses on the dimensionless parameters {beta} and {rho}{sub *}. The investigated interchange instability is the Electron Temperature Gradient driven one (ETG). The model is built by using the set of Braginskii equations. The developed simulation code is global in the sense that a fixed heat flux is imposed at the inner boundary, leaving the gradients free to evolve. From the nonlinear simulations, we have put in light three characteristics for the ETG turbulence: the turbulent transport is essentially electrostatic; the potential and pressure fluctuations form radially elongated cells called streamers; the transport level is very low compared to the experimental values. The thermal transport dependence study has shown a very small role of the normalized pressure, which is in contradiction with the Ohkama's formula. On the other hand, the crucial role of the electron normalized Larmor has been emphasized: the confinement time is inverse proportional to this parameter. Finally, the low dependence of turbulent transport with the magnetic shear and the inverse aspect ratio is also reported. Although the transport level observed in the simulations is low compared to the experiments, we have tried a direct confrontation with Tore Supra results. This tokamak is well designed to study the electron heat transport. Keeping most of the parameters from a well referenced Tore Supra shot, the nonlinear simulation gives a threshold quite close to the experimental one. The observed turbulent conductivity is a factor fifty lower than the experimental one. An important parameter can not be matched: the normalized Larmor radius, {rho}{sub *}. This limitation has to be overcome in order to confirm this results. Finally, a rigorous confrontation between this result and gyrokinetic simulations has to conclude that the ETG instability cannot describe electron heat loses in tokamaks. (author)

  15. Evaluation des apports solaires a l'echelle d'un quartier urbain en periode de chauffe selon sa typologie, son orientation et sa latitude dans un contexte de densification de la ville

    Science.gov (United States)

    Chenard, Laurent

    Mass urbanization is a major issue for town administrators. Population increase will have an impact on the quality of the environment for citizens. Government will have to take decisions to limit those effects. Green energies are part of the solution to reach fixed goals by the public administration for sustainable development. Passive solar energy is studied in this work in an urban canopy located in five different towns: San Francisco, Montreal, Bordeaux, Lyon and Stockholm. Passive solar energy is calculated in the heating season. Direct and diffuse solar radiation is considered by using the Perez model. Radiosity is not taken into account. Heating demand is calculated by the heating degree day method. Seven urban forms have been created to determine the amount of solar energy entering in every window of the urban canopy while taking into account urban context and forms. Optimal orientation of the canopy shows an increase of 5% of the passive solar radiation from original orientation, 180 degrees rotation from first orientation straight south. This value goes lower when stories are added to the urban context. A rotation of 90 degrees from the first orientation shows a decrease of 6 to 15% in solar passive gain. Densification of the urban canopy by adding stories to the buildings results in a loss up to 65% of the solar gain for the first story. It is showed that solar passive energy has a low ratio of 5% for space heating for old buildings, 1960 constructions. Today's buildings have a difference between passive solar energy and heating demand of 10 to 75% depending on the model and location.

  16. The carbon cycle in a land surface model: modelling, validation and implementation at a global scale; Cycle du carbone dans un modele de surface continentale: modelisation, validation et mise en oeuvre a l'echelle globale

    Energy Technology Data Exchange (ETDEWEB)

    Gibelin, A.L

    2007-05-15

    ISBA-A-gs is an option of the CNRM land surface model ISBA which allows for the simulation of carbon exchanges between the terrestrial biosphere and the atmosphere. The model was implemented for the first time at the global scale as a stand-alone model. Several global simulations were performed to assess the sensitivity of the turbulent fluxes and Leaf Area Index to a doubling of the CO{sub 2} atmospheric concentration, and to the climate change simulated by the end of the 21. century. In addition, a new option of ISBA, referred to as ISBA-CC, was developed in order to simulate a more detailed ecosystem respiration by separating the autotrophic respiration and the heterotrophic respiration. The vegetation dynamics and the carbon fluxes were validated at a global scale using satellite datasets, and at a local scale using data from 26 sites of the FLUXNET network. All these results show that the model is sufficiently realistic to be coupled with a general circulation model, in order to account for interactions between the terrestrial biosphere, the atmosphere and the carbon cycle. (author)

  17. Multi-scale interaction between magnetic islands and microturbulence in magnetized plasmas; Modelisation et simulation de l'interaction multi-echelle entre ilots magnetiques et la microturbulence dans les plasmas de fusion magnetises

    Energy Technology Data Exchange (ETDEWEB)

    Muraglia, M.

    2009-10-15

    In a tokamak, it exists many kinds of instability at the origin of a damage of the confinement and worst of a lost of a confinement. This work presents a study of the dynamics of a magnetic island in presence of turbulence in magnetized plasmas. More precisely, the goal is to understand the multi-scales interaction between turbulence, generated by a pressure gradient and the magnetic field curvature, and a magnetic island formed thanks to a tearing mode. Thanks to the derivation of a 2-dimensional slab model taking into account both tearing and interchange instabilities, theoretical and numerical linear studies show the pressure effect on the magnetic island linear formation and show interchange modes are stabilized in presence of a strong magnetic field. Then, a numerical nonlinear study is presented in order to understand how the interchange mechanism affects the nonlinear dynamics of a magnetic island. It is shown that the pressure gradient and the magnetic field curvature affect strongly the nonlinear evolution of a magnetic island through dynamics bifurcations. The nature of these bifurcations should be characterized in function of the linear situation. Finally, the last part of this work is devoted to the study of the origin of the nonlinear poloidal rotation of the magnetic island. A model giving the different contributions to the rotation is derived. It is shown, thanks to the model and to the numerical studies, that the nonlinear rotation of the island is mainly governed by the ExB poloidal flow and/or by the nonlinear diamagnetic drift. (author)

  18. Quantification of the greenhouse effect gases at the territorial scale. Final report; Quantification des emissions de gaz a effet de serre a l'echelle territoriale. Rapport final

    Energy Technology Data Exchange (ETDEWEB)

    Magnin, G.; Lacassagne, S

    2003-07-01

    An efficient action against the greenhouse effect needs the implication of the local collectivities. To implement appropriate energy policies, deciders need information and tools to quantify the greenhouse gases and evaluate the obtained results of their greenhouse gases reduction policies. This study is a feasibility study of the tools realization, adapted to the french context. It was done in three steps: analysis of the existing tools, application to the french context and elaboration of the requirements of appropriate tools. This report presents the study methodology, the information analysis and the conclusions. (A.L.B.)

  19. Inverse modeling for the optimization of primary sources of atmospheric pollution at a regional scale; Modelisation inverse pour l'optimisation des sources primaires de pollution atmospherique a l'echelle regionale

    Energy Technology Data Exchange (ETDEWEB)

    Pison, I.

    2005-12-15

    Atmospheric pollution at a regional scale is the result of various interacting processes: emissions, chemistry, transport, mixing and deposition of gaseous species. The forecast of air quality is then performed by models, in which the emissions are taken into account through inventories. The simulated pollutant concentrations depend highly on the emissions that are used. Now inventories that represent them have large uncertainties. Since it would be difficult today to improve their building methodologies, there remains the possibility of adding information to existing inventories. The optimization of emissions uses the information that is available in measurements to get the inventory that minimizes the difference between simulated and measured concentrations. A method for the inversion of anthropogenic emissions at a regional scale, using network measurements and based on the CHIMERE model and its adjoint, was developed and validated. A kriging technique allows us to optimize the use of the information available in the concentration space. Repeated kriging-optimization cycles increase the quality of the results. A dynamical spatial aggregation technique makes it possible to further reduce the size of the problem. The NO{sub x} emissions from the inventory elaborated by AIRPARIF for the Paris area were inverted during the summers of 1998 and 1999, the events of the ESQUIF campaign being studied in detail. The optimization reduces large differences between simulated and measured concentrations. Generally, however, the confidence level of the results decreases with the density of the measurement network. Therefore, the results with the higher confidence level correspond to the most intense emission fluxes of the Paris area. On the whole domain, the corrections to the average emitted mass and to the matching time profiles are consistent with the estimate of 15% obtained during the ESQUIF campaign. (author)

  20. A campaign to study atmospheric pollution at the regional scale: the Escompte programme; Une experience d'etude de la pollution atmospherique a l'echelle regionale. Le programme Escompte

    Energy Technology Data Exchange (ETDEWEB)

    Durand, P. [Meteo-France - Centre National de Recherches Meteorologiques, Centre National de la Recherche Scientifique (CNRS URA 1357), 31 - Toulouse (France); Cros, B. [Observatoire Midi-Pyrenees, Lab. d' Aerologie, Centre National de la Recherche Scientifique (CNRS UMR 5560), 31 - Toulouse (France)

    2004-02-01

    The Escompte programme was set up to improve and validate regional scale chemistry-transport numerical models. During summer 2001, an ambitious field campaign collected data on the meteorological and chemical parameters of the atmosphere during some photo-oxidant pollution events. Performed in the region of Marseille city and Berre lake, this campaign deployed a huge quantity of instruments, and constitutes one of the major operations in this field. (authors)

  1. Modeling of atmospheric pollution at the regional scale: application to the Esquif campaign; Modelisation a l'echelle regionale de la pollution atmospherique: application a la campagne Esquif

    Energy Technology Data Exchange (ETDEWEB)

    Sarrat, C.

    2003-06-01

    The Esquif experimental campaign (study and simulation of air quality in Ile-de-France (Paris region, France)) took place between 1998 and 2000 with the aim of better understanding the dynamical and chemical processes leading to atmospheric pollution peaks in Paris. The construction of a rich and diversified database (12 periods of intensive monitoring (PIM)) has been implemented with the aim of improving the existing chemical-transport models in general and air quality forecasting models in particular. In the framework of this study, the data collected during PIM 2 and 6 were used for the validation and analysis of situations of intensive pollution, simulated with the meso-scale numerical meteorological and chemical model Meso-NHC. The validation of both the dynamic fields (temperature and potential temperature, wind, height of the boundary layer) and the chemical fields (mainly O{sub 3}, NO{sub x}, NO{sub y}, PAN, isoprene) of the model allows to discuss some of the parameters of the model such as the initialization, the boundary forcing and the resolution. Then, a study of the dynamical processes allows to analyze the formation and reinforcement of the pollution conditions. Stress is put on the interaction of the regional scale processes with the photochemical pollution events. In this framework, the dynamical-chemical interaction processes are analyzed in detail, in particular when pollution levels are reinforced by the intrusion of residual ozone inside the convective boundary layer, dragged by the turbulence. Also, the impact of the urban hot island and of the urban wind on the redistribution of primary and secondary pollutants are considered. An analysis of the impact of hydrocarbons of biogenic origin on the ozone concentrations with respect to the temperature and to the presence of primary compounds has been performed for the PIM 2 and 6 of the Esquif campaign. (J.S.)

  2. Thermal large Eddy simulations and experiments in the framework of non-isothermal blowing; Simulations des grandes echelles thermiques et experiences dans le cadre d'effusion anisotherme

    Energy Technology Data Exchange (ETDEWEB)

    Brillant, G

    2004-06-15

    The aim of this work is to study thermal large-eddy simulations and to determine the nonisothermal blowing impact on a turbulent boundary layer. An experimental study is also carried out in order to complete and validate simulation results. In a first time, we developed a turbulent inlet condition for the velocity and the temperature, which is necessary for the blowing simulations.We studied the asymptotic behavior of the velocity, the temperature and the thermal turbulent fluxes in a large-eddy simulation point of view. We then considered dynamics models for the eddy-diffusivity and we simulated a turbulent channel flow with imposed temperature, imposed flux and adiabatic walls. The numerical and experimental study of blowing permitted to obtain to the modifications of a thermal turbulent boundary layer with the blowing rate. We observed the consequences of the blowing on mean and rms profiles of velocity and temperature but also on velocity-velocity and velocity-temperature correlations. Moreover, we noticed an increase of the turbulent structures in the boundary layer with blowing. (author)

  3. Dynamical and multi scale approach of the relationships between the aquatic organisms and their environment; Approche multi-echelles des relations dynamiques entre les organismes aquatiques et leur environnement

    Energy Technology Data Exchange (ETDEWEB)

    Daufresne, M

    2004-03-15

    Identifying the causes of spatio-temporal variations in communities has long been at the core of ecological research. I have studied the dynamic relationship between stream-living organisms and their environment. I have shown, for the first time in large stream ecosystems, the effect of climate change on fish and invertebrate community structures. At the population scale, I enhanced understanding of the influence of high discharge level during emergence on brown trout population dynamics. At the individual scale, an experimental study improved understanding of the influence of stream velocity on downstream displacement of emerging trout. Finally, this work highlighted that environmental constraints could have paradoxical effects at different biological or temporal scales. (author)

  4. Development of a single ion micro-irradiation facility for experimental radiobiology at cell level; Developpement d'une ligne d'irradiation microfaisceau en mode ion par ion pour la radiobiologie experimentale a l'echelle cellulaire

    Energy Technology Data Exchange (ETDEWEB)

    Barberet, Ph

    2003-10-01

    A micro-irradiation device has been developed for radiobiology applications at the scale of the cell. This device is based on an upgrade of an existing micro-beam line that was already able to deliver a 1 to 3 MeV proton or alpha beam of low intensity and whose space resolution is lower than 1 micrometer in vacuum. The important part of this work has been the development of an irradiation stage designed to fit on the micro-probe and able to deliver ions in the air with an absolute accuracy of a few micrometers. A program has been set up to monitor the complete irradiation line in testing and in automatic irradiation operating phases. Simulation tools based on Monte-Carlo calculations have been validated through comparisons with experimental data particularly in the field of spatial resolution and of the number of ions delivered. The promising results show the possibility in a near future to use this tool to study the response of cells to very low irradiation doses down to the extreme limit of one ion per cell.

  5. The carbon cycle in a land surface model: modelling, validation and implementation at a global scale; Cycle du carbone dans un modele de surface continentale: modelisation, validation et mise en oeuvre a l'echelle globale

    Energy Technology Data Exchange (ETDEWEB)

    Gibelin, A L

    2007-05-15

    ISBA-A-gs is an option of the CNRM land surface model ISBA which allows for the simulation of carbon exchanges between the terrestrial biosphere and the atmosphere. The model was implemented for the first time at the global scale as a stand-alone model. Several global simulations were performed to assess the sensitivity of the turbulent fluxes and Leaf Area Index to a doubling of the CO{sub 2} atmospheric concentration, and to the climate change simulated by the end of the 21. century. In addition, a new option of ISBA, referred to as ISBA-CC, was developed in order to simulate a more detailed ecosystem respiration by separating the autotrophic respiration and the heterotrophic respiration. The vegetation dynamics and the carbon fluxes were validated at a global scale using satellite datasets, and at a local scale using data from 26 sites of the FLUXNET network. All these results show that the model is sufficiently realistic to be coupled with a general circulation model, in order to account for interactions between the terrestrial biosphere, the atmosphere and the carbon cycle. (author)

  6. EarthFinder: A Precise Radial Velocity Survey Probe Mission of our Nearest Stellar Neighbors for Earth-Mass Habitable Zone Analogs Using High-Resolution UV-Vis-NIR Echelle Spectroscopy on a Space Platform

    Science.gov (United States)

    Plavchan, Peter; EarthFinder Team

    2018-01-01

    We are investigating the science case for a 1.0-1.4 meter space telescope to survey the closest, brightest FGKM main sequence stars to search for Habitable Zone (HZ) Earth analogs using the precise radial velocity (PRV) technique at a precision of 1-10 cm/s. Our baseline instrument concept uses two diffraction-limited spectrographs operating in the 0.4-1.0 microns and 1.0-2.4 microns spectral regions each with a spectral resolution of R=150,000~200,000, with the possibility of a third UV arm. Because the instrument utilizes a diffraction-limited input beam, the spectrograph would be extremely compact, less than 50 cm on a side, and illumination can be stabilized with the coupling of starlight into single mode fibers. With two octaves of wavelength coverage and a cadence unimpeded by any diurnal, seasonal, and atmospheric effects, EarthFinder will offer a unique platform for recovering stellar activity signals from starspots, plages, granulation, etc. to detect exoplanets at velocity semi-amplitudes currently not obtainable from the ground. Variable telluric absorption and emission lines may potentially preclude achieving PRV measurements at or below 10 cm/s in the visible and advantage compared to an annual ~3-6 month observing season from the ground for mitigating stellar activity and detecting the orbital periods of HZ Earth-mass analogs (e.g. ~6-months to ~2 years). Finally, we are compiling a list of ancillary science cases for the observatory, ranging from asteroseismology to the direct measurement of the expansion of the Universe.

  7. Transfer of reactive solutes in the unsaturated zone of soils at several observation scales; Transfert de solutes reactifs dans la zone non-saturee des sols a differentes echelles d'observation

    Energy Technology Data Exchange (ETDEWEB)

    Limousin, G

    2006-10-15

    The transfer of contaminants in the unsaturated zone of soils is driven by numerous mechanisms. Field studies are sometimes difficult to set up, and so the question is raised about the reliability of laboratory measurements for describing a field situation. The nuclear power plant at Brennilis (Finistere, France) has been chosen to study the transfer of strontium, cobalt and inert tracers in the soil of this industrial site. Several observation scales have been tested (batch, stirred flow-through reactor, sieved-soil column, un-repacked or repacked soil-core lysimeter, field experiments) in order to determine, at each scale, the factors that influence the transfer of these contaminants, then to verify the adequacy between the different observation scales and their field representativeness. Regarding the soil hydrodynamic properties, the porosity, the water content in the field, the pore water velocity at the water content in the field, the saturation hydraulic conductivity and the dispersion coefficient of this embanked soil are spatially less heterogeneous than those of agricultural or non-anthropic soils. The results obtained with lysimeter and field experiments suggest that hydrodynamics of this unstructured soil can be studied on a repacked sample if the volume is high compared to the rare big-size stones. Regarding the chemical soil-contaminant interactions, cobalt and strontium isotherms are non-linear at concentration higher than 10{sup -4} mol.L{sup -1}, cobalt adsorption and desorption are fast and independent on pH. On the contrary, at concentration lower than 3.5 x 10{sup -6} mol.L{sup -1}, cobalt and strontium isotherms are linear, cobalt desorption is markedly slower than adsorption and both cobalt partition coefficient at equilibrium and its reaction kinetics are highly pH-dependent. For both elements, the results obtained with batch, stirred flow-through reactor and sieved-soil column are in adequacy. However, strontium batch adsorption measurements at equilibrium do not make possible to describe the results of field transfer experiments. (author)

  8. Scale interactions in economics: application to the evaluation of the economic damages of climatic change and of extreme events; Interactions d'echelles en economie: application a l'evaluation des dommages economiques du changement climatique et des evenements extremes

    Energy Technology Data Exchange (ETDEWEB)

    Hallegatte, S

    2005-06-15

    Growth models, which neglect economic disequilibria, considered as temporary, are in general used to evaluate the damaging effects generated by climatic change. This work shows, through a series of modeling experiences, the importance of disequilibria and of endogenous variability of economy in the evaluation of damages due to extreme events and climatic change. It demonstrates the impossibility to separate the evaluation of damages from the representation of growth and of economic dynamics: the comfort losses will depend on both the nature and intensity of impacts and on the dynamics and situation of the economy to which they will apply. Thus, the uncertainties about the damaging effects of future climatic changes come from both scientific uncertainties and from uncertainties about the future organization of our economies. (J.S.)

  9. A High Resolution Solar Spectrograph for the Berkeley Undergraduate Astronomy Lab

    Science.gov (United States)

    Strickler, R.; Bresloff, C.; Graham, J.

    2005-05-01

    The discovery of extra-solar planets has stimulated interest amongst undergraduates. The Doppler method for detecting exoplanets requires extraction of signals at the 1/1000 of a pixel level. To illustrate this technique, we used a newly built spectrometer to extract sub-pixel Doppler shifts in the solar photosphere. We have used this spectrograph to measure the velocity gradient across the sun and hence infer the solar radius. The limb-to-limb Doppler shift is only 1.8 km/s. A spectral resolution > 100,000 would be required to manifest this motion. Achieving such high spectral resolution is unnecessary since even a small telescope can record high SNR (> 100) spectra. Within a few seconds it is possible to discern solar rotational Doppler shifts at resolutions as low as 10,000. We must also understand coordinate transformation to convert the Doppler signal along the observed diameter to the equatorial rotation speed assuming solid body rotation. The spectrograph system includes an 8-inch Schmidt-Cassegrain stationary telescope; a 100-micron diameter multi-mode fiber; aspheric f-number reformatting optics; a collimating lens; a 110 mm, 80 grooves/mm, θ blaze = 64.5 degree replica echelle grating; and an Apogee 1024 x 1024 thermo-electrically cooled CCD. The spectrometer optics are mounted on a 5-ft x 3-ft optical bench. Operating the spectrometer remotely using VNC and a wireless laptop, we pointed the telescope so that the fiber scanned across a diameter of the solar disk while the CCD took repeated exposures. Although we were "guinea pigs," using the spectrograph for the first time in a class, it worked remarkably well. Combining measurement of the solar radius with observation of the rotation period from sunspots, the earth-sun distance can be deduced. In the future, students may measure the eccentricity of earth's orbit by measuring the sun's radial velocity over the course of a year. This work was supported by the NSF through award DUE-0311536.

  10. CARMENES instrument overview

    Science.gov (United States)

    Quirrenbach, A.; Amado, P. J.; Caballero, J. A.; Mundt, R.; Reiners, A.; Ribas, I.; Seifert, W.; Abril, M.; Aceituno, J.; Alonso-Floriano, F. J.; Ammler-von Eiff, M.; Antona Jiménez, R.; Anwand-Heerwart, H.; Azzaro, M.; Bauer, F.; Barrado, D.; Becerril, S.; Béjar, V. J. S.; Benítez, D.; Berdiñas, Z. M.; Cárdenas, M. C.; Casal, E.; Claret, A.; Colomé, J.; Cortés-Contreras, M.; Czesla, S.; Doellinger, M.; Dreizler, S.; Feiz, C.; Fernández, M.; Galadí, D.; Gálvez-Ortiz, M. C.; García-Piquer, A.; García-Vargas, M. L.; Garrido, R.; Gesa, L.; Gómez Galera, V.; González Álvarez, E.; González Hernández, J. I.; Grözinger, U.; Guàrdia, J.; Guenther, E. W.; de Guindos, E.; Gutiérrez-Soto, J.; Hagen, H.-J.; Hatzes, A. P.; Hauschildt, P. H.; Helmling, J.; Henning, T.; Hermann, D.; Hernández Castaño, L.; Herrero, E.; Hidalgo, D.; Holgado, G.; Huber, A.; Huber, K. F.; Jeffers, S.; Joergens, V.; de Juan, E.; Kehr, M.; Klein, R.; Kürster, M.; Lamert, A.; Lalitha, S.; Laun, W.; Lemke, U.; Lenzen, R.; López del Fresno, Mauro; López Martí, B.; López-Santiago, J.; Mall, U.; Mandel, H.; Martín, E. L.; Martín-Ruiz, S.; Martínez-Rodríguez, H.; Marvin, C. J.; Mathar, R. J.; Mirabet, E.; Montes, D.; Morales Muñoz, R.; Moya, A.; Naranjo, V.; Ofir, A.; Oreiro, R.; Pallé, E.; Panduro, J.; Passegger, V.-M.; Pérez-Calpena, A.; Pérez Medialdea, D.; Perger, M.; Pluto, M.; Ramón, A.; Rebolo, R.; Redondo, P.; Reffert, S.; Reinhardt, S.; Rhode, P.; Rix, H.-W.; Rodler, F.; Rodríguez, E.; Rodríguez-López, C.; Rodríguez-Pérez, E.; Rohloff, R.-R.; Rosich, A.; Sánchez-Blanco, E.; Sánchez Carrasco, M. A.; Sanz-Forcada, J.; Sarmiento, L. F.; Schäfer, S.; Schiller, J.; Schmidt, C.; Schmitt, J. H. M. M.; Solano, E.; Stahl, O.; Storz, C.; Stürmer, J.; Suárez, J. C.; Ulbrich, R. G.; Veredas, G.; Wagner, K.; Winkler, J.; Zapatero Osorio, M. R.; Zechmeister, M.; Abellán de Paco, F. J.; Anglada-Escudé, G.; del Burgo, C.; Klutsch, A.; Lizon, J. L.; López-Morales, M.; Morales, J. C.; Perryman, M. A. C.; Tulloch, S. M.; Xu, W.

    2014-07-01

    This paper gives an overview of the CARMENES instrument and of the survey that will be carried out with it during the first years of operation. CARMENES (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Echelle Spectrographs) is a next-generation radial-velocity instrument under construction for the 3.5m telescope at the Calar Alto Observatory by a consortium of eleven Spanish and German institutions. The scientific goal of the project is conducting a 600-night exoplanet survey targeting ~ 300 M dwarfs with the completed instrument. The CARMENES instrument consists of two separate echelle spectrographs covering the wavelength range from 0.55 to 1.7 μm at a spectral resolution of R = 82,000, fed by fibers from the Cassegrain focus of the telescope. The spectrographs are housed in vacuum tanks providing the temperature-stabilized environments necessary to enable a 1 m/s radial velocity precision employing a simultaneous calibration with an emission-line lamp or with a Fabry-Perot etalon. For mid-M to late-M spectral types, the wavelength range around 1.0 μm (Y band) is the most important wavelength region for radial velocity work. Therefore, the efficiency of CARMENES has been optimized in this range. The CARMENES instrument consists of two spectrographs, one equipped with a 4k x 4k pixel CCD for the range 0.55 - 1.05 μm, and one with two 2k x 2k pixel HgCdTe detectors for the range from 0.95 - 1.7μm. Each spectrograph will be coupled to the 3.5m telescope with two optical fibers, one for the target, and one for calibration light. The front end contains a dichroic beam splitter and an atmospheric dispersion corrector, to feed the light into the fibers leading to the spectrographs. Guiding is performed with a separate camera; on-axis as well as off-axis guiding modes are implemented. Fibers with octagonal cross-section are employed to ensure good stability of the output in the presence of residual guiding errors. The

  11. Conservative treatment of soft tissue sarcomas of the extremities. Functional evaluation with LENT-SOMA scales and the Enneking score; Traitement conservateur des sarcomes des tissus mous des membres. Evaluation du resultat fonctionnel selon l'echelle LENT-SOMA et le score de Enneking

    Energy Technology Data Exchange (ETDEWEB)

    Tawfiq, N.; Lagarde, P.; Thomas, L.; Kantor, G. [Institut Bergonie, Centre Regional de Lutte Contre le Cancer, Service de Radiotherapie, 33 - Bordeaux (France); Stockle, E. [Institut Bergonie, Centre Regional de Lutte Contre le Cancer, Service de Chirurgie, 33 - Bordeaux (France); Bui, B.N. [Institut Bergonie, Centre Regional de Lutte Contre le Cancer, Service d' Oncologie Medicale, 33 - Bordeaux (France)

    2000-12-01

    Objective. - The aim of this prospective study is the feasibility of late effects assessment by LENT-SOMA scales after conservative treatment of soft tissue sarcomas of the extremities and a comparison with the functional evaluation by the Enneking score. Patients and methods. - During the systematic follow-up consultations, a series of 32 consecutive patients was evaluated in terms of late effects by LENT SOMA scales and functional results by the Enneking score. The median time after treatment was 65 months. The treatment consisted of conservative surgery (all cases) followed by radiation therapy (29 cases), often combined with adjuvant therapy (12 concomitant radio-chemotherapy association cases out of 14). The assessment of the toxicity was retrospective for acute effects and prospective for the following late tissue damage: skin/subcutaneous tissues, muscles/soft tissues and peripheral nerves. Results. -According to the Enneking score, the global score for the overall series was high (24/30) despite four the scores zero for the psychological acceptance. According to LENT SOMA scales, a low rate of severe sequelae (grade 3-4) was observed. The occurrence of high-grade sequelae and their functional consequences were not correlated with quality of exeresis, dose of radiotherapy or use of concomitant chemotherapy. A complementarity was observed between certain factors of the Enneking score and some criteria of the LENTSOMA scales, especially of muscles/soft tissues. Conclusion. -The good quality of functional results was confirmed by the two mean scoring systems for late normal tissue damage. The routine use of LENT-SOMA seems to be more time consuming than the Enneking score (mean time of scoring: 1 3 versus five minutes). The LENT-SOMA scales are aimed at a detailed description of late toxicity and sequelae while the Enneking score provides a more global evaluation, including the psychological acceptance of treatment. The late effects assessment by the LENT-SOMA scales should be carried on in prospectives studies, especially in case of concomitant radio-chemotherapy. (author)

  12. Behaviour at the indicator scale of the elements Zr, Hf and 104, Nb,Ta and Pa (105) in very complexation media; Comportement a l`echelle des indicateurs des elements Zr, Hf, et 104, Nb, Ta, et Pa (105) en milieux tres complexants

    Energy Technology Data Exchange (ETDEWEB)

    Monroy Guzman, F. [Institut de Physique Nucleaire, CNRS - IN2P3 Universite Paris Sud, 91406 Orsay Cedex (France)

    1997-12-31

    In order to determine the chemical properties of the trans-actinide elements of Z = 104 and 105 in aqueous solutions we studied their behaviour to ion exchange resin in different complex media. Due to the very short lifetimes (some tens of seconds) et to the low yield of these elements (a few atoms per irradiation hour) only very fast radiochemical techniques can be used. These severe constraints impose comparative studies of these elements with their most likely homologues to be carried out. The corresponding homologues were the elements of group 4 (Zr and Hf) for the element 104 and the elements of group 5 (Nb and Ta) and also Pa for the element 105. The complexation properties of the elements at indicator scale were determined in the media of HF, NH{sub 4}/HClO{sub 4}, NH{sub 4}SCN/HClO{sub 4}, NH{sub 4}SCN/HF and HCl/HF by ion exchange chromatography. The studies in fluorides media allowed us to identify the complexes in solution and to explain the shape of the experimentally observed sorption curves. The decrease of sorption for higher acid concentration in case of HF/HCl medium was interpreted by formation of chloro-fluoro-complexes. In case of the mixture NH{sub 4}SCN/HF, the particularly pronounced anti-synergic effects were observed and discussed. At the same time studies of the Hf and Ta short-lived isotopes were carried out by means of the RACHEL facility operating by the Orsay Tandem accelerator. These realistic simulations allowed optimization of different production, transportation and separation stages of the trans-actinide elements. The two experiments of 104 element production showed that this element forms in HF very stable anionic complexes similarly to its homologues Zr and Hf. (authors). 181 refs.

  13. Impact of different forestry strategies on the function 'carbon wells on the forest planting. Simulation and modelization at the parcel scale; Impact de differentes strategies sylvicoles sur la fonction 'puits de carbone' des peuplements forestiers. Modelisation et simulation a l'echelle de la parcelle

    Energy Technology Data Exchange (ETDEWEB)

    Vallet, P

    2005-10-15

    In the framework of the carbon storage two forestry methods are analyzed by the author: the standing capitalization (slowing of the crops) and the spices substitution (slow growing species by fast growing species). The construction of a model taking into account the all stage of the carbon implication (biomass, soil, forest products) offers simulation and quantitative results on these methods. (A.L.B.)

  14. Rating of transport and radiation source events. Draft additional guidance for the INES national officers for pilot use and feedback; Echelle de classement des incidents de radioprotection: document d'application du systeme international propose par l'AIEA pour les sources radioactives et les transports

    Energy Technology Data Exchange (ETDEWEB)

    NONE

    2004-09-15

    The International Nuclear Event Scale (INES) is a means for promptly communicating to the public in consistent terms the safety significance of any reported event associated with radioactive material and/or radiation and to any event occurring during the transport of radioactive material. As described in the 2001 Edition of the INES User.s Manual, events are classified on the scale at seven levels: the upper levels (4-7) are termed accidents. and the lower levels (1-3) incidents. Events which have no safety significance are classified below scale at Level 0 and termed deviations. An overview of the principles for the rating under INES together with flow charts summarizing the rating process is provided in Appendix I. The 2001 Edition of the INES User.s Manual provides some guidance for the rating of transport and radiation source events. At the technical meeting held in 2002 the INES National Officers requested the IAEA/NEA Secretariat to prepare additional guidance. Progress was reported at the Technical Meeting of the INES National Officers in March 2004 where preparation of this draft additional guidance was requested for pilot use. This note provides additional guidance on the rating of transport and radiation source events. It is for pilot use and feedback and is broadly consistent with the INES User.s Manual. It provides more detailed information and an expanded approach for the rating based on actual exposure of workers and members of the public. It is designed to be used as a self-standing document with limited need for reference to the INES User Manual. (author)

  15. Long-term alteration of R7T7 glass packages: development of a multi-scale approach to estimate the cracking; Alteration a long terme des colis de verres de type R7T7: developpement d'une approche multi-echelle pour evaluer l'impact de la fracturation

    Energy Technology Data Exchange (ETDEWEB)

    Chomat, L. [Paris-6 Univ. Pierre et Marie Curie, 75 (France)]|[CEA Valrho, Lab. d' Etudes du Comportement Long Terme des Materiaux de Conditionnement (LCLT), 30 - Marcoule (France)

    2006-07-01

    The aim of this work is to model the alteration and transport mechanisms implied in a cracks system and to deduce the evolution of the quantity of leached glass. This quantity will be then compared with those measured in leaching tests carried out on a package of industrial size. To estimate this quantity, several steps are required: 1)study of the local alteration inside a crack (according to the alteration parameters: flow, crack opening, pH..) or in a simple set of cracks (connexion); 2)description of a crack system at the package scale by tomography and SEM of bulk samples: opening, accessibility; 3)determination of the alteration parameters in the ALISE device (leaching device of industrial size in which is altered a package for 2001): temperatures gradients, convection, diffusion, pH..; 4)modelling: passage from the local alteration (crack) to the global alteration (package); 5)design and carrying out of a specific experiment to validate the model: control of the system of known cracks (opening, connectivity..) and of the alterations conditions (thermal gradient..); 6)confrontation of the model with the results obtained on ALISE and the specific experiment indicated in 5). The main experimental results are described. (O.M.)

  16. Report of study group 3.2 ''small scale LNG projects and modular systems''; Rapport du groupe d'etude 3.2 ''projets de GNL a petite echelle et systemes modulaires''

    Energy Technology Data Exchange (ETDEWEB)

    Larsen, B.

    2000-07-01

    This report details the work undertaken by Study Group 3.2 during the triennium 1997-2000. The Study Group has held three meetings in Stavanger (Norway) in Dubai (UAE) and in London (UK) between March 1998 and October 1999. The study group membership is listed in appendix 1. The subject treated by the Study Group is 'Small Scale LNG Projects and Modular Systems' The study report undertakes a general survey of: 1) the state of the art of the technology; 2) the potential market applications; 3) prospects for gas development and marginal fields. The study addresses three main items: a) Adapting regulation to compact LNG production systems (e.g. distances between equipment in fixed installations); b) LNG production in a marine environment; c) The need for substantial cost reductions. The questions that are addressed in this study report are: Will small scale LNG projects be economically viable? When an onshore industry moves offshore - which standards are to be applied? (author)

  17. A 3 D regional scale photochemical air quality model application to a 3 day summertime episode over Paris; Un modele photochimique 3D de qualite de l`air a l`echelle regionale. Application a un episode de 3 jours a Paris en ete

    Energy Technology Data Exchange (ETDEWEB)

    Jaecker-Voirol, A.; Lipphardt, M.; Martin, B.; Quandalle, Ph.; Salles, J. [Institut Francais du Petrole (IFP), 92 - Rueil-Malmaison (France); Carissimo, B.; Dupont, P.M.; Musson-Genon, L.; Riboud, P.M. [Electricite de France (EDF), 78 - Chatou (France). Direction des Etudes et Recherches; Aumont, B.; Bergametti, G.; Bey, I.; Toupanse, G. [Paris-12 Univ., 94 - Creteil (France). Laboratoire interuniversitaire des systemes atmospheriques]|[Paris-7 Univ., 75 (France)

    1998-03-01

    This paper presents AZUR, a 3D Eulerian photochemical air quality model for the simulation of air pollution in urban and semi-urban areas. The model tracks gas pollutant species emitted into the atmosphere by transportation and industrial sources, it computes the chemical reactions of these species under varying meteorological conditions (photolysis, pressure, temperature, humidity), their transport by wind and their turbulent diffusion as a function of air stability. It has a modular software structure which includes several components dedicated to specific processes: MERCURE, a meso-scale meteorological model to compute the wind field, turbulent diffusion coefficients, and other meteorological parameters; MIEL, an emission inventory model describing the pollutant fluxes from automotive transportation, domestic and industrial activities; MoCA a photochemical gas phase model describing the chemistry of ozone, NO{sub x}, an hydrocarbon compounds; AIRQUAL, a 3D Eulerian model describing the transport by mean wind flux and air turbulent diffusion of species in the atmosphere, associated with a Gear type chemical equation solver. The model has been applied to a 3-day summertime episode over Paris area. Simulation results are compared to ground level concentration measurements performed by the local monitoring network (Airparif). (authors) 22 refs.

  18. Behaviour at the indicator scale of the elements Zr, Hf and 104, Nb,Ta and Pa (105) in very complexation media; Comportement a l`echelle des indicateurs des elements Zr, Hf, et 104, Nb, Ta, et Pa (105) en milieux tres complexants

    Energy Technology Data Exchange (ETDEWEB)

    Monroy Guzman, F [Institut de Physique Nucleaire, CNRS - IN2P3 Universite Paris Sud, 91406 Orsay Cedex (France)

    1998-12-31

    In order to determine the chemical properties of the trans-actinide elements of Z = 104 and 105 in aqueous solutions we studied their behaviour to ion exchange resin in different complex media. Due to the very short lifetimes (some tens of seconds) et to the low yield of these elements (a few atoms per irradiation hour) only very fast radiochemical techniques can be used. These severe constraints impose comparative studies of these elements with their most likely homologues to be carried out. The corresponding homologues were the elements of group 4 (Zr and Hf) for the element 104 and the elements of group 5 (Nb and Ta) and also Pa for the element 105. The complexation properties of the elements at indicator scale were determined in the media of HF, NH{sub 4}/HClO{sub 4}, NH{sub 4}SCN/HClO{sub 4}, NH{sub 4}SCN/HF and HCl/HF by ion exchange chromatography. The studies in fluorides media allowed us to identify the complexes in solution and to explain the shape of the experimentally observed sorption curves. The decrease of sorption for higher acid concentration in case of HF/HCl medium was interpreted by formation of chloro-fluoro-complexes. In case of the mixture NH{sub 4}SCN/HF, the particularly pronounced anti-synergic effects were observed and discussed. At the same time studies of the Hf and Ta short-lived isotopes were carried out by means of the RACHEL facility operating by the Orsay Tandem accelerator. These realistic simulations allowed optimization of different production, transportation and separation stages of the trans-actinide elements. The two experiments of 104 element production showed that this element forms in HF very stable anionic complexes similarly to its homologues Zr and Hf. (authors). 181 refs.

  19. Development of a single ion micro-irradiation facility for experimental radiobiology at cell level; Developpement d'une ligne d'irradiation microfaisceau en mode ion par ion pour la radiobiologie experimentale a l'echelle cellulaire

    Energy Technology Data Exchange (ETDEWEB)

    Barberet, Ph

    2003-10-01

    A micro-irradiation device has been developed for radiobiology applications at the scale of the cell. This device is based on an upgrade of an existing micro-beam line that was already able to deliver a 1 to 3 MeV proton or alpha beam of low intensity and whose space resolution is lower than 1 micrometer in vacuum. The important part of this work has been the development of an irradiation stage designed to fit on the micro-probe and able to deliver ions in the air with an absolute accuracy of a few micrometers. A program has been set up to monitor the complete irradiation line in testing and in automatic irradiation operating phases. Simulation tools based on Monte-Carlo calculations have been validated through comparisons with experimental data particularly in the field of spatial resolution and of the number of ions delivered. The promising results show the possibility in a near future to use this tool to study the response of cells to very low irradiation doses down to the extreme limit of one ion per cell.

  20. Hydro-mechanical coupling and transport in Meuse/Haute-Marne argillite: experimental and multi-scale approaches; Couplage hydro-me canique et transfert dans l'argilite de Meuse/Haute-Marne: approches experimentale et multi-echelle

    Energy Technology Data Exchange (ETDEWEB)

    Cariou, S.

    2010-07-15

    This thesis deals with the hydro-mechanical behaviour of argillite. Classical Biot theory is shown to be badly adapted to the case of argillite. An original state equation is then built by use of homogenization tools, and takes into account the microstructure of argillite as well as physical phenomena happening inside the material, like the swelling overpressure inside the clay particles or the capillary effects in the porous network. This state equation explains some experiments which were not by the classical Biot theory. It is then improved by integrating the experimental data that are the dependency of the elasticity tensor with the saturation degree and the existence of a porosity surrounding the inclusions. Combined with the monitoring of length variation under hydric loading, this relevant state equation permits one to determine the Biot tensor of argillite. Since this state equation is coupled with the hydric state of the material, one is interested in modelling the variation of the saturation degree during a drying process. Two transport models are studied and compared, then a model for the porous network is proposed in order to explain the unusual permeability measurements. (author)

  1. Large-eddy simulation and Lagrangian stochastic modelling of solid particle and droplet dispersion and mixing. Application to atmospheric pollution; Dispersion et melange turbulents de particules solides et de gouttelettes par une simulation des grandes echelles et une modelisation stochastique lagrangienne. Application a la pollution de l'atmosphere

    Energy Technology Data Exchange (ETDEWEB)

    Vinkovic, I.

    2005-07-15

    In order to study atmospheric pollution and the dispersion of industrial stack emissions, a large eddy simulation with the dynamic Smagorinsky-Germano sub-grid-scale model is coupled with Lagrangian tracking of fluid particles containing scalar, solid particles and droplets. The movement of fluid particles at a sub-grid level is given by a three-dimensional Langevin model. The stochastic model is written in terms of sub-grid-scale statistics at a mesh level. By introducing a diffusion model, the coupling between the large-eddy simulation and the modified three-dimensional Langevin model is applied to passive scalar dispersion. The results are validated by comparison with the wind-tunnel experiments of Fackrell and Robins (1982). The equation of motion of a small rigid sphere in a turbulent flow is introduced. Solid particles and droplets are tracked in a Lagrangian way. The velocity of solid particles and droplets is considered to have a large scale component (directly computed by the large-eddy simulation) and a sub-grid scale part. Because of inertia and gravity effects, solid particles and droplets, deviate from the trajectories of the surrounding fluid particles. Therefore, a modified Lagrangian correlation timescale is introduced into the Langevin model previously developed for the sub-grid velocity of fluid particles. Two-way coupling and collisions are taken into account. The results of the large-eddy simulation with solid particles are compared with the wind-tunnel experiments of Nalpanis et al. (1993) and of Taniere et al. (1997) on sand particles in saltation and in modified saltation, respectively. A model for droplet coalescence and breakup is implemented which allows to predict droplet interactions under turbulent flow conditions in the frame of the Euler/Lagrange approach. Coalescence and breakup are considered as a stochastic process with simple scaling symmetry assumption for the droplet radius, initially proposed by Kolmogorov (1941). At high-frequency of breakup/coalescence phenomena, this stochastic process is equivalent to the evolution of the probability density function of droplet radii, which is governed by a Fokker-Planck equation. The parameters of the model are obtained dynamically by relating them to the local resolved properties of the dispersed phase compared to the main fluid. Within each grid cell, mass conservation is applied. The model is validated by comparison with the agglomeration model of Ho and Sommerfeld (2002), the stochastic model for secondary breakup of Apte et al. (2003) and the experimental results on secondary breakup in a coaxial jet of Lasheras et al. (1998). The large-eddy simulation coupled with Lagrangian particle tracking and the model for droplet coalescence and breakup is applied to the study of the atmospheric dispersion of wet cooling tower plumes. The simulations are done for different droplet size distributions and volume fractions. We focused on the influence of these parameters on mean concentration, concentration variance and mass flux profiles. In order to gain insight into the transport of solid particles and droplets in a turbulent boundary layer flow, the evolution of particles that were initially distributed in an uniform way in the flow, is analysed. This simple test case represents a first approach for understanding the phenomena that take place within large clouds of pollution, sand storms or when fog disappears under the influence of a rising wind. The period and the size of regions of preferential concentration are determined. This regions are of particular interest in the study of atmospheric dispersion of particles because they can lead to pollution peaks in an otherwise, not polluted atmosphere. (author)

  2. Techniques of Large Scale Processing of Counting Data; Les techniques d'exploitation a grande echelle des donnees de comptage; Tekhnika obrabotki dannykh izmerenij, provodyashchejsya v bol'shikh masshtabakh; Tecnicas de tratamiento en gran escala de los datos obtenidos en el recuento

    Energy Technology Data Exchange (ETDEWEB)

    Manov, G G; Eads, D L [Reactor Monitoring Center, Tracerlab Inc., Richmond, CA (United States)

    1960-06-15

    The problems of a laboratory performing over 10.000 radionuclide analyses per year each of which requires a high degree of accuracy, but below that required in absolute standardization, call for special requirements in data handling and in data processing. Typical measurements involve mixtures of {alpha} emitters and multi-channel pulse-height analyses, 2 {pi} and 4 {pi} {beta} counting, {pi}-{gamma} coincidence measurements. Efficient use of instruments for measuring low levels of activity is achieved by the technique of multi-plexing with magnetic tape storage and read-out. Arithmetical errors, particularly the troublesome ones involving inadvertent transposition of digits is virtually eliminated by the use of electronic calculators. In one typical operation involving a mixture of known nuclides, the gross counting data are fed into a machine which prints (reads-out) the answer on an electric typewriter. Alternatively, the results, if from a spectrometer, can be automatically plotted on an X-Y graph for further interpretive analysis. Block diagrams illustrating the sequence of steps are presented. Decay corrections are easily handled by discarding the concept of the Gregorian calendar and employing instead a vear in which the days are numbered consecutively beginning at midnight of the night of 31 December - 1 January, Greenwich Mean Time. For example, July 17, 1959, 3 : 5 PM Pacific Coast Daylight Saving Time is 198.920 days, and 2 : 30 PM October 16, 1959, Vienna time is 289.854. The advantages of being able to add, subtract, multiply or divide times expressed in this manner is apparent. The electronic circuit of a time clock based on this principle is described together with photographs. (author) [French] Dans un laboratoire qui fait chaque annee plus de 10.000 analyses de radionuclides, dont chacune doit avoir une grande precision, sans atteindre celle qui est requise aux fins de normalisation absolue, le depouillement et l'exploitation des donnees posent des problemes particuliers. On doit cour{alpha}amment proceder aux operations suivantes: mesures de melanges d'emetteurs a, analyses de hauteurs d'impulsions par multicanaux, comptage {beta} 2 {pi} et 4 {pi}, mesures par coincidences {beta}-{gamma}. On assure une utilisation efficace des instruments de mesure de faibles niveaux d'activite en recourant a la technique ''multiplex'' avec enregistrement sur bande magnetique et dispositif de lecture. Les erreurs de calcul, particulierement les fautes d'inattention difficiles a retrouver, comme la permutation de deux' chiffres, sont pratiquement eliminees par l'emploi de calculatrices electoniques. Dans une operation courante portant sur un melange de nuclides connus, les donnees brutes resultant du comptage sont communiquees a la calculatrice qui imprime la reponse finale au moyen d'une machine a ecrire electrique. Si les resultats proviennent d'un spectrometre, on peut egalement en obtenir automatiquement une representation graphique en coordonnees cartesiennes pour en faire l'analyse et en donner une interpretation plus poussee. Le memoire contient des schemas d'operations. Pour operer facilement les corrections de taux de desintegration, on remplace l'annee du calendrier gregorien par une annee dont les jours, sont numerotes consecutivement, et qui commence le 1er Janvier, a 0 heure de Greenwich. Par exemple, le 17 juillet 1959 a 15 h. 15 (heure d'ete de la cote du Pacifique) sera le jour 198, 920 et le 16 octobre 1959 a 14 h. 30 (heure de Vienne) sera le jour 289, 854. Les avantages qui decoulent de la possibilite d'ajouter, de retrancher, de multiplier et de diviser les temps exprimes de cette maniere sont evidents. Le circuit electronique d'une horloge fondee sur ce principe est decrit dans le memoire, qui contient en outre des photos. (author) [Spanish] En un laboratorio donde se tengan que efectuar anualmente mas de 10 000 analisis de radionuclidos con una precision elevada, pero no tanto como la necesaria en los trabajos de calibracion absoluta, el acopio, registro y tratamiento de los datos plantea problemas especiales. La metrologia de los radionuclidos suele comprender las siguientes operaciones tipicas: medicion de la actividad de mezclas de emisores {alpha}, determinacion de la amplitud de impulsos mediante analizadores de canales multiples, recuento {beta} 2 {pi} u 4 {pi} y mediciones {beta}-{gamma} por el metodo de coincidencias. El registro de datos en cintas magneticas y la lectura de los mismos con arreglo al sistema ''multiplex'' asegura el aprovechamient o racional de los instrumentos utilizados en la medicion de bajas actividades. Los errores aritmeticos, en especial las enojosas equivocaciones debidas a la transposicion inadvertida de cifras, quedan practicamente eliminados cuando se utilizan calculadoras electronicas. En una operacion corriente de medicion de una mezcla de nuclidos conocidos, los datos brutos obtenidos en el recuento se comunican a una calculadora que imprime el resultado mediante una maquina de escribir electrica. Si se trata de determinacione s espectrometricas, los resultados pueden representarse automaticament e en coordenadas cartesianas, lo que permite proceder a su analisis e interpretacion. En la memoria se reproducen esquemas que indican el orden de las operaciones. Las correcciones del tiempo de desintegracion se facilitan sustituyendo el ano del calendario gregoriano por un ano en que los dias estan numerados consecutivamente, comenzado a medianoche del 31 de deciembre (hora del meridiano de Greenwich). Asi las 15.05 horas del 17 de julio de 1959, hora de verano del Pacifico, se expresan, segun este sistema, como dia 198,920, y las 14.30 del 16 de octubre de 1959 hora centroeuropea), como dia 289,854. Es evidente la ventaja de este metodo, que permite sumar, testar, multiplicar o dividir los tiempos expresados con arreglo al mismo. Se describe el circuito electronico de un cronometro basado en este principio; la descripcion se ilustra con fotografias. (author) [Russian] Problemy, s kotorymi stalkivaetsya lyubaya laboratoriya, vypolnyayushchaya v god okolo 10 000 analizov radioaktivnykh izotopov, trebuyushchikh vysokoj stepeni tochnosti, krome neobkhodimost i priderzhivat's ya absolyutnoj standartizatsii, vyzyvayut spetsial'nuyu potrebnost' v materialakh, otnosyashchikhsya k nakopleniyu i obrabotke dannykh izmerenij. Tipichnye izmereniya vklyuchayut: izluchateli a{alpha}-chastits i mnogokanal'ny j amplitudnyj analizator impul'sov, otschet{beta}-izluchenij na 2 {pi} i 4 {pi}, registratsiyu sovpadenij {beta}-{gamma} izluchenij. Poleznoe ispol'zovanie priborov dlya izmereniya aktivnosti maloj moshchnosti dostigaetsya s pomoshch'yu tekhniki perekhoda na mnogokratnost ' s nakopleniem na magintnoj lente i s pomoshch'yu fotoehlementa. Arifmeticheski e oshibki i osobenno te, kotorye svyazany s perestanovkoj tsifr, fakticheski ustranyayutsya s pomoshch'yu ehlektronnykh schetnykh priborov. V odnoj iz tipichnykh operatsij v otneshenii smesi izvestnykh izotopov dannye po izmereniyam napravlyayutsya na mashinu, kotoraya pechataet otvet na ehlektricheskoj pishushchej mashinke. Sootvetstvenn o rezul'taty, esli oni dayutsya so spektrometra, mogut avtomaticheski nanosit'sya na osi koordinat dlya dal'nejshego analiza. Daetsya blok-skhema, illyustriruyushchaya posledovatel'nost ' predprinimaemy kh operatsij. Popravki na raspad mogut legko byt' sdelany posredstvom primeneniya dlya podschetov vmesto goda po Gregorianskom u kalendaryu takogo goda, v kotorom schet dnej nachinaetsya v polnoch' s 31 dekabrya na 1 yanvarya po grinvicheskomu standartnomu vremeni. Naprimer: 17-mu iyulya 1959 goda, 3 chasam 05 min. dnya po tikhookeanskom u dnevnomu vremeni po takoj sisteme budet sootvetstvovat ' 198, 920 dnya, a 2 ch. 30 m. dnya 16-go oktyabrya 1959 goda po Venskomu vremeni budet sootvetstvovat ' 289, 854 dnya. Ochevidny preimushchestva takogo metoda podscheta vsledstvie poyavlyayushchejsya vozmozhnosti skladyvat', vychitat', umnozhat' i delit'. Daetsya opisanie ehlektronnogo kontura chasov, osnovannogo na takogo roda printsipe i prilagayutsya fotografii. (author)

  3. Methodology of regional emission inventories: Application to the emission inventories of the ESCOMPTE experiment and to their regional extension to the PACA (Provence-Alpes-Cote-d'Azur) region; Methodologie d'etablissement de cadastres d'emissions a l'echelle regionale: application au cadastre escompte et a son extension a la region PACA

    Energy Technology Data Exchange (ETDEWEB)

    Francois, St.

    2004-06-01

    With the industrial revolution and then the massive use of fossil fuels, the air quality has been considerably worsening. Air quality is a complex function of meteorological situations (wind, sun radiation) and pollutant emissions. All those parameters must be accounted for modelling the reactive transports of pollutants in the atmosphere but only the anthropogenic emissions can be managed on a short time frame, as well concerning the composition of the flux as the emitted quantities. This overall modelling problematic emphasize the crucial role of emission databases in the air quality modelling processes, as diagnostic or prognostic tool for air quality issues. To obtain a consistent and realistic modelling, not only the emissions and meteorological data have to be taken take into account, especially the emissions in the proper chemical reaction mechanisms but the quality of the emission data is crucial. The starting point of our study was that few or no inventories exist, and from the ones available, they are not adapted to be used efficiently in regional air quality modelling. The resolution, especially regarding spatial emission distribution of the national inventories can not lead to proper input data for this kind of studies. Our study include both the method aspects (theoretical studies) and the operational aspects (applied studies) regarding the generation of high resolution spatial emission data (based on national statistical data standards) that can be used as suitable input data for meso-scale photochemical models of the reactive transport of pollutants. This work was part of the ESCOMPTE program, an unparalleled scientific in the domain of air quality experiment in France. Our tasks in this program also included a methodological transfer (accompanied with the software tools related to the emission databases) of the study to the local air quality monitoring authority (AIRMARAIX for the city of Marseille). This overall application proved the feasibility of high resolution regional emission inventories at a sustainable operational cost. (author)

  4. Scale interactions in economics: application to the evaluation of the economic damages of climatic change and of extreme events; Interactions d'echelles en economie: application a l'evaluation des dommages economiques du changement climatique et des evenements extremes

    Energy Technology Data Exchange (ETDEWEB)

    Hallegatte, S

    2005-06-15

    Growth models, which neglect economic disequilibria, considered as temporary, are in general used to evaluate the damaging effects generated by climatic change. This work shows, through a series of modeling experiences, the importance of disequilibria and of endogenous variability of economy in the evaluation of damages due to extreme events and climatic change. It demonstrates the impossibility to separate the evaluation of damages from the representation of growth and of economic dynamics: the comfort losses will depend on both the nature and intensity of impacts and on the dynamics and situation of the economy to which they will apply. Thus, the uncertainties about the damaging effects of future climatic changes come from both scientific uncertainties and from uncertainties about the future organization of our economies. (J.S.)

  5. Statistical Physics

    CERN Document Server

    Mandl, Franz

    1988-01-01

    The Manchester Physics Series General Editors: D. J. Sandiford; F. Mandl; A. C. Phillips Department of Physics and Astronomy, University of Manchester Properties of Matter B. H. Flowers and E. Mendoza Optics Second Edition F. G. Smith and J. H. Thomson Statistical Physics Second Edition E. Mandl Electromagnetism Second Edition I. S. Grant and W. R. Phillips Statistics R. J. Barlow Solid State Physics Second Edition J. R. Hook and H. E. Hall Quantum Mechanics F. Mandl Particle Physics Second Edition B. R. Martin and G. Shaw The Physics of Stars Second Edition A. C. Phillips Computing for Scient

  6. Statistics a guide to the use of statistical methods in the physical sciences

    CERN Document Server

    Barlow, Roger J

    1989-01-01

    The Manchester Physics Series General Editors: D. J. Sandiford; F. Mandl; A. C. Phillips Department of Physics and Astronomy, University of Manchester Properties of Matter B. H. Flowers and E. Mendoza Optics Second Edition F. G. Smith and J. H. Thomson Statistical Physics Second Edition F. Mandl Electromagnetism Second Edition I. S. Grant and W. R. Phillips Statistics R. J. Barlow Solid State Physics Second Edition J. R. Hook and H. E. Hall Quantum Mechanics F. Mandl Particle Physics Second Edition B. R. Martin and G. Shaw The Physics of Stars Second Edition A.C. Phillips Computing for Scienti

  7. Quantum mechanics

    CERN Document Server

    Mandl, Franz

    1992-01-01

    The Manchester Physics Series General Editors: D. J. Sandiford; F. Mandl; A. C. Phillips Department of Physics and Astronomy, University of Manchester Properties of Matter B. H. Flowers and E. Mendoza Optics Second Edition F. G. Smith and J. H. Thomson Statistical Physics Second Edition F. Mandl Electromagnetism Second Edition I. S. Grant and W. R. Phillips Statistics R. J. Barlow Solid State Physics Second Edition J. R. Hook and H. E. Hall Quantum Mechanics F. Mandl Particle Physics Second Edition B. R. Martin and G. Shaw The Physics of Stars Second Edition A. C. Phillips Computing for Scient

  8. Electromagnetism

    CERN Document Server

    Grant, Ian S

    1990-01-01

    The Manchester Physics Series General Editors: D. J. Sandiford; F. Mandl; A. C. Phillips Department of Physics and Astronomy, University of Manchester Properties of Matter B. H. Flowers and E. Mendoza Optics Second Edition F. G. Smith and J. H. Thomson Statistical Physics Second Edition F. Mandl Electromagnetism Second Edition I. S. Grant and W. R. Phillips Statistics R. J. Barlow Solid State Physics Second Edition J. R. Hook and H. E. Hall Quantum Mechanics F. Mandl Particle Physics Second Edition B. R. Martin and G. Shaw the Physics of Stars Second Edition A. C. Phillips Computing for Scient

  9. VizieR Online Data Catalog: Photometry and spectroscopy of KELT-11 (Pepper+, 2017)

    Science.gov (United States)

    Pepper, J.; Rodriguez, J. E.; Collins, K. A.; Johnson, J. A.; Fulton, B. J.; Howard, A. W.; Beatty, T. G.; Stassun, K. G.; Isaacson, H.; Colon, K. D.; Lund, M. B.; Kuhn, R. B.; Siverd, R. J.; Gaudi, B. S.; Tan, T. G.; Curtis, I.; Stockdale, C.; Mawet, D.; Bottom, M.; James, D.; Zhou, G.; Bayliss, D.; Cargile, P.; Bieryla, A.; Penev, K.; Latham, D. W.; Labadie-Bartz, J.; Kielkopf, J.; Eastman, J. D.; Oberst, T. E.; Jensen, E. L. N.; Nelson, P.; Sliski, D. H.; Wittenmyer, R. A.; McCrady, N.; Wright, J. T.; Relles, H. M.; Stevens, D. J.; Joner, M. D.; Hintz, E.

    2017-08-01

    KELT-11b is located in the Kilodegree Extremely Little Telescope (KELT)-South field 23, which is centered at J2000 α=10h43m48s, δ=-20°00'00''. This field was monitored from UT 2010 March 12 to UT 2014 July 9, resulting in 3910 images after post-processing and removal of bad images. We obtained follow-up time-series photometry of KELT-11b. We obtained nine full or partial transits in multiple bands between 2015 January and 2016 February. We observed an ingress of KELT-11b from the Westminster College Observatory (WCO), PA, on UT 2015 January 1 in the I filter. The observations employed a 0.35m f/11 Celestron C14 Schmidt-Cassegrain telescope and SBIG STL-6303E CCD with a 3k*2k array of 9μm pixels, yielding a 24'*16' field of view and 1.4''/pixel image scale at 3*3 pixel binning. We observed a partial transit of KELT-11b using an 0.6m RCOS telescope at the Moore Observatory (MORC), operated by the University of Louisville. The telescope has an Apogee U16M 4K*4K CCD, giving a 26'*26' field of view and 0.39''/pixel. We observed the transit on UT 2015 February 08 in alternating Sloan g and i filters from before the ingress and past the mid-transit. We observed a transit of KELT-11b in the Sloan i-band using one of the Miniature Exoplanet Radial Velocity Array (MINERVA) Project telescopes (Swift et al. 2015JATIS...1b7002S) on the night of UT 2015 February 08. MINERVA used four 0.7m PlaneWave CDK-700 telescopes that are located on Mt. Hopkins, Arizona, at the Fred L. Whipple Observatory. While the four telescopes are normally used to feed a single spectrograph to discover and characterize exoplanets through radial velocity measurements, for the KELT-11 observations, we used a single MINERVA telescope in its photometric imaging mode. That telescope had an Andor iKON-L 2048*2048 camera, which gave a field of view of 20.9'*20.9' and a plate scale of 0.6''/pixel. The camera has a 2048*2048 back-illuminated deep depletion sensor with fringe suppression. Due to the

  10. VizieR Online Data Catalog: Follow-up photometry and spectroscopy of KELT-17 (Zhou+, 2016)

    Science.gov (United States)

    Zhou, G.; Rodriguez, J. E.; Collins, K. A.; Beatty, T.; Oberst, T.; Heintz, T. M.; Stassun, K. G.; Latham, D. W.; Kuhn, R. B.; Bieryla, A.; Lund, M. B.; Labadie-Bartz, J.; Siverd, R. J.; Stevens, D. J.; Gaudi, B. S.; Pepper, J.; Buchhave, L. A.; Eastman, J.; Colon, K.; Cargile, P.; James, D.; Gregorio, J.; Reed, P. A.; Jensen, E. L. N.; Cohen, D. H.; McLeod, K. K.; Tan, T. G.; Zambelli, R.; Bayliss, D.; Bento, J.; Esquerdo, G. A.; Berlind, P.; Calkins, M. L.; Blancato, K.; Manner, M.; Samulski, C.; Stockdale, C.; Nelson, P.; Stephens, D.; Curtis, I.; Kielkopf, J.; Fulton, B. J.; Depoy, D. L.; Marshall, J. L.; Pogge, R.; Gould, A.; Trueblood, M.; Trueblood, P.

    2017-05-01

    0.58''/pixel scale and a 20'*20' field of view. One full transit of KELT-17b was observed from the Westminster College Observatory (WCO), PA, on UT 2015 November 4 in the z' filter. The observations employed a 0.35m f/11 Celestron C14 Schmidt-Cassegrain telescope and SBIG STL-6303E CCD with a ~3K*2K array of 9μm pixels, yielding a 24'*16' field of view and 1.4''/pixel image scale at 3*3 pixel binning. The stellar FWHM was seeing-limited with a typical value of ~3.2''. Three full transits of KELT-17b were observed on UT 2016 February 26 (g' and i') and UT 2016 March 31 (r') using the Manner-Vanderbilt Ritchie-Chrtien (MVRC) telescope located at the Mt. Lemmon summit of Steward Observatory, AZ. The observations employed a 0.6m f/8 RC Optical Systems Ritchie-Chretien telescope and SBIG STX-16803 CCD with a 4K*4K array of 9μm pixels, yielding a 26'*26' field of view and 0.39''/pixel image scale. The telescope was heavily defocused for all three observations resulting in a typical stellar FWHM of ~17''. The Perth Exoplanet Survey Telescope (PEST) observatory is a backyard observatory owned and operated by ThiamGuan (TG) Tan, located in Perth, Australia. It is equipped with a 0.3m Meade LX200 SCT f/10 telescope with focal reducer yielding f/5 and an SBIG ST-8XME CCD camera. The telescope and camera combine to have a 31'*21' field of view and a 1.2'' pixel scale. PEST observed KELT-17b on UT 2016 March 06 in the B band. A series of spectroscopic follow-up observations were performed to characterize the KELT-17 system. We performed low-resolution, high-signal-to-noise reconnaissance spectroscopic follow-up of KELT-17 using the Wide Field Spectrograph (WiFeS) on the Australian National University (ANU) 2.3m telescope at Siding Spring Observatory, Australia in 2015 February. In-depth spectroscopic characterization of KELT-17 was performed by the Tillinghast Reflector Echelle Spectrograph (TRES) on the 1.5m telescope at the Fred Lawrence Whipple Observatory, Mount Hopkins

  11. Comparison of various methods for mathematical analysis of the Foucault knife edge test pattern to determine optical imperfections

    Science.gov (United States)

    Gatewood, B. E.

    1971-01-01

    The linearized integral equation for the Foucault test of a solid mirror was solved by various methods: power series, Fourier series, collocation, iteration, and inversion integral. The case of the Cassegrain mirror was solved by a particular power series method, collocation, and inversion integral. The inversion integral method appears to be the best overall method for both the solid and Cassegrain mirrors. Certain particular types of power series and Fourier series are satisfactory for the Cassegrain mirror. Numerical integration of the nonlinear equation for selected surface imperfections showed that results start to deviate from those given by the linearized equation at a surface deviation of about 3 percent of the wavelength of light. Several possible procedures for calibrating and scaling the input data for the integral equation are described.

  12. Impact of technology scaling in SOI back-channel total dose tolerance. A 2-D numerical study using a self-consistent oxide code; Effet du facteur d'echelle sur la tolerance en dose de rayonnement dans le cas du courant de fuite arriere des transistors MOS/SOI. Une etude d'un oxyde utilise un code auto coherent en deux dimensions

    Energy Technology Data Exchange (ETDEWEB)

    Leray, J.L.; Paillet, Ph.; Ferlet-Cavrois, V. [CEA Bruyeres le Chatel DRIF, 91 (France); Tavernier, C.; Belhaddad, K. [ISE Integrated System Engineering AG (Switzerland); Penzin, O. [ISE Integrated System Engineering Inc., San Jose (United States)

    1999-07-01

    A new 2-D and 3-D self-consistent code has been developed and is applied to understanding the charge trapping in SOI buried oxide causing back-channel MOS leakage in SOI transistors. Clear indications on scaling trends are obtained with respect to supply voltage and oxide thickness. (authors)

  13. New developments of high dust-SCR technology in the cement industry results of pilot tests in Solnhofen and development state of a full scale SCR unit; Nouveaux developpements de la technologie SCR ''High Dust'' dans l'industrie du ciment - resultats de tests pilotes a Solnhoffen et etat de developpement d'une unite pilote a l'echelle

    Energy Technology Data Exchange (ETDEWEB)

    Samant, G. [Lurgi Energie und Entsorgung GmbH, Frankfurt (Germany); Sauter, G. [Soinhofer Portland Zementwerke AG, Solnhofen (Germany); Haug, N. [Agence Federale de l' Environnement, Berlin (Germany)

    2001-07-01

    The production of clinker in the cement industry involve the formation of nitrous oxides, and the emission limits are becoming more stringent from year to year. The added up total NOx emissions from the European cement industry amounts at present approx. 450.000 Mg/year. As such it is high time for the decision to develop and implement a technology to reduce NOx-emissions. At present SCR technology which is implemented in the glass industry, waste incineration and power plants seems to be the best economical and ecological solution for cement industry. In the period time from 1997 to the end of 1999 pilot plant test work was carried out by the companies 'Solnhofer Portland Zementwerke AG' and 'mg Engineering Lurgi' in the cement plant in Solnhofen. The results of pilot plan test work show that NOx reduction rates above 90% with NH{sub 3} slip less then 5 vppm can be achieved. The results of the test work with different type of catalysts are discussed. Based on the results of the test work a suitable SCR-process for cement industry is developed. At present a High-Dust-SCR demonstration plant at 'Solnhofer Portland Zementwerke AG' with the help of German Federal Environmental Agency, UBA-Berlin, is under commissioning and going on stream. (authors)

  14. Study of air pollution in urban and peri-urban area during the Escompte campaign using meso-scale modeling. Impact of dynamics and emission inventories; Etude de la pollution en zone urbaine et peri-urbaine a l'aide d'une modelisation meso-echelle durant la campagne Escompte. Impact de la dynamique et des inventaires d'emission

    Energy Technology Data Exchange (ETDEWEB)

    Taghavi, S.M.

    2003-11-01

    This work involves the study of the redistribution of photochemical species over urban and peri-urban areas during the ESCOMTE campaign over southern France. This region includes Marseilles, an urban area close to the industrial zone of Fos-Berre, one of the most polluted sites in Europe. The comprehensive R AMS model, version 4.3, coupled on-line with a chemical module including 29 species (MOCA2.2) is used in parallel code. The efficiency of coupling is checked using Amdahl's law (1967). The percentage of parallelization is 96% for the RAMS model and increases to 98% for RAMS-Chimie. A number of sensitivity tests were performed to obtain realistic meteorological fields. In this work, the heterogeneity of the ground humidity depends on the surface texture, and the topography option accurately retrieves the location of mountaintops and valleys. To avoid bias in the chemical results, the meteorological simulation is first validated with surface data, Lidar, Sodar, soundings and airborne measurements for three IOPs (Intensive Observation Periods) which ave contrasting meteorological conditions. Secondly, the redistribution of chemical modeled species (CO, NO{sub x}, SO{sub 2}, O{sub 3}) is validated with surface, aircraft and Lidar data over this region where the circulation is complex (sea breeze associated with northern (Mistral) or southern flow). Use of two way nested grids resolves the problem of lateral boundaries for chemical fields (Taghavi et al, 2004). The location of convective cells and the channelling of Rhone and Durance depend on direction of synoptic flow and play a role in the redistribution of pollutants and their chemical regime. Two emission inventories of varying quality (30% difference in average) are compared (Taghavi et al, 2004), one with a high resolution (I km) and the other with an average resolution. In both cases, ozone plume location and concentration are the same, and thus we conclude a low resolution inventory is satisfactory to investigate ozone plume formation because it is a nonlinear process. This type of modelling can be used to develop appropriate strategies for emissions reductions. (author)

  15. LAMMR: A new generation satellite microwave radiometer - Its concepts and capabilities. [Large Antenna Multichannel Microwave Radiometer

    Science.gov (United States)

    Walton, W. T.; Wilheit, T. T.

    1981-01-01

    Definition studies and baseline design are summarized for the proposed, and now discontinued, LAMMR. The instrument is an offset parabolic reflector with Cassegrain feeds. The three-meter aperture reflector, to be constructed using graphite-epoxy technology, rotates continuously at 0.833 rps. The scan drive subsystem includes momentum compensation for the rotating mass which includes the reflector, the support arm and Cassegrain subreflector, feed horns and radiometer. Two total power radiometers are recommended for each frequency, one each for horizontal and vertical polarizations. The selection plan, definition study specifications, LAMMR performance specifications, and predicted accuracies and resolutions after processing are shown.

  16. VizieR Online Data Catalog: 10 nearby solar-type dwarfs RV curves (Gorynya+, 2014)

    Science.gov (United States)

    Gorynya, N. A.; Tokovinin, A.

    2017-05-01

    The observations were conducted in 2012 and 2013 at the 1-m telescope of the Crimean Astrophysical Observatory sited in Simeiz, Crimea. Radial velocities were measured by the CORAVEL-type echelle spectrometer, the Radial Velocity Meter. (2 data files).

  17. An Evaluation of a High-Resolution Operational Wave Forecasting System in the Adriatic Sea

    Science.gov (United States)

    2009-01-01

    1226 Office of Counsel,Code 1008.3 ADOR/Director NCST E. R. Franchi , 7000 Public Affairs (Unclassified/ Unlimited Only), Code 703o 4 VO-oV 4/2...examine and evaluate wind-wave modeling capability (Cavaleri et al., 1989). Many institutions run global and regional atmospheric and wave models...limited-area model (LAM) built on the basis of the global model IFS/ARPEGE (ARPEGE - Action de Recherche Petite Echelle Grande Echelle, 1FS - Integrated

  18. The Disk Mass project; science case for a new PMAS IFU module

    NARCIS (Netherlands)

    Verheijen, M. A. W.; Bershady, M. A.; Andersen, D. R.; Swaters, R. A.; Westfall, K.; Kelz, A.; Roth, M. M.

    2004-01-01

    We present our Disk Mass project as the main science case for building a new fiber IFU-module for the PMAS spectrograph, currently mounted at the Cassegrain focus of the 3.5m telescope on Calar Alto. Compared to traditional long-slit observations, the large light collecting power of 2-dimensional

  19. X-shooter: UV-to-IR intermediate-resolution high-efficiency spectrograph for the ESO VLT

    NARCIS (Netherlands)

    D'Odorico, S.; Andersen, M.I.; Conconi, P.; De Caprio, V.; Delabre, B.; Di Marcantonio, P.; Dekker, H.; Downing, M.D.; Finger, G.; Groot, P.; Hanenburg, H.H.; Hammer, F.; Horville, D.; Hjorth, J.; Kaper, L.; Klougart, J.; Kjaergaard-Rasmussen, P.; Lizon, J.-L.; Marteaud, M.; Mazzoleni, R.; Michaelsen, N.; Pallavicini, R.; Rigal, F.; Santin, P.; Norup Soerensen, A.; Spano, P.; Venema, L.; Vola, P.; Zerbi, F.M.; Hasinger, G.; Turner, M.J.L.

    2004-01-01

    X-shooter is a single target spectrograph for the Cassegrain focus of one of the VLT UTs. It covers in a single exposure the spectral range from the UV to the H band with a possible extension into part of the K band. It is designed to maximize the sensitivity in this spectral range through the

  20. X-shooter, the new wide band intermediate resolution spectrograph at the ESO Very Large Telescope

    NARCIS (Netherlands)

    Vernet, J.; Dekker, H.; D'Odorico, S.; Kaper, L.; Kjaergaard, P.; Hammer, F.; Randich, S.; Zerbi, F.; Groot, P.J.; Hjorth, J.; Guinouard, I.; Navarro, R.; Adolfse, T.; Albers, P.W.; Amans, J.-P.; Andersen, J.J.; Andersen, M.I.; Binetruy, P.; Bristow, P.; Castillo, R.; Chemla, F.; Christensen, L.; Conconi, P.; Conzelmann, R.; Dam, J.; De Caprio, V.; de Ugarte Postigo, A.; Delabre, B.; Di Marcantonio, P.; Downing, M.; Elswijk, E.; Finger, G.; Fischer, G.; Flores, H.; François, P.; Goldoni, P.; Guglielmi, L.; Haigron, R.; Hanenburg, H.; Hendriks, I.; Horrobin, M.; Horville, D.; Jessen, N.C.; Kerber, F.; Kern, L.; Kiekebusch, M.; Kleszcz, P.; Klougart, J.; Kragt, J.; Larsen, H.H.; Lizon, J.-L.; Lucuix, C.; Mainieri, V.; Manuputy, R.; Martayan, C.; Mason, E.; Mazzoleni, R.; Michaelsen, N.; Modigliani, A.; Moehler, S.; Møller, P.; Norup Sørensen, A.; Nørregaard, P.; Péroux, C.; Patat, F.; Pena, E.; Pragt, J.; Reinero, C.; Rigal, F.; Riva, M.; Roelfsema, R.; Royer, F.; Sacco, G.; Santin, P.; Schoenmaker, T.; Spano, P.; Sweers, E.; ter Horst, R.; Tintori, M.; Tromp, N.; van Dael, P.; van Vliet, H.; Venema, L.; Vidali, M.; Vinther, J.; Vola, P.; Winters, R.; Wistisen, D.; Wulterkens, G.; Zacchei, A.

    2011-01-01

    X-shooter is the first 2nd generation instrument of the ESO Very Large Telescope (VLT). It is a very efficient, single-target, intermediate-resolution spectrograph that was installed at the Cassegrain focus of UT2 in 2009. The instrument covers, in a single exposure, the spectral range from 300 to

  1. X-shooter, the new wide band intermediate resolution spectrograph at the ESO Very Large Telescope

    DEFF Research Database (Denmark)

    Vernet, J.; Dekker, H.; D'Odorico, S.

    2011-01-01

    X-shooter is the first 2nd generation instrument of the ESO Very Large Telescope (VLT). It is a very efficient, single-target, intermediate-resolution spectrograph that was installed at the Cassegrain focus of UT2 in 2009. The instrument covers, in a single exposure, the spectral range from 300 t...

  2. Multiaperture spectroscopy with rapid mask fabrication and installation

    International Nuclear Information System (INIS)

    Fort, B.; Mellier, Y.; Picat, J.P.; Lelievre, G.; Rio, Y.

    1986-03-01

    A multiaperture spectroscopy device has been installed on the focal reducer at the Cassegrain focus of the Canada-France-Hawaii Telescope. The mask processing and positioning operations are described. Emphasis is placed on the speed and reliability of a fully automatic method controlled by a computer routine. Spectra obtained during the first observations at C.F.H.T. are shown as illustration

  3. Double Star Measurements at the Internationale Amateur Sternwarte (IAS) in Namibia in 2008 and 2009

    Science.gov (United States)

    Anton, Rainer

    2010-04-01

    A 40-cm-Cassegrain telescope in Namibia was used for observing double and multiple systems in the southern sky. Digital images were recorded with a CCD camera at high frame rates via a firewire interface directly in a computer. Measurements of 34 double and multiple systems are presented and compared with literature data. Some noteworthy objects are discussed in more detail.

  4. Double Star Measurements at the Internationale Amateur Sternwarte (IAS) in Namibia in 2009

    Science.gov (United States)

    Anton, Rainer

    2012-01-01

    This paper is a continuation of earlier work published in JDSO in 2010. Using a 40-cm-Cassegrain telescope in Namibia and a fast CCD camera, 87 double and multiple systems were recorded and analyzed with the technique of "lucky imaging". Measurements are compared with literature data. Some noteworthy systems are discussed in more detail.

  5. The ICE spectrograph for PEPSI at the LBT: preliminary optical design

    Science.gov (United States)

    Pallavicini, Roberto; Zerbi, Filippo M.; Spano, Paolo; Conconi, Paolo; Mazzoleni, Ruben; Molinari, Emilio; Strassmeier, Klaus G.

    2003-03-01

    We present a preliminary design study for a high-resolution echelle spectrograph (ICE) to be used with the spectropolarimeter PEPSI under development at the LBT. In order to meet the scientific requirements and take full advantage of the peculiarities of the LBT (i.e. the binocular nature and the adaptive optics capabilities), we have designed a fiber-fed bench mounted instrument for both high resolution (R ≍ 100,000; non-AO polarimetric and integral light modes) and ultra-high resolution (R ≍ 300,000; AO integral light mode). In both cases, 4 spectra per order (two for each primary mirror) shall be accomodated in a 2-dimensional cross dispersed echelle format. In order to obtain a resolution-slit product of ≍ 100,000 as required by the science case, we have considered two alternative designs, one with two R4 echelles in series and the other with a sigle R4 echelle and fiber slicing. A white-pupil design, VPH cross-dispersers and two cameras of different focal length for the AO and non-AO modes are adopted in both cases. It is concluded that the single-echelle fiber-slicer solution has to be preferred in terms of performances, complexity and cost. It can be implemented at the LBT in two phases, with the long-camera AO mode added in a second phase depending on the availability of funds and the time-scale for implementation of the AO system.

  6. VizieR Online Data Catalog: Line list for red giants in open clusters (Reddy+, 2015)

    Science.gov (United States)

    Reddy, A. B. S.; Giridhar, S.; Lambert, D. L.

    2017-11-01

    Observations were carried out during observing runs in 2011 May and November, 2012 November and 2013 March using the Robert G. Tull echelle spectrograph (Tull et al. 1995PASP..107..251T) at the coude focus of the 2.7m Harlan J. Smith telescope located at the McDonald Observatory. On all occasions we employed a 2048x2048 24μm pixel, backside-illuminated, anti-reflection coated CCD as a detector and the 52.67 grooves/mm echelle grating with exposures centred at 5060Å. (2 data files).

  7. An Amateur's Guide to Observing and Imaging the Heavens

    Science.gov (United States)

    Morison, Ian

    2014-06-01

    Foreword; Acknowledgments; Prologue: a tale of two scopes; 1. Telescope and observing fundamentals; 2. Refractors; 3. Binoculars and spotting scopes; 4. The Newtonian telescope and its derivatives; 5. The Cassegrain telescope and its derivatives - Schmidt-Cassegrains and Maksutovs; 6. Telescope maintenance, collimation and star testing; 7. Telescope accessories: finders, eyepieces and bino-viewers; 8. Telescope mounts: alt/az and equatorial with their computerised variants; 9. The art of visual observing; 10. Visual observations of the Moon and planets; 11. Imaging the Moon and planets with DSLRs and web-cams; 12. Observing and imaging the Sun in white light and H-alpha; 13. Observing with an astro-video camera to 'see' faint objects; 14. Deep sky imaging with standard and H-alpha modified DSLR cameras; 15. Deep sky imaging with cooled CCD cameras; 16. Auto-guiding techniques and equipment; 17. Spectral studies of the Sun, stars and galaxies; 18. Improving and enhancing images in Photoshop; Index.

  8. Airport Solar Photovoltaic Concentrator Project. Phase 1 - final report, June 1, 1978-February 28, 1979

    Energy Technology Data Exchange (ETDEWEB)

    1979-12-01

    The system design, analysis, and specification, site preparation, and operation and evaluation plan for a 500 kWe photovoltaic power supply to be located at the Phoenix Sky Harbor International Airport in Phoenix, Arizona, are presented. The solar cell arrays are concentrator silicon solar cells with tracking 70X Cassegrain-type concentrators. The power conditioning system, tracking system, and control systems are described in detal. Environmental impact studies are described. Component specifications and drawings are included. (WHK)

  9. Design of a solar-pumped frequency-doubled 532 nm Nd:YVO4 laser

    Science.gov (United States)

    Kittiboonanan, P.; Putchana, W.; Deeudomand, M.; Ratanavis, A.

    2017-09-01

    During the last year we have made progresson a development of a frequency-doubled 532 nm Nd:YVO4 laser pumped by solar light. The research aimed to demonstrate solar pumped lasers consisting of the optically contracted Nd:YVO4 crystal and KTP crystal with a system of laser mirrors deposited onto crystal sides. The Cassegrain reflector is used as the configuration. This solar pumped laser system is appealing for a variety applications including laser communication, imaging and defense applications.

  10. VizieR Online Data Catalog: RV and [Fe/H] in 5 open clusters (Carrera+, 2015)

    Science.gov (United States)

    Carrera, R.; Casamiquela, L.; Ospina, N.; Balaguer-Nunez, L.; Jordi, C.; Monteagudo, L.

    2015-05-01

    Medium-resolution spectra in the region of the near-infrared CaII triplet (CaT) at ~8500Å were obtained using the Intermediate Dispersion Spectrograph (IDS) mounted at the Cassegrain focus of the 2.5m Isaac Newton Telescope (INT) located at Roque de los Muchachos Observatory, Spain. Berkeley 23 was observed in service mode on 2013 January 17 and 18, and the other clusters were observed on 2014 July 18 and 19. (1 data file).

  11. Alignment and focusing tolerance influences on optical performance

    International Nuclear Information System (INIS)

    Cross, E.W.

    1982-01-01

    Alignment errors among components of an optical system may substantially degrade the image quality. Focus errors also affect system performance. The potential for serious degradation of image quality is substantial and requires that the tolerances for these errors receive significant attention early in system design. The image quality and reconnaissance performance of an all-reflecting Cassegrain is compared to an all-refractive optical system under conditions of zero and anticipated real world misalignments

  12. VLT/UVES abundances in four nearby dwarf spheroidal galaxies. II. Implications for understanding galaxy evolution

    NARCIS (Netherlands)

    Tolstoy, E; Venn, KA; Shetrone, M; Primas, F; Hill, [No Value; Kaufer, A; Szeifert, T

    We have used the Ultraviolet Visual-Echelle Spectrograph (UVES) on Kueyen (UT2) of the Very Large Telescope to take spectra of 15 individual red giant stars in the centers of four nearby dwarf spheroidal galaxies (dSph's) : Sculptor, Fornax, Carina, and Leo I. We measure the abundance variations of

  13. Smith-Purcell radiation from a 50 MeV beam

    Energy Technology Data Exchange (ETDEWEB)

    Brownell, J.H.; Walsh, J. [Dartmouth Coll., Hanover, NH (United States). Dept. of Physics and Astronomy; Kirk, H.G.; Fernow, R.C. [Brookhaven National Lab., Upton, NY (United States). Dept. of Physics; Robertson, S.H. [Univ. of Colorado, Boulder, CO (United States). Dept. of Astrophysics and Geophysics

    1996-10-01

    A 50 MeV electron beam and a 1 mm period, 5{degree} blaze, echelle grating have been used to produce radiation in the mid-infrared spectral region. The emission is highly collimated and forward-directed. The intensity level in the few ps pulse (2 nJ/sr) indicates a degree of coherent enhancement.

  14. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    The optical design and performance of the recently commissioned fiber fed echelle spectrometer of 2.34 meter Vainu Bappu Telescope are described. The use of it for stellar spectroscopic studies is discussed. Author Affiliations. N. Kameswara Rao1 S. Sriram1 K. Jayakumar1 F. Gabriel1. Indian Institute of Astrophysics, ...

  15. Laser solid sampling for a solid-state-detector ICP emission spectrometer

    International Nuclear Information System (INIS)

    Noelte, J.; Moenke-Blankenburg, L.; Schumann, T.

    1994-01-01

    Solid sampling with laser vaporization has been coupled to an ICP emission spectrometer with an Echelle optical system and a solid-state-detector for the analysis of steel and soil samples. Pulsation of the vaporized material flow was compensated by real-time background correction and internal standardization, resulting in good accuracy and precision. (orig.)

  16. On the design of the PEPSI spectropolarimeter for the LBT

    Science.gov (United States)

    Ilyin, I.; Strassmeier, K. G.; Woche, M.; Dionies, F.; Di Varano, I.

    2011-10-01

    We present the design concept of the spectropolarimeter for the high-resolution echelle spectrograph PEPSI to be installed at the 2×8.4 m Large Binocular Telescope (LBT) in Arizona. We discuss the optical key elements, the principles of operations of the instrument and its instrumental polarization effects.

  17. Measurements of plasma temperature and electron density in laser

    Indian Academy of Sciences (India)

    The temperature and electron density characterizing the plasma are measured by time-resolved spectroscopy of neutral atom and ion line emissions in the time window of 300–2000 ns. An echelle spectrograph coupled with a gated intensified charge coupled detector is used to record the plasma emissions.

  18. Spectroscopy of laser-produced plasmas

    Indian Academy of Sciences (India)

    It is a well-known fact that laser-induced breakdown spectroscopy (LIBS) has emerged as one of the best analytical techniques for multi-elemental compositional analysis of samples. We report assembling and optimization of LIBS set up using high resolution and broad-range echelle spectrograph coupled to an intensified ...

  19. Development of Multiple-Element Flame Emission Spectrometer Using CCD Detection

    Science.gov (United States)

    Seney, Caryn S.; Sinclair, Karen V.; Bright, Robin M.; Momoh, Paul O.; Bozeman, Amelia D.

    2005-01-01

    The full wavelength coverage of charge coupled device (CCD) detector when coupled with an echelle spectrography, the system allows for simultaneously multiple element spectroscopy to be performed. The multiple-element flame spectrometer was built and characterized through the analysis of environmentally significant elements such as Ca, K, Na, Cu,…

  20. The chemical composition of two supergiants in the dwarf irregular galaxy WLM

    NARCIS (Netherlands)

    Venn, K. A.; Tolstoy, E.; Kaufer, A.; Skillman, E. D.; Clarkson, S. M.; Smartt, S. J.; Lennon, D. J.; Kudritzki, R. P.

    The chemical composition of two stars in WLM has been determined from high-quality Ultraviolet-Visual Echelle Spectrograph (UVES) data obtained at the VLT-UT2. The model atmospheres analysis shows that they have the same metallicity, [Fe/H] = - 0.38 +/- 0.20 (+/- 0.29). Reliable magnesium abundances

  1. First stellar abundances in the dwarf irregular galaxy Sextans A

    NARCIS (Netherlands)

    Kaufer, A; Venn, KA; Tolstoy, E; Pinte, C; Kudritzki, RP

    We present the abundance analyses of three isolated A-type supergiant stars in the dwarf irregular galaxy Sextans A (= DDO 75) from high-resolution spectra obtained with the Ultraviolet-Visual Echelle Spectrograph (UVES) on the Kueyen telescope (UT2) of the ESO Very Large Telescope (VLT). Detailed

  2. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    Home; Journals; Journal of Astrophysics and Astronomy. N. Kameswara Rao. Articles written in Journal of Astrophysics and Astronomy. Volume 26 Issue 2-3 June-September 2005 pp 331-338. High Resolution Stellar Spectroscopy with VBT Echelle Spectrometer · N. Kameswara Rao S. Sriram K. Jayakumar F. Gabriel.

  3. Solar-like oscillations in the G9.5 subgiant β Aquilae

    DEFF Research Database (Denmark)

    Corsaro, E.; Grundahl, F.; Leccia, S.

    2012-01-01

    was observed during six nights in August 2009 by means of the high-resolution \\'echelle spectrograph SARG operating with the TNG 3.58 m Italian telescope on the Canary Islands, exploiting the iodine cell technique. We present the result and the detailed analysis of high-precision radial velocity measurements...

  4. High-speed knots in the hourglass shaped planetary nebula Hubble 12

    DEFF Research Database (Denmark)

    Vaytet, N. M. H.; Rushton, A. P.; Lloyd, M.

    2009-01-01

    We present a detailed kinematical analysis of the young compact hourglass-shaped planetary nebula Hb 12. We performed optical imaging and longslit spectroscopy of Hb 12 using the Manchester echelle spectrometer with the 2.1m San Pedro Martir telescope. We reveal, for the first time, the presence...

  5. The SONG prototype: Efficiency of a robotic telescope

    DEFF Research Database (Denmark)

    Andersen, M. F.; Grundahl, F.; Beck, A. H.

    2016-01-01

    The Stellar Observations Network Group prototype telescope at the Teide Observatory has been operating in scientific mode since March 2014. The first year of observations has entirely been carried out using the high resolution echelle spectrograph. Several asteroseismic targets were selected for ...

  6. Optical and ultraviolet study of five stars in the Pleiades open cluster

    International Nuclear Information System (INIS)

    Younan, K.F.; Dufton, P.L.

    1984-01-01

    Optical and ultraviolet observations of five low-reddened stars in the Pleiades open cluster have been obtained with an echelle spectrograph and the IUE satellite. The observed interstellar absorption lines have been analysed with different cloud models to estimate interstellar gas abundances for each line-of-sight. These results have been discussed in the light of current models for diatomic formation. (author)

  7. Fisheries and Limnological Studies on West Point Reservoir, Alabama-Georgia. Phase IV.

    Science.gov (United States)

    1984-05-01

    This is seemingly due to the irregular fishing effort and catch during the winter as dictated by the vagaries of the weather. To substantially increase...Agri. Exp. Stat. Bull. 477. 21 pp. Echelle, A. A., and J. B. Mense . 1968. Forage value of Mississippi silverside in Lake Texoma. Proc. Okla. Acad. Sci

  8. Smith-Purcell radiation from a 50 MeV beam

    International Nuclear Information System (INIS)

    Brownell, J.H.; Walsh, J.; Kirk, H.G.; Fernow, R.C.; Robertson, S.H.

    1996-10-01

    A 50 MeV electron beam and a 1 mm period, 5 degree blaze, echelle grating have been used to produce radiation in the mid-infrared spectral region. The emission is highly collimated and forward-directed. The intensity level in the few ps pulse (2 nJ/sr) indicates a degree of coherent enhancement

  9. Mechanical conceptual design of 6.5 meter telescope: Telescopio San Pedro Mártir (TSPM)

    Science.gov (United States)

    Uribe, Jorge; Bringas, Vicente; Reyes, Noe; Tovar, Carlos; López, Aldo; Caballero, Xóchitl; Martínez, César; Toledo, Gengis; Lee, William; Carramiñana, Alberto; González, Jesús; Richer, Michael; Sánchez, Beatriz; Lucero, Diana; Manuel, Rogelio; Rubio, Saúl; González, Germán.; Hernández, Obed; Segura, José; Macias, Eduardo; García, Mary; Lazaro, José; Rosales, Fabián.; del Llano, Luis

    2016-07-01

    Telescopio San Pedro Mártir (TSPM) project intends to build a 6.5 meters telescope with alt-azimuth design, currently at the conceptual design. The project is an association between Instituto de Astronomía de la Universidad Nacional Autónoma de México (IA-UNAM) and the Instituto Nacional de Astrofísica, Óptica Electrónica (INAOE) in partnership with department of Astronomy and Steward Observatory of University of Arizona and Smithsonian Astrophysical Observatory of Harvard University. Conceptual design of the telescope is lead and developed by the Centro de Ingeniería y Desarrollo Industrial (CIDESI). An overview of the feasibility study and the structural conceptual design are summarized in this paper. The telescope concept is based on telescopes already commissioned such as MMT and the Baade and Clay Magellan telescopes, building up on these proven concepts. The main differences relative to the Magellan pair are; the elevation axis is located 1 meter above the primary mirror vertex, allowing for a similar field of view at the Cassegrain and both Nasmyth focal stations; instead of using a vane ends to position the secondary mirror TSPM considers an Steward platform like MMT; finally TSPM has a larger floor distance to m1 cell than Magellans and MMT. Initially TSPM will operate with an f/5 Cassegrain station, but the design considers further Nasmyth configurations from a Cassegrain f/5 up to a Gregorian f/11. The telescope design includes 7 focal stations: 1 Cassegrain; 2 Nasmyth; and 4 folded-Cassegrain. The telescope will be designed and manufactured in Mexico, will be design in Queretaro by CIDESI and built between Queretaro and Michoacán manufacturing facilities; it will be preassembled in these facilities and disassembled to send it to the San Pedro Mártir Observatory for final integration. The azimuth and altitude structure is planned to be constructed in modules and transported by truck and shipped to Ensenada and finally to the OAN where is going

  10. Developpement D'un Modele Climatique Regional: Fizr Simulation des Conditions de Janvier de la Cote Ouest Nord Americaine

    Science.gov (United States)

    Goyette, Stephane

    1995-11-01

    Le sujet de cette these concerne la modelisation numerique du climat regional. L'objectif principal de l'exercice est de developper un modele climatique regional ayant les capacites de simuler des phenomenes de meso-echelle spatiale. Notre domaine d'etude se situe sur la Cote Ouest nord americaine. Ce dernier a retenu notre attention a cause de la complexite du relief et de son controle sur le climat. Les raisons qui motivent cette etude sont multiples: d'une part, nous ne pouvons pas augmenter, en pratique, la faible resolution spatiale des modeles de la circulation generale de l'atmosphere (MCG) sans augmenter a outrance les couts d'integration et, d'autre part, la gestion de l'environnement exige de plus en plus de donnees climatiques regionales determinees avec une meilleure resolution spatiale. Jusqu'alors, les MCG constituaient les modeles les plus estimes pour leurs aptitudes a simuler le climat ainsi que les changements climatiques mondiaux. Toutefois, les phenomenes climatiques de fine echelle echappent encore aux MCG a cause de leur faible resolution spatiale. De plus, les repercussions socio-economiques des modifications possibles des climats sont etroitement liees a des phenomenes imperceptibles par les MCG actuels. Afin de circonvenir certains problemes inherents a la resolution, une approche pratique vise a prendre un domaine spatial limite d'un MCG et a y imbriquer un autre modele numerique possedant, lui, un maillage de haute resolution spatiale. Ce processus d'imbrication implique alors une nouvelle simulation numerique. Cette "retro-simulation" est guidee dans le domaine restreint a partir de pieces d'informations fournies par le MCG et forcee par des mecanismes pris en charge uniquement par le modele imbrique. Ainsi, afin de raffiner la precision spatiale des previsions climatiques de grande echelle, nous developpons ici un modele numerique appele FIZR, permettant d'obtenir de l'information climatique regionale valide a la fine echelle spatiale

  11. Iodine-131 production by a dry method using reactor-irradiated elementary tellurium. Part 1 - Conditions for obtaining iodine emanation and its capture. Part 2 - comparative study of preparation conditions using Pyrex, stainless steel and alumina equipment. Part 3 - production on a semi-industrial scale; Production de l'iode 131 par voie seche a partir de tellure elementaire irradie a la pile. 1ere partie - Etudes des conditions pour obtenir l'emanation de l'iode et le capter. 2eme partie - Etude comparee des conditions pour effectuer cette preparation avec des appareils en Pyrex, en acier inoxydable et en alumine. 3eme partie - production a l'echelle semi-industrielle

    Energy Technology Data Exchange (ETDEWEB)

    Bardy, A; Beydon, J; Murthy, T S; Doyen, J B; Lefrancois, J [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1967-04-15

    A previous report has described how iodine 131 can be prepared from elementary tellurium by a dry method which consists in treating irradiated tellurium at 400 degrees in argon. The possibility of carrying out this treatment in a stainless steel or alumina apparatus has been considered. The behavior of gaseous iodine 131 towards these materials has thus been studied. If the adsorption of iodine on stainless steel is superficial desorption is rapid at 250 degrees in oxygen or 400 degrees in argon. If the adsorption is chemical in nature it becomes necessary to heat to higher temperatures. Adsorption of iodine on alumina is very weak and the iodine can be desorbed rapidly. With these materials tests have been carried out on 300 gms of tellurium containing 41 curies of iodine 131; the yields were very satisfactory ( 98 per cent). (author) [French] La methode de preparation de l iode 131 par voie seche a partir de tellure elementaire decrite dans un precedent rapport consiste a traiter le tellure irradie a 400 degres sous argon. Nous avons examine la possibilite d effectuer ce traitement dans un appareil en acier inoxidable ou en alumine. Le comportement de l iode 131 gazeux vis a vis de ces materiaux a donc ete etudie. Si l adsorption de l iode sur l acier inoxidable est superficielle la desorption est rapide a 250 degres sous oxygene ou 400 degres sous argon. Si la fixation est de nature chimique il est necessaire de chauffer a des temperatures plus elevees. L adsorption de l iode sur l alumine est res faible et l iode peut etre desorbe rapideemnt. En employant ces materiaux des essais ont ete obtenus sur 300 g de tellure contenant 41 curies d iode 131 avec un bon rendement (98 pour cent). (auteur00.

  12. Study of the hydrolysis of protactinium (V), at tracer scale, by solvent extraction method with thenoyl-tri-fluoro-acetone (TTA) as chelating agent. Characterization of the partition of TTA in the system TTA / H{sub 2}O / toluene / Na{sup +} / H{sup +} / ClO{sub 4}{sup -}; Contribution a l'etude thermodynamique de l'hydrolyse de Pa(V) a l'echelle des traces par la technique d'extraction liquide-liquide avec la thenoyltrifluoroacetone (TTA). Caracterisation du partage de la thenoyltrifluoroacetone dans le systeme TTA / H{sub 2}O / toluene / Na{sup +} / H{sup +} / ClO{sub 4}{sup -}

    Energy Technology Data Exchange (ETDEWEB)

    Jaussaud, Ch

    2003-01-01

    Hydrolysis of protactinium (V) according to the reactions: PaO(OH){sup 2+} +H{sub 2}O {r_reversible} PaO(OH){sub 2}{sup +} + H{sup +} (K{sub 2}] PaO(OH){sup 2+} +2H{sub 2}O {r_reversible} PaO(OH){sub 5} + H{sup +} (K{sub 3}) has been studied, at tracer scale, by solvent extraction method, with thenoyl-tri-fluoro-acetone (TTA) as chelating agent. A previous study concerning the partition of TTA between two immiscible phases (corresponding to TTA/toluene/Na{sup +}/H{sup +}/ClO{sub 4}{sup -} system) has allowed a complete characterization of this system (partition constants, standard thermodynamic values, TTA hydration degree in toluene). Owing to specific properties of protactinium (V) (sorption onto various materials, formation of colloids), an extremely rigorous protocol has been established, protocol which could be used for other hydrolysable elements. Hydrolysis constants were deduced from a systematic study of partition of Pa(V) as a function TTA and proton concentration, ionic strength and temperature. Extrapolations to zero ionic strength were performed using SIT model and the specific interaction coefficients {epsilon}{sub (i,j)} as well as the Pitzer parameters {beta}{sup (0)} and {beta}{sup (1)} were determined. Standard thermodynamic data relative to hydrolysis equilibriums of Pa(V) were also estimated. (author)

  13. Short-Lived Isotopes Used as Tracers in Industry (with Special Reference to Swedish Industry); Emploi de Radioindicateurs de Courte Periode a l'Echelle Industrielie dans les Usines Suedoises; ПРИМЕНЕНИЕ КОРОТКОЖИВУЩИХ ИЗОТОПОВ В ПРОМЫШЛЕННОСТИ В КАЧЕСТВЕ МЕЧЕНЫХ АТОМОВ; Isotopos de Periodo Corto Utilizados Como Indicadores en la Industria Sueca

    Energy Technology Data Exchange (ETDEWEB)

    Erwall, L. G.; Forsberg, H. G.; Ljunggren, K. [Isotoptekniska Laboratoriet, Stockholm (Sweden)

    1963-03-15

    Radioactive tracer methods are rapidly being recognized as a valuable means in industrial research and control. They have already been used with great advantage in trouble shooting, in investigations of the characteristics of process units and as an aid in designing such units. This review comprises typical examples of applications of short-lived tracers, which can be produced in medium neutron fluxes, for example, Na{sup 24}, Cl{sup 38}, K{sup 42}, Mn{sup 56}, Br{sup 8}'2, La{sup 140} and Au{sup 198}; studies of the transport of solids through process units - rotary kilns, blast furnaces, cellulose digesters, bleaching towers, dorr- thickeners ; determination of flow rates for liquids in tubes and open streams, to measure, for example, the total water consumption in a plant; determination of residence times, hold-back and blocked volume for liquids indifferent process units, for example in the pulp and paper industry; ''weighing'' by means of isotope dilution techniques for determination of the amount of slag in open-hearth furnaces, etc. ; determination of the origin of non- metallic inclusions in steel to find better lining materials and to optimize pouring techniques; labelling for quality identification - experimental steel baths and specific material in the iron and steel industry are being identified with absolute certainty; determination of the efficiency of mixers in the concrete industry; mapping of flow in receivers for sewage or waste water to find the best point for the outlet of such liquids; and detection and localization of leaks. To minimize the contamination of the final products, the availability of short-lived tracers has been essential in many of these studies. Most cases are of the physical tracing type, with a variety of possible tracers. Thus a tracer can be chosen which has a suitable halt-lite and radiation characteristics. If the radioactive nuclide used has a large neutron activation cross-section, which is the case for the above-mentioned nuclides, a research reactor has sufficient neutron flux for the production of quantities of even curies of the tracers, providing that high specific activity is not a requisite. In Sweden a joint industrial institute, the Isotope Techniques Laboratory, was formed in 1960 to make research and development work and to assist the industrial enterprises with advice, personnel and instruments necessary in industrial radioisotope application. (author) [French] Les methodes reposant sur l'emploi de radioindicateurc jouent, dans les travaux de recherche et les operations de controle industriels, un role dont on reconnait de plus en plus l'utilite. On les emploie avantageusement pour depister les defauts et avaries, pour analyser les caracteristiques des installations de traitement et pour l'etude de ces installations. Les auteurs donnent des exemples typiques d'applications de radioisotopes de courte periode qui peuvent etre produits par des flux de neutrons de moyenne intensite, par exemple: {sup 24}Na, {sup 56}Mn, {sup 82}Br, {sup 140}La, {sup 38}Cl, {sup 42}K et {sup 198}Au. On trouvera ci-apres quelques exemples de ces etudes: Etudes sur le mouvement des solides dans des installations de traitement - fours rotatifs, hauts fourneaux, digesteurs a cellulose, tours de blanchiment, epaississeurs Dorr; determination du debit de liquides dans des canalisations et a decouvert, par exemple, pour mesurer la quantite totale d'eau consommee par une plante ; determination des temps de sejour, de la retention et du volume bloque de liquides a divers stades de la fabrication du papier et de la pate a papier, par exemple; 'pesage' par les methodes de dilution isotopique, en vue de determiner la quantite de scories dans les fours a sole; determination de l'origine des inclusions non metalliques dans l'acier, en vue de l'obtention de meilleurs materiaux de revetement et du perfectionnement des methodes de coulee; marquage aux firs de controle de la qualite, procede permettant d'identifier avec une certitude absolue des bains d'acier d'experimentation et certains autres produits de l'industrie siderurgique determination de l'efficacite des melangeurs dans l'industrie du beton; etude de l'ecoulement dans les fosses receptrices d'eaux usees en vue de decouvrir le meilleur point d'evacuation; detection et localisation des fuites. Dans beaucoup de ces etudes, l'utilisation d'indicateuts de courte periode a ete indispensable pour reduire au minimum la contamination du produit final. Dans la plupart des cas, il s'agit d'un marquage purement physique a l'aide de divers indicateurs possibles. On peut ainsi choisir un indicateur ayant une periode appropriee et les caracteristiques de rayonnement voulues. Si le radionucleide utilise presente une grande section efficace pour l'activation par les neutrons - ce qui est le cas des nucleides enumeres plus haut - un reacteur de recherche aura un flux de neutrons suffisant pour produire des activites de l'ordre de plusieurs curies, a moins que l'on ait besoin d'une forte activite specifique. En Suede, un institut industriel mixte, le Laboratoire des methodes isotopiques, a ete cree en 1960 et charge de faire des travaux de recherche et de mise au point, et d'aider les entreprises industrielles en leur donnant lea conseils, le personnel et les appareils dont elles ont besoin pour appliquer les methodes utilisant les radioisotopes. (author) [Spanish] Rapidamente se va reconociendo que los metodos basados en el empleo de indicadores radiactivos son muy valiosos en la investigacion y el control industriales. Se han utilizado ya con gian exito para localizar defectos, estudiar las caracteristicas de instalaciones industriales y como ayuda para disenar dichas instalaciones. La presente memoria cita ejemplos tipicos de las aplicaciones de los indicadores de periodo corto que se pueden obtener con flujos neutronicos medios, por ejemplo, {sup 24}Na, {sup 38}Cl, {sup 42}K, {sup 56}Mn, {sup 82}Br, {sup 140}La y {sup 198}Au: Estudio del transporte de solidos en instalaciones industriales (hornos giratorios, altos hornos, digestores para celulosa, torres de blanqueo, espesadores Dorr); determinacion del caudal de liquidos en tuberias y canales abiertos, por ejemplo, para medir el consumo total de agua en una fabrica; determinacion de tiempos de permanencia y de volumenes bloqueados para liquidos en diversas instalaciones, por ejemplo, en las industrias de la pulpa y del papel; 'determinacion de pesos' por medio de tecnicas de dilucion isotopica, por ejemplo, para evaluar la cantidad de escoria presente en hornos de hogar abierto; determinacion del origen de inclusiones no metalicas en el acero, para perfeccionar revestimientos y hallar las tecnicas optimas de colada; marcacion para identificar la calidad (en las industrias del hierro y del acero se estan identiticando con certeza absoluta bafios experimentales y materiales especificos); determinacion del rendimiento de mezcladoras en la industria delhoimigon; determinacion de las corrientes en tanques receptores de aguas servidas con miras a encontrar el lugar optimo para la boca de salida del liquido; y deteccion y localizacion de fugas. Los indicadores de periodo corto han sido esenciales en muchos de estos estudios para reducir a un minimo la contaminacion del producto final. En la mayoria de los casos, la marcacion es fisica, pudiendo elegirse el indicador de forma que su periodo de semidesintegracion y las caracteristicas de las radiaciones que emiten sean adecuados. Si el nuclido radiactivo que se emplea tiene una elevada seccion eficaz de activacion neutronica, como es el caso de los nuclidos mencionados, el flujo neutronico de un reactor de investigacion basta para obtener indicadores de algunos curies de actividad, siempre que no sea imprescindible una actividad especifica elevada. En 1960 se creo en Suecia un instituto industrial central, el Laboratorio de Tecnicas Isotopicas, cuya mision es llevar a cabo trabajos de investigacion y desarrollo y prestar asistencia a las empresas industriales proporcionandoles asesoiamiento, personal y los instrumentos necesarios para las aplicaciones industriales de los radioisotopos. (author) [Russian] Metody radioaktivnyh mechenyh atomov bystro nahodjat svoe priznanie kak neocenimoe sredstvo dlja issledovanij i kontrolja v promyshlennosti. Oni uhe uspeshno primenjalis' v avarijnyh sluchajah, pri issle- dovanii harakteristik proizvodstvennyh uzlov i kak vspomogatel'noe sredstvo pri konstruirovanii takih proizvodstvennyh uzlov. Dannyj obzor soderzhit tipichnye primery primenenija korotkozhivushhih mechenyh atomov, kotorye mogut byt' polucheny v umerennyh nejtronnyh potokah, naprimer,natrija-24, magnija-56, broma-62, lantana-140, a takzhe hlora-38, kalija-42 i zolota-196. S pomoshh'ju korotkozhivushhih izotopov mozhno proizvodit': - izuchenie prohozhdenija tverdyh veshhestv cherez proizvodstvennye uzly (vrashhavshiesja sushil'nye pechi, domennye pechi, celljuloznye avtoklavy, bashni dlja otbelki, sgustiteli Dorra) ; - opredelenie skorosti potoka zhidkostej v trubah i v otkrytyh ruslah (naprimer, dlja izmerenija obshego kolichestva potreblenija vody na ustanovke); - opredelenie vremeni nahozhdenija zaderzhki i ob{sup e}ma zhidkostej v razlichnyh tehnologicheskih uzlah v celljuloznoj i bumazhnoj promyshlennosti - ''vzveshivanie'' po metodu izotopnogo razbavlenija dlja opredelenija kolichestva shlakov v martenovskih pechah; - opredelenie proishozhdenija nemetallicheskih primesej v stali dlja izyskanija luchshih materialov dlja oblicovki i dlja usovershenstvovanija metodov otlivki; - mechenie dlja opredelenija kachestva, pozvoljajushhee ustanovit' s absoljutnoj dostovernost'ju jeksperimental'nye stal'nye plavki i specificheskie materialy v chernoj metallurgii; - opredelenie jeffektivnosti mesilok v betonnoj promyshlennosti; - sostavlenie diagramm potoka v bassejnah dlja stochnyh vod ili zhidkih othodov v celjah nahozhdenija nailuchshego mesta dlja spuska takih zhidkostej; - obnaruzhenie utechek. Chtoby svesti k minimumu zagrjaznenija okonchatel'nyh produktov pri provedenii mnogih iz jetih issledovanij, bylo sushhestvenno vazhno ispol'zovat' korotkozhivushhie mechenye atomy. V bol'shinstve sluchaev primenjalis' metody fizicheskogo mechenija s vozmozhnost'ju vybora samyh raznoobraznyh mechenyh atomov. Tem samym predstavljaetsja vozmozhnym vybirat' mechenye atomy s podhodjashhim poluperiodom raspada i s nuzhnymi harakteristikami izluchenija. Esli ispol'zuemyj radioizotop obladaet bol'shim secheniem aktivacii nejtronov, chto prisushhe perechislennym vyshe izotopam, to issledovatel'skij reaktor mozhet dat' dostatochnyj potok nejtronov dlja proizvodstva aktivnostej indikatorov porjadka do neskol'kih kjuri pri uslovii, chto ne trebuetsja dlja nih znachitel'noj udel'noj aktivnosti. V Shvecii v 1960 godu byl obrazovan ob{sup e}dinennyj promyshlennyj institut i laboratorija izotopnyh metodov dlja provedenija issledovanij i rabot po razvitiju, a takzhe dlja okazanija pomoshhi promyshlennym predprijatijam posredstvom predostavlenija konsul'tacij, personala i neobhodimyh priborov po promyshlennomu primeneniju radioizotopov. (author)

  14. Discovery Channel Telescope active optics system early integration and test

    Science.gov (United States)

    Venetiou, Alexander J.; Bida, Thomas A.

    2012-09-01

    The Discovery Channel Telescope (DCT) is a 4.3-meter telescope with a thin meniscus primary mirror (M1) and a honeycomb secondary mirror (M2). The optical design is an f/6.1 Ritchey-Chrétien (RC) with an unvignetted 0.5° Field of View (FoV) at the Cassegrain focus. We describe the design, implementation and performance of the DCT active optics system (AOS). The DCT AOS maintains collimation and controls the figure of the mirror to provide seeing-limited images across the focal plane. To minimize observing overhead, rapid settling times are achieved using a combination of feed-forward and low-bandwidth feedback control using a wavefront sensing system. In 2011, we mounted a Shack-Hartmann wavefront sensor at the prime focus of M1, the Prime Focus Test Assembly (PFTA), to test the AOS with the wavefront sensor, and the feedback loop. The incoming wavefront is decomposed using Zernike polynomials, and the mirror figure is corrected with a set of bending modes. Components of the system that we tested and tuned included the Zernike to Bending Mode transformations. We also started open-loop feed-forward coefficients determination. In early 2012, the PFTA was replaced by M2, and the wavefront sensor moved to its normal location on the Cassegrain instrument assembly. We present early open loop wavefront test results with the full optical system and instrument cube, along with refinements to the overall control loop operating at RC Cassegrain focus.

  15. Visible and infrared mapping spectrometer (VIMS) - a facility instrument for planetary missions

    International Nuclear Information System (INIS)

    Wellman, J.B.; Duval, J.; Juergens, D.; Voss, J.

    1988-01-01

    A second-generation visible and IR mapping spectrometer (VIMS), selected for both the Mars Observer and Comet Rendezvous Asteroid Flyby (CRAF) missions, is described. VIMS is a scanning spectrometer with a focal plane consisting of linear arrays of visible and IR detectors, cooled by a radiative cooler. It is noted that a wide-angle scan using a full-aperture scan mirror was implemented for the Mars Observer; a narrow-angle scan using a scanning secondary mirror within a Cassegrain foreoptic was achieved for the CRAF mission. 11 references

  16. Requirements and concept design for large earth survey telescope for SEOS

    Science.gov (United States)

    Mailhot, P.; Bisbee, J.

    1975-01-01

    The efforts of a one year program of Requirements Analysis and Conceptual Design for the Large Earth Survey Telescope for the Synchronous Earth Observatory Satellite is summarized. A 1.4 meter aperture Cassegrain telescope with 0.6 deg field of view is shown to do an excellent job in satisfying the observational requirements for a wide range of earth resources and meteorological applications. The telescope provides imagery or thermal mapping in ten spectral bands at one time in a field sharing grouping of linear detector arrays. Pushbroom scanning is accomplished by spacecraft slew.

  17. The Polatron: A Millimeter-Wave Cosmic Microwave Background Polarimeter for the OVRO 5.5 m Telescope

    OpenAIRE

    Philhour, B. J.; Keating, B. G.; Ade, P. A. R.; Bhatia, R. S.; Bock, J. J.; Church, S. E.; Glenn, J.; Hinderks, J. R.; Hristov, V. V.; Jones, W. C.; Kamionkowski, M.; Kumar, D. E.; Lange, A. E.; Leong, J. R.; Marrone, D. P.

    2001-01-01

    We describe the development of a bolometric receiver designed to measure the arcminute-scale polarization of the cosmic microwave background (CMB). The Polatron will be mounted at the Cassegrain focus of the 5.5 m telescope at the Owens Valley Radio Observatory (OVRO). The receiver will measure both the Q and U Stokes parameters over a 20% pass-band centered near 100 GHz, with the input polarization signal modulated at ~0.6 Hz by a rotating, birefringent, quartz half-wave plate. In six months...

  18. Cámara CCD Directa con el Telescopio de 2.15 m del CASLEO: algunos diagnósticos

    Science.gov (United States)

    Cellone, S. A.

    Se efectuaron algunas pruebas con la cámara CCD (+ Reductor Focal) instalada en el foco Cassegrain del Telescopio de 2.15 m del Complejo Astronómico El Leoncito (CASLEO). Las conclusiones más significativas son: Los tiempos de exposición efectivos difieren de los nominales en una fracción apreciable de segundo. En exposiciones de menos de 3 segundos, la iluminación no es pareja en todo el detector. En consecuencia, se recomiendan los pasos a seguir por los astrónomos tanto durante la observación como en la reducción de sus datos.

  19. VizieR Online Data Catalog: V346 Cen multiwavelength light curves (Mayer+, 2016)

    Science.gov (United States)

    Mayer, P.; Harmanec, P.; Wolf, M.; Nemravova, J.; Prsa, A.; Fremat, Y.; Zejda, M.; Liska, J.; Jurysek, J.; Honkova, K.; Masek, M.

    2016-06-01

    We present photographic light curves from O'Connell (1939, Publications of the Riverview College Observatory, 2, 5), uvby light curves from Gimenez et al. (1986A&AS...66...45G), BVR light curves from 0.6 m reflector with a CCD camera, Mt. John, New Zealand, green light curve from Sonnar 4/135mm telephoto lens with a CCD ATIK16IC camera, Sutherland, South Africa and BVRI light curves from 0.3m Meade Schmidt-Cassegrain reflector with a CCD camera. (5 data files).

  20. Student Observations of Double Star Delta Orionis (STFA 14 AC)

    Science.gov (United States)

    Estrada, Reed; Aguilera, Sophia; Bowden, Sam; Gillette, Travis; Givens, Jalynn; Reder, Gabriel; Rhoades, Breauna; Sharpe, Scott; Shattles, Jenna; Cha, Brendon; Do, Vicky; Ewing, Malachi; Kiamco, Alex Junior; Nelms, Brenda; Peña, Emilie; Maricarmen, Richard; Thielen, Austin

    2018-01-01

    A group of eight eighth graders and eight high schoolers studied the double star STFA 14 AC. They used the procedure from Argyle's book to get the separation and position angle for the double star. The students used a Celestron C8 Schmidt-Cassegrain telescope with a Baader Planetarium microguide eyepiece with similar markings to a Celestron Eyepiece. The students determined the separation to be 56 arcseconds and the position angle to be 4.19°. They compared their results to the Washington Double Star Catalog and found that they had a 2.88 arcseconds difference in separation and a 2.19° in position angle.

  1. Morphology of bipolar planetary nebulae. I. Two-dimensional spectrophotometry

    International Nuclear Information System (INIS)

    Pascoli, G.

    1990-01-01

    Two-dimensional spectrophotometric observations of bipolar planetary nebulae were performed by using a CCD detector mounted at the Cassegrain focus of either 1.54 m Danish Telescope or 2.2 m German Telescope at La Silla (ESO) in Chile. Emission lines have been selected with the help of narrow band-pass interference filters (Δλ∼ 10 - 20 A). Isophotal maps in various lines Hα, [NII] λ 6584, [OIII] λ 5007 and [SII] λλ 6717-6731 are presented. Particular attention has been given to scrutinize the symmetries inside a few bipolar planetary nebulae, in order to subsequently investigate their space structure

  2. New BV light curves of the eclipsing binary 44i Bootis

    International Nuclear Information System (INIS)

    Rovithis, P.; Rovithis-Livaniou, H.

    1990-01-01

    The eclipsing binary 44i Bootis, the fainter component of the visual binary ADS 9494, has been observed during 1980 as well as during 1988. The observations were made with the 48-inch Cassegrain reflector at the Kryonerion Station of the National Observatory of Athens, Greece. The individual observations of 44i Bootis are presented for years 1980 and 1988 and are also discussed. A linear as well as a quadratic least square fitting to the O-C diagram of 44i Boo for the last decade is given in which it is shown that the period of the system continues to increase

  3. Speckle Interferometry with the OCA Kuhn 22" Telescope

    Science.gov (United States)

    Wasson, Rick

    2018-04-01

    Speckle interferometry measurements of double stars were made in 2015 and 2016, using the Kuhn 22-inch classical Cassegrain telescope of the Orange County Astronomers, a Point Grey Blackfly CMOS camera, and three interference filters. 272 observations are reported for 177 systems, with separations ranging from 0.29" to 2.9". Data reduction was by means of the REDUC and Speckle Tool Box programs. Equipment, observing procedures, calibration, data reduction, and analysis are described, and unusual results for 11 stars are discussed in detail.

  4. Design of an imaging microscope for soft X-ray applications

    Science.gov (United States)

    Hoover, Richard B.; Shealy, David L.; Gabardi, David R.; Walker, Arthur B. C., Jr.; Lindblom, Joakim F.

    1988-01-01

    An imaging soft X-ray microscope with a spatial resolution of 0.1 micron and normal incidence multilayer optics is discussed. The microscope has a Schwarzschild configuration, which consists of two concentric spherical mirrors with radii of curvature which minimize third-order spherical aberration, coma, and astigmatism. The performance of the Stanford/MSFC Cassegrain X-ray telescope and its relevance to the present microscope are addressed. A ray tracing analysis of the optical system indicates that diffraction-limited performance can be expected for an object height of 0.2 mm.

  5. A unique airborne observation. [Martian atmospheric temperature and abundances from occultation of Epsilon Geminorum

    Science.gov (United States)

    Elliot, J. L.; Dunham, E.; Church, C.

    1976-01-01

    The occultation of 3rd magnitude Epsilon Geminorum by Mars was observed using a 36-inch telescope equipped with a photoelectric photometer at the bent Cassegrain focus, carried aboard the Kuiper Airborne Observatory at altitudes up to 45,000 feet. Scintillation from the earth's atmosphere was greatly reduced in comparison with ground observations. The observations clearly show the central flash, caused by the symmetrical refraction of light by the atmosphere of Mars. The data are being analyzed to obtain temperature profiles and to assess the relative abundance of argon and carbon dioxide in the atmosphere of the planet.

  6. Quasi-optical techniques for ECRH

    International Nuclear Information System (INIS)

    Andenaerde, K.; Beyer, J.; Vernon, R.

    1985-01-01

    The status of research at Wisconsin on quasi-optical launchers for ECRH is presented. Wengenroth's mode transducing antenna has been investigated theoretically. Agreement with experiment using TE 01 excitation is excellent, and the theory has been expanded to include TE 02 and TE 03 excitation as well. A system incorporating such and similar mode transducing antennas with a Cassegrain system will combine the output of various gyrotrons. A device to test this and similar concepts is being built and has been preliminarily tested for mode purity

  7. A compact led lidar system fitted for a mars rover - design and ground experiment

    Science.gov (United States)

    Ong, Prane Mariel B.; Shiina, Tatsuo; Manago, Naohiro; Kuze, Hiroaki; Senshu, Hiroki; Otobe, Naohito; Hashimoto, George; Kawabata, Yasuhiro

    2018-04-01

    A compact LED lidar was constructed and fieldtested with the aim to observe the Mars' dust devils. To be able to fit it on the Mars rover, a specialized Cassegrain telescope was designed to be within a 10 cm-cube, with a field of view of 3mrad. The transmitter has 385 nm LED light source with 3 cmϕ opening, 70mrad divergence, 0.75W (7.5nJ/10ns) pulse power, and 500 kHz repetition frequency. The configuration of the optical system is biaxial to easily configure the overlap between their optical axes.

  8. Digitalized Mirror Array and Its Application in Large Telescope: Principle and Case Studies

    International Nuclear Information System (INIS)

    Chen Yingtian; Zhang Yang; Lim, Boon Ham; Lim, Chen Sin; Hu Sen; Ho, Tso-Hsiu; Chong, Kok Keong; Tan, Boon Kok

    2009-01-01

    In this article, we report the principle and conceptual design of a fundamentally different technology in fabricating high precision aberration free optical devices. The tip-tilt of facet in a mirror array is produced by digitally controlled line-tilts of rows and columns. It has not only provided a cost-effective designing methodology in optical physics but also led to a much finer precision of 1 mili arc sec or less. As examples of the application of the proposed digitalised optics, two case studies have been given: a 10 m Schmidt telescope (off-axis) and an 8 m Cassegrain telescope (on-axis). (geophysics, astronomy, and astrophysics)

  9. A compact led lidar system fitted for a mars rover – design and ground experiment

    Directory of Open Access Journals (Sweden)

    Ong Prane Mariel B.

    2018-01-01

    Full Text Available A compact LED lidar was constructed and fieldtested with the aim to observe the Mars’ dust devils. To be able to fit it on the Mars rover, a specialized Cassegrain telescope was designed to be within a 10 cm-cube, with a field of view of 3mrad. The transmitter has 385 nm LED light source with 3 cmϕ opening, 70mrad divergence, 0.75W (7.5nJ/10ns pulse power, and 500 kHz repetition frequency. The configuration of the optical system is biaxial to easily configure the overlap between their optical axes.

  10. Soft X-ray sources and their optical counterparts in the error box of the COS-B source 2CG 135+01

    Energy Technology Data Exchange (ETDEWEB)

    Caraveo, P A; Bignami, G F [Consiglio Nazionale delle Ricerche, Milan (Italy). Lab. di Fisica Cosmica e Tecnologie Relative; Paul, J A [CEA Centre d' Etudes Nucleaires de Saclay, 91 - Gif-sur-Yvette (France). Section d' Astrophysique; Marano, B [Bologna Univ. (Italy). Ist. di Astronomia; Vettolani, G P [Consiglio Nazionale delle Ricerche, Bologna (Italy). Lab. di Radioastronomia

    1981-01-01

    We shall present here the Einstein observations for the 2CG 135+01 region where the results are complete in the sense that we have a satisfactory coverage of the COS-B error box and, more important, that all the IPC sources found have been identified, through both HRI and optical observations. In particular, the new spectral classifications of the present work were obtained at the Lojano Observatory (Bologna, Italy) with the Boller and Chivens spectrograph at the Cassegrain focus of the 1.52 in telescope. The spectral dispersion is 80 A/mm.

  11. GO Shaping of Omnidirectional Dual-Reflector Antennas with Arbitrary Main-Beam Direction in Elevation Plane by Connecting Conic Sections

    Directory of Open Access Journals (Sweden)

    Rafael A. Penchel

    2018-01-01

    Full Text Available This work discusses an alternative geometrical optics (GO technique to synthesize omnidirectional dual-reflector antennas with uniform aperture phase distribution together with an arbitrary main-beam direction for the antenna radiation pattern. Sub- and main reflectors are bodies of revolution generated by shaped curves defined by local conic sections consecutively concatenated. The shaping formulation is derived for configurations like ADC (axis-displaced Cassegrain and ADE (axis-displaced ellipse omnidirectional antennas. As case studies, two configurations fed by a TEM coaxial horn are designed and analyzed by a hybrid technique based on mode matching and method of moments in order to validate the GO shaping procedure.

  12. VizieR Online Data Catalog: K2-19b light curve (Armstrong+, 2015)

    Science.gov (United States)

    Armstrong, D. J.; Santerne, A.; Veras, D.; Barros, S. C. C.; Demangeon, O.; Lillo-Box, J.; McCormac, J.; Osborn, H. P.; Tsantaki, M.; Almenara, J.-M.; Barrado, D.; Boisse, I.; Bonomo, A. S.; Brown, D. J. A.; Bruno, G.; Rey Cerda, J.; Courcol, B.; Deleuil, M.; Diaz, R. F.; Doyle, A. P.; Hebrard, G.; Kirk, J.; Lam, K. W. F.; Pollacco, D. L.; Rajpurohit, A.; Spake, J.; Walker, S. R.

    2015-08-01

    The Near Infrared Transiting ExoplanetS (NITES) Telescope is a semi-robotic 0.4m (f/10) Meade LX200GPS Schmidt-Cassegrain telescope installed at the ORM, La Palma. One transit of K2-19b was observed on 2015 Feb 28. The telescope was defocused slightly to 3.3 FWHM and 814 images of 20s exposure time were obtained with 5s dead time between each. Observations were obtained without a filter. The table presents data taken with the NITES telescope shown in Figure 1 of the publication. (1 data file).

  13. Small-scale kinematic structures in ring nebulae around Wolf-Rayet stars

    International Nuclear Information System (INIS)

    Chu, Y.H.

    1988-01-01

    Four ring nebulas around galactic Wolf-Rayet stars have been observed with echelle spectrographs in the long-slit mode: NGC 2359, NGC 3199, NGC 6888, and RCW 58. The spatial resolution of these observations is seeing limited at about 1-3 arcsec, which is almost a two orders of magnitude improvement from the previous Fabry-Perot scanner observations. To avoid large geometric corrections, the slit positions were placed as close to the central stars as possible. The results show that the ejecta-type nebula RCW 58 is a clumpy shell expanding regularly at about 110 km/s, as opposed to the chaotic expansion concluded from the earlier Fabry-Perot observations. For the three windblown bubbles, NGC 2359, NGC 3199, and NGC 6888, the small-scale structures revealed in the echelle data can explain the apparently discrepant expansion velocities derived from the previous large-aperture Fabry-Perot observations. 20 references

  14. Observations of Superwinds in Dwarf Galaxies

    Science.gov (United States)

    Marlowe, A. T.; Heckman, T. M.; Wyse, R.; Schommer, R.

    1993-12-01

    Dwarf galaxies are important in developing our understanding of the formation and evolution of galaxies, and of the structure in the universe. The concept of supernova-driven mass outflows is a vital ingredient in theories of the structure and evolution of dwarfs galaxies. We have begun a detailed multi-waveband search for outflows in starbursting dwarf galaxies, and have obtained Fabry-Perot images and Echelle spectra of 20 nearby actively-star-forming dwarf galaxies. In about half the sample, the Fabry-Perot Hα images show loops and filaments with sizes of one to a few kpc. The Echelle spectra taken through the loops and filaments show kinematics consistent with expanding bubble-like structures. We describe these data, and present seven dwarfs in our sample that have the strongest evidence of outflows.

  15. Process analysis of recycled thermoplasts from consumer electronics by laser-induced plasma spectroscopy.

    Science.gov (United States)

    Fink, Herbert; Panne, Ulrich; Niessner, Reinhard

    2002-09-01

    An experimental setup for direct elemental analysis of recycled thermoplasts from consumer electronics by laser-induced plasma spectroscopy (LIPS, or laser-induced breakdown spectroscopy, LIBS) was realized. The combination of a echelle spectrograph, featuring a high resolution with a broad spectral coverage, with multivariate methods, such as PLS, PCR, and variable subset selection via a genetic algorithm, resulted in considerable improvements in selectivity and sensitivity for this complex matrix. With a normalization to carbon as internal standard, the limits of detection were in the ppm range. A preliminary pattern recognition study points to the possibility of polymer recognition via the line-rich echelle spectra. Several experiments at an extruder within a recycling plant demonstrated successfully the capability of LIPS for different kinds of routine on-line process analysis.

  16. VizieR Online Data Catalog: Accurate astrometry & RVs of 4 multiple systems (Tokovinin+, 2017)

    Science.gov (United States)

    Tokovinin, A.; Latham, D. W.

    2017-10-01

    The outer subsystems are classical visual binaries. Historic micrometric measurements and modern speckle interferometric data have been obtained from the WDS database on our request. Additionally, we secured new speckle astrometry and relative photometry of two systems at the 4.1m SOAR telescope. Published radial velocities (RVs) are used here together with the new data. The RVs were measured with the CfA Digital Speedometers, initially using the 1.5m Wyeth Reflector at the Oak Ridge Observatory in the town of Harvard, Massachusetts, and subsequently with the 1.5m Tillinghast Reflector at the Whipple Observatory on Mount Hopkins, Arizona. Starting in 2009, the new fiber-fed Tillinghast Reflector Echelle Spectrograph (TRES) was used. The spectral resolution was 44000 for all three spectrographs. Two objects, HIP 101955 and 103987, were observed in 2015 with the CHIRON echelle spectrograph at the 1.5m telescope at CTIO with a spectral resolution of 80000. (4 data files).

  17. VizieR Online Data Catalog: Abundance ratio for 5 local stellar associations (Reddy+, 2015)

    Science.gov (United States)

    Reddy, A. B. S.; Lambert, D. L.

    2018-01-01

    In this paper, we have performed a homogeneous and a comprehensive abundance analysis using high-resolution spectroscopy. High-resolution and high signal-to-noise (S/N) spectra of the program stars were obtained during the nights of 2015 February 10-11 with the Robert G. Tull coude cross-dispersed echelle spectrograph (Tull et al. 1995PASP..107..251T) of the 2.7 m Harlan J. Smith reflector at the McDonald Observatory. We employed a Tektronix 2048x2048 24 μm pixel, backside illuminated and anti-reflection coated CCD as a detector and an R2 echelle grating with 52.67 grooves/mm with exposures centred at 5060 Å. (7 data files).

  18. Using laser-induced breakdown spectroscopy on vacuum alloys-production process for elements concentration analysis

    Science.gov (United States)

    Zhao, Tianzhuo; Fan, Zhongwei; Lian, Fuqiang; Liu, Yang; Lin, Weiran; Mo, Zeqiang; Nie, Shuzhen; Wang, Pu; Xiao, Hong; Li, Xin; Zhong, Qixiu; Zhang, Hongbo

    2017-11-01

    Laser-induced breakdown spectroscopy (LIBS) utilizing an echelle spectrograph-ICCD system is employed for on-line analysis of elements concentration in a vacuum induction melting workshop. Active temperature stabilization of echelle spectrometer is implemented specially for industrial environment applications. The measurement precision is further improved by monitoring laser parameters, such as pulse energy, spatial and temporal profiles, in real time, and post-selecting laser pulses with specific pulse energies. Experimental results show that major components of nickel-based alloys are stable, and can be well detected. By using internal standard method, calibration curves for chromium and aluminum are obtained for quantitative determination, with determination coefficient (relative standard deviation) to be 0.9559 (< 2.2%) and 0.9723 (< 2.8%), respectively.

  19. HPF: The Habitable Zone Planet Finder at the Hobby-Eberly Telescope

    Science.gov (United States)

    Wright, Jason T.; Mahadevan, Suvrath; Hearty, Fred; Monson, Andy; Stefansson, Gudmundur; Ramsey, Larry; Ninan, Joe; Bender, Chad; Kaplan, Kyle; Roy, Arpita; Terrien, Ryan; Robertson, Paul; Halverson, Sam; Schwab, Christian; Kanodia, Shubham

    2018-01-01

    The Habitable Zone Planet Finder (HPF) is an ultra-stable NIR (ZYJ) high resolution echelle spectrograph on the 10-m Hobby-Eberly Telescope capable of 1-3 m/s Doppler velocimetry on nearby late M dwarfs (M4-M9). This precision is sufficient to detect terrestrial planets in the Habitable Zones of these relatively unexplored stars. Here we present its capabilities and early commissioning results.

  20. An Operational Implementation of a CBRN Sensor-Driven Modeling Paradigm for Stochastic Event Reconstruction

    Science.gov (United States)

    2010-05-01

    operationnelle pour la reconstruction de sources, au systeme de model- isation urbaine multi echelle integre mis en oeuvre dans !’infrastructure informatique...or urbanLS, respectively. However, for the Bayesian inversion of concentration data to be practical , fast and efficient techniques are required for...sensitivity and/or uncertainty analysis methods that have been used to quantify and reduce them. In this paper , all the various error contributions to

  1. Carbon and oxygen abundances of field RR Lyrae stars. I. Carbon abundances

    International Nuclear Information System (INIS)

    Butler, D.; Manduca, A.; Deming, D.; Bell, R.A.

    1982-01-01

    From an analysis of KPNO 4-m echelle plates and simultaneous uvbyβ photometry, we have determined carbon abundances and carbon-to-iron ratios for a large number of field RR Lyrae stars having [Fe/H]> or approx. =-1.2. It is found that these field RR Lyrae stars: stars which are known to be in an advanced evolutionary state: have carbon-to-iron ratios which are similar to those of unevolved stars

  2. Optical observations of the morphology and kinematics of the compact core of the peculiar supernova remnant CTB 80

    International Nuclear Information System (INIS)

    Whitehead, M.J.; Meaburn, J.; Clayton, C.A.

    1989-01-01

    Optical observations of the 1-arcmin core of the complex supernova remnant CTB 80 have been made with the Manchester echelle spectrometer, in both its imaging and spectral modes, on the Isaac Newton and William Herschel telescopes. Four 'shells' (A-D) are found in the light of Hα but only the central two of these (A and B) are bright at [N II]. Ionization by shocks of shells with different velocities is implied. (author)

  3. Analysis of the action of X-rays on the multiplication of a unicellular chlorophyllous organism: the chlorophycee scenesdesmus crassus chod (1961); Analyse de l'action des rayons X sur la multiplication d'un organisme chlorophyllien unicellulaire: la chlorophycee scenesdesmus crassus chod (1961)

    Energy Technology Data Exchange (ETDEWEB)

    Gilet, R; Ozenda, P [Commissariat a l' Energie Atomique, Grenoble (France). Centre d' Etudes Nucleaires

    1961-07-01

    The technique of growing cultures on agar-agar has made it possible to obtain on single cultures results which had previously been acquired on populations of unicellular algae in a liquid medium. (authors) [French] La technique de culture sur gelose a permis une analyse a l'echelle individuelle des resultats precedemment acquis sur des populations d'algues unicellulaires en milieu liquide. (auteurs)

  4. The third flight of CHESS: Preliminary analysis of interstellar H2 on the β1 Sco sightline

    Science.gov (United States)

    Kruczek, Nick; France, Kevin

    2018-01-01

    We describe the scientific motivation and technical development of the Colorado High-resolution Echelle Stellar Spectrograph (CHESS), focusing on the preliminary science results for the third launch of the payload (CHESS-3). CHESS is a far ultraviolet rocket-borne instrument designed to study the atomic-to-molecular transitions within translucent cloud regions in the interstellar medium. CHESS is an objective echelle spectrograph, which uses a mechanically-ruled echelle and a powered (f/12.4) cross-dispersing grating, and is designed to achieve a resolving power R > 100,000 over the band pass λλ 1000-1600 Å. CHESS-3 launched on 14 June 2017 aboard NASA/CU sounding rocket mission 36.323 UG. The target for the flight was β1 Sco, a B1V star with a sightline that is likely sampling translucent material. We present flight results of interstellar molecular hydrogen excitation, including initial measurements of the column density and temperature, on the sightline.

  5. A new alignment procedure for the South African Astronomical Observatory's 74-inch telescope

    Science.gov (United States)

    Crause, Lisa A.; Booth, John A.; Doss, David; Loubser, Egan; O'Connor, James E.; Sass, Craig; Sickafoose, Amanda A.; Worters, Hannah L.

    2016-07-01

    Considerable effort has gone into improving the performance and reliability of the SAAO's 74-inch telescope. This included replacing the telescope encoders, refining the pointing model and increasing the telescope throughput. The latter involved re-aluminising the primary and formulating a procedure to ensure optimal alignment of the telescope mirrors. To this end, we developed the necessary hardware and techniques to ensure that such alignment is achieved and maintained, particularly following re-aluminising of the mirrors. In essence, the procedure involves: placing a Taylor Hobson Alignment Telescope on the mechanical rotation axis of the 74-inch (which we define to be the optical axis, since the Cassegrain instruments attach to the associated turntable), then adjusting the tip/tilt of the secondary mirror to get it onto that axis and, lastly, adjusting the tip/tilt of the primary mirror to eliminate coma. An eyepiece (or wavefront camera) is installed at the Cassegrain port for this final step since comatic star images indicate the need to tip/tilt the primary mirror to align it to the secondary. Tuning out any brightness gradients seen in an out-of-focus image of a bright star may also be used for feedback when adjusting the tip/tilt of the primary mirror to null coma.

  6. An integrated thermo-structural model to design a polarimeter for the GTC

    Science.gov (United States)

    Di Varano, I.; Strassmeier, K. G.; Woche, M.; Laux, U.

    2016-07-01

    The GTC (Gran Telescopio Canarias), with an equivalent aperture of 10.4 m, effective focal length of 169.9 m, located at the Observatorio del Roque de los Muchachos , in La Palma, Canary Islands, will host on its Cassegrain focus the GRAPE polarimeter (GRAntecan PolarimEter). At such focus the plate scale is 1.21 arcsec/mm and the unvignetted FOV 8 arcmin. The instrument will provide full Stokes polarimetry in the spectral range 380-1500 nm, feeding simultaneously up to two spectrographs. At the moment an interface to HORS (High Optical Resolution Spectrograph) is being defined, located on the Nasmyth platform, it has a FWHM resolving power of about 25,000 (5 pixel) within a spectral range of 400-680 nm. The rotator and instrumental flanges for the Cassegrain focus are currently under definition. Hereafter I present the state of art of the mechanical design of the polarimeter, whose strategy is based on an integrated model of Zemax design into ANSYS FEM static and dynamic analyses with thermal loads applied, in order to retrieve tip-tilt, decentering errors and other significant parameters to be looped back to the Zemax model. In such a way it is possible to compare and refine the results achieved through the tolerance analysis.

  7. The Submillimeter Telescope (SMT) project

    International Nuclear Information System (INIS)

    Martin, R.N.; Baars, J.W.M.

    1990-01-01

    To exploit the potential of submillimeter astronomy, the Submillimeter Telescope (SMT) will be located at an altitude of 3178 meters on Emerald Peak 75 miles northeast of Tucson in Southern Arizona. The instrument is an altazimuth mounted f/13.8 Cassegrain homology telescope with two Nasmyth and bent Cassegrain foci. It will have diffraction limited performance at a wavelength of 300 microns and an operating overall figure accuracy of 15 microns rms. An important feature of the SMT is the construction of the primary and secondary reflectors out of aluminum-core CFRP face sheet sandwich panels, and the reflector backup structure and secondary support out of CFRP structural elements. This modern technology provides both a means for reaching the required precision of the SMT for both night and day operation (basically because of the low coefficient of thermal expansion and high strength-to-weight ratio of CFRP) and a potential route for the realization of lightweight telescopes of even greater accuracy in the future. The SMT will be the highest accuracy radio telescope ever built (at least a factor of 2 more accurate than existing telescopes). In addition, the SMT will be the first 10 m-class submillimeter telescope with a surface designed for efficient measurements at the important 350 microns wavelength atmospheric window. 9 refs

  8. Eclipse parcial de Luna - 23-24 de Marzo de 1997

    Science.gov (United States)

    Arquiola, A. P.; Arquiola, F. E.

    Luego de varios años en que las condiciones climáticas no nos permitían registrar el fenómeno, pudimos observar y realizar secuencias fotográficas del eclipse parcial Luna. Siendo de una magnitud de 0.92 (muy cercano a la totalidad) se obtuvo una serie de fotografías muy claras y preferentemente con gran contraste a fin de destacar las tonalidades de las sombras, en especial la penumbra, que desde ya el clima nos favoreció. Los métodos fotográficos fueron, en primer lugar, con telezoom de 210mm a f/4.5 con película color de 1600 ASA; y el ya clásico método a foco primario en el Telescopio Schmidt - Cassegrain de 200mm a f/10. Paralelamente a la observación del eclipse, estábamos al instante comunicados por correo electrónico con otros observadores desde diferentes lugares del mundo intercambiando reportes, y también usuarios en general de la red, de esta forma se hizo muy especial el fenómeno. Instrumentos utilizados : Telescopio Schmidt-Cassegrain 200mm f/10, Cámara fotográfica Minolta con Telezoom 210mm f/4.5, Película 1600 ASA color, Telescopio Refractor 80mm a f/15

  9. "First Light" for HARPS at La Silla

    Science.gov (United States)

    2003-03-01

    . PR Photo 08b/03 : The HARPS spectrograph . PR Photo 08c/03 : HARPS spectrum of the star HD100623 ("raw"). PR Photo 08d/03 : Extracted spectral tracing of the star HD100623 . PR Photo 08e/03 : Measured stability of HARPS. The HARPS Spectrograph ESO PR Photo 08a/03 ESO PR Photo 08a/03 [Preview - JPEG: 449 x 400 pix - 58k [Normal - JPEG: 897 x 800 pix - 616k] [Full-Res - JPEG: 1374 x 1226 pix - 1.3M] ESO PR Photo 08b/03 ESO PR Photo 08b/03 [Preview - JPEG: 500 x 400 pix - 83k [Normal - JPEG: 999 x 800 pix - 727k] [Full-Res - JPEG: 1600 x 1281 pix - 1.3M] Captions : PR Photo 08a/03 and PR Photo 08b/03 show the HARPS spectrograph during laboratory tests. The vacuum tank is open so that some of the high-precision components inside can be seen. On PR Photo 08a/03 , the large optical grating by which the incoming stellar light is dispersed is visible on the top of the bench; it measures 200 x 800 mm. HARPS is a unique fiber-fed "echelle" spectrograph able to record at once the visible range of a stellar spectrum (wavelengths from 380 - 690 nm) with very high spectral resolving power (better than R = 100,000 ). Any light losses inside the instrument caused by reflections of the starlight in the various optical components (mirrors and gratings), have been minimised and HARPS therefore works very efficiently . First observations ESO PR Photo 08c/03 ESO PR Photo 08c/03 [Preview - JPEG: 400 x 490 pix - 52k [Normal - JPEG: 800 x 980 pix - 362k] [Full-Res - JPEG: 1976 x 1195 pix - 354k] ESO PR Photo 08d/03 ESO PR Photo 08d/03 [Preview - JPEG: 485 x 400 pix - 53k [Normal - JPEG: 969X x 800 pix - 160k] Captions : PR Photo 08c/03 displays a HARPS untreated ("raw") exposure of the star HD100623 , of the comparatively cool stellar spectral type K0V. The frame shows the complete image as recorded with the 4000 x 4000 pixel CCD detector in the focal plane of the spectrograph. The horizontal white lines correspond to the stellar spectrum, divided into 70 adjacent spectral bands which

  10. The Multiple-component Binary Hyad, vA 351 - a Progress Report

    Science.gov (United States)

    Benedict, George Fritz; Franz, Otto G.; Wasserman, Lawrence H.

    2017-06-01

    We extend results first announced by Franz et al. (1998) in the abstract, http://adsabs.harvard.edu/abs/1998AAS...19310207F ,that identified vA 351 = H346 in the Hyades as a multiple star system containing a white dwarf. With HST/FGS fringe tracking and scanning, spanning four years, we establish a parallax, relative orbit, and mass fraction for the A-B components, with a period, P~5.47y. With ground-based radial velocities from the McDonald Observatory Struve 2.1m telescope and Sandiford Spectrograph, spanning 14 years, we find that component B consists of BC, two M dwarf stars orbiting with a very short period (P(BC)~0.75 days), having a mass ratio C/B~0.94. We confirm that the total mass of the system can only be reconciled with the distance and component photometry by including a fainter, higher mass component, proposed to be a ~0.8Msun white dwarf. Thus, the quadruple system consists of three M dwarfs (A,B,C) and one white dwarf (D). The M dwarf masses and absolute magnitudes are consistent with the Benedict et al. (2016, http://adsabs.harvard.edu/abs/2016AJ....152..141B) lower Main Sequence Mass-Luminosity Relation. The radial velocity signal has so far yielded a signature only for the short-period BC orbital motion. Velocities from H-α and He I emission lines confirm the BC period from absorption lines, with similar (He I) and higher (H-α) velocity amplitudes.

  11. C. C. Rafn, J. J. A. Worsaae, Archaeology, History and Danish National Identity in the Schleswig-Holstein Question

    Directory of Open Access Journals (Sweden)

    C. Stephen Briggs

    2005-11-01

    Full Text Available Between 1789 and 1815 Europe was devastated by a series of intermittent Wars waged by the French. The first part came about through the French Revolution, the second, the Napoleonic Wars, were about Bonaparte’s thirst for conquest. Almost at the end of them, Denmark’s attempted neutrality was to cost her the loss of Norway by cessation to Sweden under the Treaty of Kiel in 1814. The Norwegians felt particularly aggrieved by this, a ploy on the part of the British to disarm the Scandinavians and retain British Naval access to the Baltic. Thus began a half a century of particular national insecurity for Denmark, during which she felt under constant threat from German ambition through an increasingly powerful, predatory Prussia. Schleswig-Holstein was particularly at risk of annexation, because though much of Slesvig was culturally and ethnically Danish, southern Jutland had been strongly infiltrated by German influences unchecked for many decades (Sandiford 1975: 21. With a small population (2,225,000 in 1848 and now detached from those potentially sympathetic in Scandinavia, Denmark would have difficulty effectively opposing any major industrial power. Britain and Germany aside, there was also Russia, still largely undeveloped, but a power with strong Baltic interests. Maintaining Denmark’s borders through this delicately balanced neutrality was not going to be easy for such a small nation state. Would it be remotely possible to achieve this passively by developing trade? Could enduring borders otherwise be protected by influencing perceptions of Denmark’s historic cultural identity and ethnicity?

  12. Optical design of a versatile FIRST high-resolution near-IR spectrograph

    Science.gov (United States)

    Zhao, Bo; Ge, Jian

    2012-09-01

    We report the update optical design of a versatile FIRST high resolution near IR spectrograph, which is called Florida IR Silicon immersion grating spectromeTer (FIRST). This spectrograph uses cross-dispersed echelle design with white pupils and also takes advantage of the image slicing to increase the spectra resolution, while maintaining the instrument throughput. It is an extremely high dispersion R1.4 (blazed angle of 54.74°) silicon immersion grating with a 49 mm diameter pupil is used as the main disperser at 1.4μm -1.8μm to produce R=72,000 while an R4 echelle with the same pupil diameter produces R=60,000 at 0.8μm -1.35μm. Two cryogenic Volume Phase Holographic (VPH) gratings are used as cross-dispersers to allow simultaneous wavelength coverage of 0.8μm -1.8μm. The butterfly mirrors and dichroic beamsplitters make a compact folding system to record these two wavelength bands with a 2kx2k H2RG array in a single exposure. By inserting a mirror before the grating disperser (the SIG and the echelle), this spectrograph becomes a very efficient integral field 3-D imaging spectrograph with R=2,000-4,000 at 0.8μm-1.8μm by coupling a 10x10 telescope fiber bundle with the spectrograph. Details about the optical design and performance are reported.

  13. VizieR Online Data Catalog: HI-selected Lyman limit systems metallicities (Lehner+, 2016)

    Science.gov (United States)

    Lehner, N.; O'Meara, J. M.; Howk, J. C.; Prochaska, J. X.; Fumagalli, M.

    2018-04-01

    All the new data presented here are from our Keck Observatory Database of Ionized Absorption toward Quasars (KODIAQ) database as part of our new KODIAQ Z survey (Lehner+ 2014, J/ApJ/788/119 ; O'Meara+ 2015, J/AJ/150/111). In short, these data were acquired with the HIgh Resolution Echelle Spectrometer (HIRES) on the Keck I telescope on Maunakea. These data were obtained by different PIs from different institutions with Keck access, and hundreds of spectra of QSOs at 0

  14. High resolution atlas of the solar spectrum 2678-2931 A

    Science.gov (United States)

    Allen, M. S.; Mcallister, H. C.; Jefferies, J. T.

    1977-01-01

    A portion of the ultraviolet solar spectrum is presented in this high resolution atlas. The data, originating from a rocket echelle spectrogram obtained on 19 June 1974 of a quiet area near the center of the solar disk, extend from 2678 to 2931 A. The instrument had a nominal resolving power of 200,000 at these wavelengths and the rms precision of the rectified wavelength scale is 15 mA. Absolute intensities are computed by calibration to the absolute measurements of Kohl and Parkinson.

  15. THE METALLICITY OF THE PLEIADES

    International Nuclear Information System (INIS)

    Soderblom, David R.; Laskar, Tanmoy; Valenti, Jeff A.; Stauffer, John R.; Rebull, Luisa M.

    2009-01-01

    We have measured the abundances of Fe, Si, Ni, Ti, and Na in 20 Pleiades stars with T eff values near solar and with low vsin i using high-resolution, high signal-to-noise echelle spectra. We have validated our procedures by also analyzing 10 field stars of a range of temperatures and metallicities that were observed by Valenti and Fischer. Our result for the Pleiades is [Fe/H] = +0.03 ± 0.02 ± 0.05 (statistical and systematic). The average of published measurements for the Pleiades is +0.042 ± 0.021.

  16. Stellar C III Emissions as a New Classification Parameter for (WC) Central Stars

    Science.gov (United States)

    Feibelman, W. A.

    1999-01-01

    We report detection of stellar C III lambda 1909 emission in International Ultraviolet Explorer (IUE) echelle spectra of early-type [WC] planetary nebula central stars (CSPNs). Additionally, stellar C III emission at lambda 2297 is observed in early- and late-type [WC) CSPNS. Inclusion of these C III features for abundance determinations may resolve a conflict of underabundance of C/O for early type [WC2] - [WC4] CSPNS. A linear dependence on stellar C III lambda 2297 equivalent widths can be used to indicate a new classification of type [WCUV] central stars.

  17. Vector magnetic field observations with the Haleakala polarimeter

    Science.gov (United States)

    Mickey, D. L.

    1985-01-01

    Several enhancements were recently made to the Haleakala polarimeter. Linear array detectors provide simultaneous resolution over a 3-A wavelength range, with spectral resolution of 40 mA. Optical fibers are now used to carry the intensity-modulated light from the rotating quarter-wave plate polarimeter to the echelle spectrometer, permitting its removal from the spar to a more stable environment. These changes, together with improved quarter-wave plates, reduced systematic errors to a few parts in 10,000 for routine observations. Examples of Stokes profiles and derived magnetic field maps are presented.

  18. PEPSI, the High-Resolution Optical-IR Spectrograph for the LBT

    Science.gov (United States)

    Andersen, Michael; Strassmeier, Klaus; Hoffman, Axel; Woche, Manfred; Spano, Paolo

    PEPSI is a high resolution fibre feed optical-IR polarimetric echelle spectrograph for the Large Binocular Telescope (LBT). PEPSI utilizes the two 8.4m LBT apertures to simultaneously record four polarization states at a resolution of 120.000. The extension of the coverage towards the IR is mainly motivated by the larger Zeeman splitting of IR lines, which would allow to study weaker/fainter magnetic structures on stars. The two optical arms, which also have an integral light mode with R up to 300.000, are under construction, while the IR arm is being designed.

  19. Abundancias químicas de estrellas de Mercurio-Manganeso obtenidas con espectros EBASIM

    Science.gov (United States)

    Pintado, O. I.; Adelman, S. J.

    Se determinan las abundancias químicas de estrellas de HgMn usando espectros obtenidos con EBASIM en CASLEO en un rango de longitud de onda comprendido entre los 400 y 890 nm. Los valores iniciales de temperatura efectiva y gravedad superficial se calculan con la fotometría uvbyβ. Las abundancias se calculan usando WIDTH9 y SYNTHE. Los resultados se comparan análisis realizados por los autores usando espectros obtenidos con el espectrógrado REOSC del CASLEO, el espectrógrafo echelle del Telescopio Anglo-Australiano y el espectrógrafo Coudé del Dominion Astrophysical Observatory.

  20. Abundancias químicas de ψ Octantis

    Science.gov (United States)

    Medina, M. C.; Pintado, O. I.

    Se determinan las abundancias químicas de ψ Oct usando espectros obtenidos con EBASIM en CASLEO. Los valores iniciales de temperatura efectiva y gravedad superficial se calculan con la fotometría uvbyβ. Esta estrella fue estudiada por Pintado y Adelman (1996) usando espectros REOSC y Adelman y otros (1993), este último basado en espectros echelle obtenidos con el Telescopio Anglo Australiano. Comparamos nuestros resultados con los de los trabajos anteriormente mencionados, pudiéndose realizar una evaluación de la calidad de los espectros EBASIM.

  1. Observations of the radial velocity of the Sun as measured with the novel SONG spectrograph

    DEFF Research Database (Denmark)

    Pallé, P. L.; Grundahl, F.; Hage, A. Triviño

    2013-01-01

    Deployment of the prototype node of the SONG project took place in April 2012 at Observatorio del Teide (Canary Islands). Its key instrument (echelle spectrograph) was installed and operational a few weeks later while its 1 m feeding telescope suffered a considerable delay to meet the required...... specifications. Using a fibre-feed, solar light could be fed to the spectrograph and we carried out a 1-week observing campaign in June 2012 to evaluate its performance for measuring precision radial velocities. In this work we present the first results of this campaign by comparing the sensitivity of the SONG...

  2. Optical design for a breadboard high-resolution spectrometer for SIRTF/IRS

    Science.gov (United States)

    Brown, Robert J.; Houck, James R.; van Cleve, Jeffrey E.

    1996-11-01

    The optical design of a breadboard high resolution infrared spectrometer for the IRS instrument on the SIRTF mission is discussed. The spectrometer uses a crossed echelle grating configuration to cover the spectral region from 10 to 20 micrometer with a resolving power of approximately equals 600. The all reflective spectrometer forms a nearly diffraction limited image of the two dimensional spectrum on a 128 multiplied by 128 arsenic doped silicon area array with 75 micrometer pixels. The design aspects discussed include, grating numerology, image quality, packaging and alignment philosophy.

  3. High efficiency spectro graphs for the EUV and soft x-rays

    International Nuclear Information System (INIS)

    Cash, W.

    1983-01-01

    A basic need of modern UV and x-ray astronomy is the capability to perform high resolution spectroscopy of faint stars. The use of modern grazing incidence optics can be coupled to high blaze angle reflection gratings used in the conical diffraction mount to offer a versatile, efficient approach to the design problem. The authors discuss two designs of interest: an echelle spectrograph for use longward of 100 A, and an Objective Reflection Grating Spectrograph for use in the soft x-rays. General design considerations and measurements of grating efficiencies are also presented

  4. bHROS: A New High-Resolution Spectrograph Available on Gemini South

    Science.gov (United States)

    Margheim, S. J.; Gemini bHROS Team

    2005-12-01

    The Gemini bench-mounted High-Resolution Spectrograph (bHROS) is available for science programs beginning in 2006A. bHROS is the highest resolution (R=150,000) optical echelle spectrograph optimized for use on an 8-meter telescope. bHROS is fiber-fed via GMOS-S from the Gemini South focal plane and is available in both a dual-fiber Object/Sky mode and a single (larger) Object-only mode. Instrument characteristics and sample data taken during commissioning will be presented.

  5. VizieR Online Data Catalog: Vi' LCs and RVs of the EB star TYC 5227-1023-1 (Traven+, 2017)

    Science.gov (United States)

    Traven, G.; Munari, U.; Dallaporta, S.; Zwitter, T.

    2017-11-01

    CCD photometry in the Landolt V and SLOAN i' bands of TYC5227-1023-1 has been obtained with ANS Collaboration telescope N.36 located in Cembra (Trento, Italy). Spectra of TYC 5227-1023-1 were secured in 2015-2016 with the Echelle+CCD spectrograph mounted on the 1.82m telescope operated by Osservatorio Astronomico di Padova atop Mt. Ekar (Asiago). Here we recall that the 3600-7400Å wavelength region is covered in 30 orders at a resolving power of 20000. (2 data files).

  6. Exoplanets search and characterization with the SOPHIE spectrograph at OHP

    Directory of Open Access Journals (Sweden)

    Hébrard G.

    2011-02-01

    Full Text Available Several programs of exoplanets search and characterization have been started with SOPHIE at the 1.93-m telescope of Haute-Provence Observatory, France. SOPHIE is an environmentally stabilized echelle spectrograph dedicated to high-precision radial velocity measurements. The objectives of these programs include systematic searches for exoplanets around different types of stars, characterizations of planet-host stars, studies of transiting planets through RossiterMcLaughlin effect, follow-up observations of photometric surveys. The instrument SOPHIE and a review of its latest results are presented here.

  7. SALT Spectroscopy of Evolved Massive Stars

    Science.gov (United States)

    Kniazev, A. Y.; Gvaramadze, V. V.; Berdnikov, L. N.

    2017-06-01

    Long-slit spectroscopy with the Southern African Large Telescope (SALT) of central stars of mid-infrared nebulae detected with the Spitzer Space Telescope and Wide-Field Infrared Survey Explorer (WISE) led to the discovery of numerous candidate luminous blue variables (cLBVs) and other rare evolved massive stars. With the recent advent of the SALT fiber-fed high-resolution echelle spectrograph (HRS), a new perspective for the study of these interesting objects is appeared. Using the HRS we obtained spectra of a dozen newly identified massive stars. Some results on the recently identified cLBV Hen 3-729 are presented.

  8. The Metallicity of the Pleiades

    OpenAIRE

    Soderblom, David R.; Laskar, Tanmoy; Valenti, Jeff A.; Stauffer, John R.; Rebull, Luisa M.

    2009-01-01

    We have measured the abundances of Fe, Si, Ni, Ti, and Na in 20 Pleiades stars with T_(eff) values near solar and with low v sin i using high-resolution, high signal-to-noise echelle spectra. We have validated our procedures by also analyzing 10 field stars of a range of temperatures and metallicities that were observed by Valenti and Fischer. Our result for the Pleiades is [Fe/H] = +0.03 ± 0.02 ± 0.05 (statistical and systematic). The average of published measurements for the Pleiades is +0....

  9. A multi-frequency study of symbiotic stars: Pt. 1

    International Nuclear Information System (INIS)

    Ivison, R.J.; Bode, M.F.; Roberts, J.A.

    1991-01-01

    The relationship between optical line flux and 5 GHz radio flux is investigated for a sample of 17 northern sky symbiotic stars. Data were obtained near-simultaneously with the Manchester Echelle Spectrograph mounted on the Isaac Newton Telescope, La Palma and the Broad Band Interferometer at Jodrell Bank. Colour excesses, calculated from Balmer hydrogen line fluxes assuming Case B recombination ratios, are compared with other reddening estimates and also combined with extinction maps to provide improved distance estimates. Optical line fluxes are used in combination with radio fluxes to estimate physical parameters of these objects, including mass-loss rates. (author)

  10. Atlas of Vega: 3850-6860 Å

    Science.gov (United States)

    Kim, Hyun-Sook; Han, Inwoo; Valyavin, G.; Lee, Byeong-Cheol; Shimansky, V.; Galazutdinov, G. A.

    2009-10-01

    We present a high resolving power (λ/Δλ = 90,000) and high signal-to-noise ratio (˜700) spectral atlas of Vega covering the 3850-6860 Å wavelength range. The atlas is a result of averaging of spectra recorded with the aid of the echelle spectrograph BOES fed by the 1.8 m telescope at Bohyunsan Observatory (Korea). The atlas is provided only in machine-readable form (electronic data file) and will be available in the SIMBAD database upon publication. Based on data collected with the 1.8 m telescope operated at BOAO Observatory, Korea.

  11. Chemical composition of δ Scuti stars: 1. AO CVn, CP Boo, KW Aur

    Science.gov (United States)

    Galeev, A. I.; Ivanova, D. V.; Shimansky, V. V.; Bikmaev, I. F.

    2012-11-01

    We used high-resolution echelle spectra acquired with the 1.5-m Russian-Turkish Telescope to determine the fundamental atmospheric parameters and abundances of 30 chemical elements for three δ Scuti stars: AOCVn, CP Boo, and KWAur. The chemical compositions we find for these stars are similar to those for Am-star atmospheres, though some anomalies of up to 0.6-0.7 dex are observed for light and heavy elements. We consider the effect of the adopted stellar parameters (effective temperature, log g, microturbulent velocity) and the amplitude of pulsational variations on the derived elemental abundances.

  12. A very demanding spectrometer optical design for ExoMars Mission

    Science.gov (United States)

    Belenguer, T.; Fernandez-Rodriguez, M.; Colombo, M.; Diaz-Catalá, E.; Sanchez-Páramo, J.

    2017-11-01

    The objective of this report is to present the study performed for a specially demanding solution of a spectrometer [1] design based on a transmissive holographic grating especially designed to actuate as the dispersion element. The main driver of the design has been to obtain a device with a clear reduction in mass, power and mechanical envelope with respect to the previous configuration based on a prism and/or Echelle grating. This simplification is produced mainly at expense of the waveband range. This study has been carried out by Laboratorio de Instrumentación Espacial (LINES) optical designers from Instituto Nacional de Técnica Aeroespacial (INTA).

  13. The crowded magnetosphere of the post common envelope binary QS Virginis

    OpenAIRE

    Parsons, S. G.; Hill, C. A.; Marsh, T. R.; Gansicke, B. T.; Watson, C. A.; Steeghs, D.; Dhillon, V. S.; Littlefair, S. P.; Copperwheat, C. M.; Schreiber, M. R.; Zorotovic, M.

    2016-01-01

    We present high-speed photometry and high-resolution spectroscopy of the eclipsing post-common-envelope binary QS Virginis (QS Vir). Our Ultraviolet and Visual Echelle Spectrograph (UVES) spectra span multiple orbits over more than a year and reveal the presence of several large prominences passing in front of both the M star and its white dwarf companion, allowing us to triangulate their positions. Despite showing small variations on a time-scale of days, they persist for more than a year an...

  14. The Evolution of Spiral Disks

    Science.gov (United States)

    Bershady, Matthew A.; Andersen, David R.

    We report on aspects of an observational study to probe the mass assembly of large galaxy disks. In this contribution we focus on a new survey of integral-field Hα velocity-maps of nearby, face on disks. Preliminary results yield disk asymmetry amplitudes consistent with estimates based on the scatter in the local Tully-Fisher relation. We also show how the high quality of integral-field echelle spectroscopy enables determinations of kinematic inclinations to i ~20 °. This holds the promise that nearly-face-on galaxies can be included in the Tully-Fisher relation. Finally, we discuss the prospects for measuring dynamical asymmetries of distant galaxies.

  15. Absolute spectrophotometry of Wolf-Rayet stars: Are the colors the same

    International Nuclear Information System (INIS)

    Massey, P.

    1982-01-01

    For the past year the author has collecting data on all the northern hemisphere WR stars brighter than v approximately 15 with the Intensified Reticon Scanner (IRS) on the Kitt Peak No. 1 - 36'' (0.9-m) telescope. The instrument consists of the regular cassegrain spectrograph followed by a three stage image tube coupled to a 920x2 Reticon via a microchannel plate. Measurements were made with simultaneous sky subtraction, with coverage obtained from lambdalambda 3300 - 7100 A. The resolution is 3 A in the blue and 6 A in the red. Counts were converted to absolute flux by observations of standard stars tied into the Hayes and Latham (1975) calibration of Vega. (Auth.)

  16. Security scanning at 94GHz

    Science.gov (United States)

    Anderton, Rupert N.; Appleby, Roger; Beale, John E.; Coward, Peter R.; Price, Sean

    2006-05-01

    It is well known that millimetre waves can pass through clothing. In short range applications such as in the scanning of people for security purposes, operating at W band can be an advantage. The size of the equipment is decreased when compared to operation at Ka band and the equipments have similar performance. In this paper a W band mechanically scanned imager designed for imaging weapons and contraband hidden under clothing is discussed. This imager is based on a modified folded conical scan technology previously reported. In this design an additional optical element is added to give a Cassegrain configuration in image space. This increases the effective focal length and enables improved sampling of the image and provides more space for the receivers. This imager is constructed from low cost materials such as polystyrene, polythene and printed circuit board materials. The trade off between image spatial resolution and thermal sensitivity is discussed.

  17. 3.6-m Devasthal Optical Telescope Project: Completion and first results

    Science.gov (United States)

    Kumar, Brijesh; Omar, Amitesh; Maheswar, Gopinathan; Pandey, Anil Kumar; Sagar, Ram; Uddin, Wahab; Sanwal, Basant Ballabh; Bangia, Tarun; Kumar, Tripurari Satyanarayana; Yadav, Shobhit; Sahu, Sanjit; Pant, Jayshreekar; Reddy, Bheemireddy Krishna; Gupta, Alok Chandra; Chand, Hum; Pandey, Jeewan Chandra; Joshi, Mohit Kumar; Jaiswar, Mukeshkuma; Nanjappa, Nandish; Purushottam; Yadav, Rama Kant Singh; Sharma, Saurabh; Pandey, Shashi Bhushan; Joshi, Santosh; Joshi, Yogesh Chandra; Lata, Sneh; Mehdi, Biman Jyoti; Misra, Kuntal; Singh, Mahendra

    2018-04-01

    We present an update on the 3.6-m aperture optical telescope, which has been installed at Devasthal in the year 2016. In this paper, a brief overview of installation activities at site and first results are presented. The 3.6-m Devasthal Optical Telescope project was initiated in 2007 by the Aryabhatta Research Institute of Observational Sciences (ARIES; Nainital, India) in partnership with Belgium. The telescope has Ritchey-Chretien optics, an alt-azimuth mount, an active control of the primary and a corrected science field of view of 30' at the Cassegrain focus. The construction of the telescope enclosure building was completed in June 2014 and after successful installation of the telescope. The first engineering light was obtained on 22 March 2015. The on-sky performance of the telescope was carried out till February 2016.

  18. Long wavelength infrared camera (LWIRC): a 10 micron camera for the Keck Telescope

    Energy Technology Data Exchange (ETDEWEB)

    Wishnow, E.H.; Danchi, W.C.; Tuthill, P.; Wurtz, R.; Jernigan, J.G.; Arens, J.F.

    1998-05-01

    The Long Wavelength Infrared Camera (LWIRC) is a facility instrument for the Keck Observatory designed to operate at the f/25 forward Cassegrain focus of the Keck I telescope. The camera operates over the wavelength band 7-13 {micro}m using ZnSe transmissive optics. A set of filters, a circular variable filter (CVF), and a mid-infrared polarizer are available, as are three plate scales: 0.05``, 0.10``, 0.21`` per pixel. The camera focal plane array and optics are cooled using liquid helium. The system has been refurbished with a 128 x 128 pixel Si:As detector array. The electronics readout system used to clock the array is compatible with both the hardware and software of the other Keck infrared instruments NIRC and LWS. A new pre-amplifier/A-D converter has been designed and constructed which decreases greatly the system susceptibility to noise.

  19. Main-sequence turnoff of the Draco dwarf galaxy

    International Nuclear Information System (INIS)

    Stetson, P.B.; Mcclure, R.D.; Vandenberg, D.A.; Victoria Univ., Canada)

    1985-01-01

    Deep photometry on the B,V system for 182 stars in the dwarf spheroidal galaxy in Draco was obtained with a CCD camera at the Cassegrain focus of the Canada-France-Hawaii 3.6-m telescope. Draco's main-sequence turnoff if found near V(to) = 23.5, which is about 3.4 magnitudes below the galaxy's horizontal branch. This leads to the interpretation that Draco is not measurably younger than the clusters or Ursa Minor: the age of Draco is about 18 Gyr according to current star-revolution chronologies. No blue stragglers are definitely detected in Draco, and it is concluded that any young population in Draco probably represents less than 10 percent of the total. 30 references

  20. VizieR Online Data Catalog: Circumnuclear star-forming regions (Alvarez-Alvarez+, 2015)

    Science.gov (United States)

    Alvarez-Alvarez, M.; Diaz, A. I.; Terlevich, E.; Terlevich, R.

    2016-01-01

    In order to achieve our scientific goals, we have studied a diverse population of galaxies with reported circumnuclear rings of SFRs in the bibliography. The data were acquired during five observing runs. For the first two runs (from 1988 to 1990), we used a blue sensitive GEC CCD at the f/15 Cassegrain focus of the 1.0m. Jacobus Kaptein Telescope of the Isaac Newton Group at the Observatorio del Roque de los Muchachos, La Palma, Spain. The CCD had 578x385 pixels 22um wide. The last three observing runs were carried on from 1999 to 2000 at the Centro Astronomico Hispano Aleman de Calar Alto, Almeria, Spain. (3 data files).

  1. The SPEAR 3 Diagnostic Beamlines

    CERN Document Server

    Corbett, Jeff; Mok, Walter; Ringwall, Andrew

    2005-01-01

    SPEAR 3 is equipped with an x-ray pinhole camera and a visible/UV beam line to evaluate electron beam properties. The pinhole camera has a 30 x 25 micron Ta aperture and 60% image demagnification on a phosphor screen. The image is captured by a National Instruments frame-grabber on a remote computer with a parallel video signal for control room monitoring. The visible/UV beam line features a horizontal ± 0.3 mrad 'cold finger' to remove the x-ray core of the beam. The remaining visible/UV light is deflected 18 degrees onto an optical bench where it is focused via refractive Cassegrain optics. The beam is then split into parallel optics for gated- and streak camera measurements. This paper describes the experimental set up and preliminary measurements obtained with both systems.

  2. VizieR Online Data Catalog: Galactic HII region IRAS 16148-5011 content (Mallick+, 2015)

    Science.gov (United States)

    Mallick, K. K.; Ojha, D. K.; Tamura, M.; Linz, H.; Samal, M. R.; Ghosh, S. K.

    2015-11-01

    NIR photometric observations in J (1.25um), H (1.63um), and Ks (2.14um) bands (centred on RA=16:18:31, DE=-50:17:32 (2000)) were carried out on 2004 July 29 using the 1.4m Infrared Survey Facility (IRSF) telescope, South Africa. The observations were taken with the help of the Simultaneous InfraRed Imager for Unbiased Survey (SIRIUS) instrument, a three colour simultaneous camera mounted at the f/10 Cassegrain focus of the telescope. Radio continuum observations at 1280MHz were obtained on 2012 November 09 using the Giant Metrewave Radio Telescope (GMRT) array. The GMRT array consists of 30 antennas arranged in an approximate Y-shaped configuration, with each antenna having a diameter of 45m. This translates to a primary beam-size of 26.2-arcmin at 1280MHz. (2 data files).

  3. Blue stragglers in open clusters - a test of the binary hypothesis

    International Nuclear Information System (INIS)

    Manteiga, M.; Martinez, R.C.; Beckman, J.E.; Pickles, A.J.

    1987-01-01

    A search for binaries among 17 blue stragglers in five galactic clusters, NGC 7789, 6633, 6819, 6939, and M 67, has been performed using measurements of radial velocity variations. The spectra were obtained with the Intermediate Dispersion Spectrograph attached to the f/15 Cassegrain focus of the 2.5 m Isaac Newton Telescope at the Spanish Observatory of the Roque de los Muchachos. The wavelength coverage was 200 A, centered at 8510 A with a scale of 12.4 km/sec per pixel. All radial velocity determinations were made using cross-correlation techniques. A velocity resolution of about 3 km/sec/pixel was obtained for the standard radial velocity stars and the brighter program stars. For three of the blue stragglers variations in radial velocity greater than 30 km/sec are reported. 10 references

  4. Recent observational evidence on W Ursae Majoris stars

    International Nuclear Information System (INIS)

    Rovithis-Livaniou, H.; Rovithis, P.

    1982-01-01

    During the last four years (1978-1981), some close binaries of W Ursae Majoris type have been observed from the National Observatory of Athens. In all cases a two-beam, multi-mode, nebular-stellar photometer has been used, attached to the 48-inch Cassegrain reflector at the Kryonerion Station. The observed systems are: 44i Boo, VW Cep, AB And, BV Dra, BW Dra, U Peg, V508 Oph. Especially VW Cep and 44i Boo, are very interesting objects; in addition to the light curves that have already been published (Rovithis and Rovithis-Livaniou, 1980-1981), other observations were obtained during the last year and are now at computational stage. The observations of these two systems will be continued during the next years. (Auth.)

  5. Where size does matter: foldable telescope design for microsat application

    Science.gov (United States)

    Segert, Tom; Danziger, Björn; Lieder, Matthias

    2017-11-01

    The DOBSON SPACE TELESCOPE Project (DST) at the Technical University of Berlin (TUB) believes that micro satellites can be a challenging competitor in the high resolution remote sensing market. Using a micro satellite as basis for a remote sensing platform will dramatically reduce the cost for the end users thereby initiating the predicted remote sensing boom. The Challenging task is that an optic required for a GSD smaller than 1m is much bigger than the given room for secondary payload. In order to break the volume limits of hitchhiker payloads the DST team develops an optical telescope with deployable structures. The core piece of DST is a 20 inch modified Cassegrain optic. Stored during ascend the instrument fits in a box measuring 60 x 60 x 30cm (including telescope and optical plane assembly). After the satellite was released into free space the telescope unfolds and collimates automatically.

  6. Multilayer X-ray imaging systems

    Science.gov (United States)

    Shealy, D. L.; Hoover, R. B.; Gabardi, D. R.

    1986-01-01

    An assessment of the imaging properties of multilayer X-ray imaging systems with spherical surfaces has been made. A ray trace analysis was performed to investigate the effects of using spherical substrates (rather than the conventional paraboloidal/hyperboloidal contours) for doubly reflecting Cassegrain telescopes. These investigations were carried out for mirrors designed to operate at selected soft X-ray/XUV wavelengths that are of significance for studies of the solar corona/transition region from the Stanford/MSFC Rocket X-Ray Telescope. The effects of changes in separation of the primary and secondary elements were also investigated. These theoretical results are presented as well as the results of ray trace studies to establish the resolution and vignetting effects as a function of field angle and system parameters.

  7. Design of a normal incidence multilayer imaging X-ray microscope

    Science.gov (United States)

    Shealy, David L.; Gabardi, David R.; Hoover, Richard B.; Walker, Arthur B. C., Jr.; Lindblom, Joakim F.

    Normal incidence multilayer Cassegrain X-ray telescopes were flown on the Stanford/MSFC Rocket X-ray Spectroheliograph. These instruments produced high spatial resolution images of the sun and conclusively demonstrated that doubly reflecting multilayer X-ray optical systems are feasible. The images indicated that aplanatic imaging soft X-ray/EUV microscopes should be achievable using multilayer optics technology. A doubly reflecting normal incidence multilayer imaging X-ray microscope based on the Schwarzschild configuration has been designed. The design of the microscope and the results of the optical system ray trace analysis are discussed. High resolution aplanatic imaging X-ray microscopes using normal incidence multilayer X-ray mirrors should have many important applications in advanced X-ray astronomical instrumentation, X-ray lithography, biological, biomedical, metallurgical, and laser fusion research.

  8. Low noise cryogenic receiver for spectroscopic applications in mm-wave radioastronomy at 230 GHz

    International Nuclear Information System (INIS)

    Pagani, L.; Ruffie, G.; Beaudin, G.; Gheudin, M.; Deschamps, A.

    1986-01-01

    A new cooled mm-wave receiver is presented. This receiver has been in operation since October 1985 with a 2.5 m Cassegrain telescope located at the Plateau de Bure in the French Alps. It is tunable from 210 to 240 GHz and has a DSB system noise temperature of 360 K and a 600 MHz instantaneous bandwidth. The receiver is composed of a local oscillator (klystron frequency tripler) and a Schottky diode mixer with a cooled FET amplifier. Quasi-optical techniques are used for signal injection. A computer-controlled microprocessor drives the whole system and performs calibration and frequency tuning of the receiver. The different parts of the receiver, frequency tripler, quasi-optical techniques, mixer, FET amplifier, and microprocessor, are described. 13 references

  9. Large Deployable Reflector (LDR) - A concept for an orbiting submillimeter-infrared telescope for the 1990s

    Science.gov (United States)

    Swanson, P. N.; Gulkis, S.; Kulper, T. B. H.; Kiya, M.

    1983-01-01

    The history and background of the Large Deployable Reflector (LDR) are reviewed. The results of the June 1982 Asilomar (CA) workshop are incorporated into the LDR science objectives and telescope concept. The areas where the LDR may have the greatest scientific impact are in the study of star formation and planetary systems in the own and nearby galaxies and in cosmological studies of the structure and evolution of the early universe. The observational requirements for these and other scientific studies give rise to a set of telescope functional requirements. These, in turn, are satisfied by an LDR configuration which is a Cassegrain design with a 20 m diameter, actively controlled, segmented, primary reflector, diffraction limited at a wavelength of 30 to 50 microns. Technical challenges in the LDR development include construction of high tolerance mirror segments, surface figure measurement, figure control, vibration control, pointing, cryogenics, and coherent detectors. Project status and future plans for the LDR are discussed.

  10. Opto-mechanical design of ShaneAO: the adaptive optics system for the 3-meter Shane Telescope

    Science.gov (United States)

    Ratliff, C.; Cabak, J.; Gavel, D.; Kupke, R.; Dillon, D.; Gates, E.; Deich, W.; Ward, J.; Cowley, D.; Pfister, T.; Saylor, M.

    2014-07-01

    A Cassegrain mounted adaptive optics instrument presents unique challenges for opto-mechanical design. The flexure and temperature tolerances for stability are tighter than those of seeing limited instruments. This criteria requires particular attention to material properties and mounting techniques. This paper addresses the mechanical designs developed to meet the optical functional requirements. One of the key considerations was to have gravitational deformations, which vary with telescope orientation, stay within the optical error budget, or ensure that we can compensate with a steering mirror by maintaining predictable elastic behavior. Here we look at several cases where deformation is predicted with finite element analysis and Hertzian deformation analysis and also tested. Techniques used to address thermal deformation compensation without the use of low CTE materials will also be discussed.

  11. Apparent luminosity function of galaxies to the twenty-first magnitude

    International Nuclear Information System (INIS)

    Brown, G.S.

    1979-01-01

    Galaxy counts to limiting magnitudes B=17.7 to 21.0 in 13 selected areas in the north galactic polar cap are presented. The photographs were taken with a reducing camera at the Cassegrain focus of the 91 cm and 205 cm reflectors of McDonald Observatory. Both galaxy and star images were counted and recorded. On each plate a few stars and galaxies were marked as representative of the plate limit. Selected brighter galaxies and stars were measured photoelectrically to fix the zero points. The B magnitude limits of each plate for stars and galaxies are obtained by a combination of photoelectric and photographic photometry. The resulting apparent luminosity functions of galaxies and stars are compared with earlier data. Sources of error in the counts are discussed in detail

  12. New redshifts of bright galaxies. III

    International Nuclear Information System (INIS)

    de Vaucouleurs, G.; de Vaucouleurs, A.; Nieto, J.

    1979-01-01

    Redshifts of 196 bright galaxies, and 2 QSO's are derived from 246 spectrograms obtained from 1972 to 1977 with the Galaxy meter's two-state image tube grism spectrograph attached at the Cassegrain focus of the McDonald Observatory Struve reflector. The reciprocal dispersion in 335 A/mm at Hα and the wavelength range lambdalambda 4500--8000 A. The galaxy redshifts are in the range -28 -1 , but few exceed 5,000 km s -1 . The internal mean errors of the weighted mean velocities range from 22 to 140 km s -1 . Comparisons with other systems of redshifts, particularly the RC2, 21-cm and Sandage systems, indicate a mean systematic error of -35 +- 16 km s -1 , but it is probably variable with V. The external mean error is sigma*=90 km s -1 for velocities V -1 having a mean weight =4.0

  13. Sodium temperature/wind lidar based on laser-diode-pumped Nd:YAG lasers deployed at Tromsø, Norway (69.6°N, 19.2°E).

    Science.gov (United States)

    Kawahara, T D; Nozawa, S; Saito, N; Kawabata, T; Tsuda, T T; Wada, S

    2017-06-12

    An Nd:YAG laser-based sodium temperature/wind lidar was developed for the measurement of the northern polar mesosphere and lower thermosphere at Tromsø (69.6N, 19.2E), Norway. Coherent light at 589 nm is produced by sum frequency generation of 1064 nm and 1319 nm from two diode laser end-pumped pulsed Nd:YAG lasers. The output power is as high as 4W, with 4 mJ/pulse at 1000 Hz repetition rate. Five tilting Cassegrain telescopes enable us to make five-direction (zenith, north, south, east, west) observation for temperature and wind simultaneously. This highly stable laser system is first of its kind to operate virtually maintenance-free during the observation season (from late September to March) since 2010.

  14. The High-Resolution Lightweight Telescope for the EUV (HiLiTE)

    Energy Technology Data Exchange (ETDEWEB)

    Martinez-Galarce, D S; Boerner, P; Soufli, R; De Pontieu, B; Katz, N; Title, A; Gullikson, E M; Robinson, J C; Baker, S L

    2008-06-02

    The High-resolution Lightweight Telescope for the EUV (HiLiTE) is a Cassegrain telescope that will be made entirely of Silicon Carbide (SiC), optical substrates and metering structure alike. Using multilayer coatings, this instrument will be tuned to operate at the 465 {angstrom} Ne VII emission line, formed in solar transition region plasma at {approx}500,000 K. HiLiTE will have an aperture of 30 cm, angular resolution of {approx}0.2 arc seconds and operate at a cadence of {approx}5 seconds or less, having a mass that is about 1/4 that of one of the 20 cm aperture telescopes on the Atmospheric Imaging Assembly (AIA) instrument aboard NASA's Solar Dynamics Observatory (SDO). This new instrument technology thus serves as a path finder to a post-AIA, Explorer-class missions.

  15. Wavefront control of the Large Optics Test and Integration Site (LOTIS) 6.5m Collimator

    Energy Technology Data Exchange (ETDEWEB)

    West, Steven C.; Bailey, Samuel H.; Burge, James H.; Cuerden, Brian; Hagen, Jeff; Martin, Hubert M.; Tuell, Michael T.

    2010-06-20

    The LOTIS Collimator provides scene projection within a 6.5m diameter collimated beam used for optical testing research in air and vacuum. Diffraction-limited performance (0.4 to 5{mu}m wavelength) requires active wavefront control of the alignment and primary mirror shape. A hexapod corrects secondary mirror alignment using measurements from collimated sources directed into the system with nine scanning pentaprisms. The primary mirror shape is controlled with 104 adjustable force actuators based on figure measurements from a center-of-curvature test. A variation of the Hartmann test measures slopes by monitoring the reflections from 36 small mirrors bonded to the optical surface of the primary mirror. The Hartmann source and detector are located at the f/15 Cassegrain focus. Initial operation has demonstrated a closed-loop 110nmrms wavefront error in ambient air over the 6.5mcollimated beam.

  16. Observations of new Wolf-Rayet binaries

    International Nuclear Information System (INIS)

    Niemela, V.S.

    1982-01-01

    The author reports here preliminary results of spectrographic observations for three southern WR stars, whose binary nature had not been previously verified: HDE 320102, CD -45 0 4482, HD 62910. The observations were carried out at the Cerro Tololo Inter-American Observatory, Chile, mostly with the Cassegrain spectrograph with IT attached to the 1-m reflector. These spectrograms were secured on Kodak IIIaJ emulsion, and have a dispersion of 45 A/mm. The results suggest that HDE 320102 must be a double-lined 05-7 + WN3 spectroscopic binary, that CD -45 0 4482 appears to be a single-lined spectroscopic binary and that HD 62910 may be a binary. (Auth.)

  17. Methods for the performance enhancement and the error characterization of large diameter ground-based diffractive telescopes.

    Science.gov (United States)

    Zhang, Haolin; Liu, Hua; Lizana, Angel; Xu, Wenbin; Caompos, Juan; Lu, Zhenwu

    2017-10-30

    This paper is devoted to the improvement of ground-based telescopes based on diffractive primary lenses, which provide larger aperture and relaxed surface tolerance compared to non-diffractive telescopes. We performed two different studies devised to thoroughly characterize and improve the performance of ground-based diffractive telescopes. On the one hand, we experimentally validated the suitability of the stitching error theory, useful to characterize the error performance of subaperture diffractive telescopes. On the other hand, we proposed a novel ground-based telescope incorporated in a Cassegrain architecture, leading to a telescope with enhanced performance. To test the stitching error theory, a 300 mm diameter, 2000 mm focal length transmissive stitching diffractive telescope, based on a three-belt subaperture primary lens, was designed and implemented. The telescope achieves a 78 cy/mm resolution within 0.15 degree field of view while the working wavelength ranges from 582.8 nm to 682.8 nm without any stitching error. However, the long optical track (35.49 m) introduces air turbulence that reduces the final images contrast in the ground-based test. To enhance this result, a same diameter compacted Cassegrain ground-based diffractive (CGD) telescope with the total track distance of 1.267 m, was implemented within the same wavelength. The ground-based CGD telescope provides higher resolution and better contrast than the transmissive configuration. Star and resolution tests were experimentally performed to compare the CGD and the transmissive configurations, providing the suitability of the proposed ground-based CGD telescope.

  18. Prime focus architectures for large space telescopes: reduce surfaces to save cost

    Science.gov (United States)

    Breckinridge, J. B.; Lillie, C. F.

    2016-07-01

    Conceptual architectures are now being developed to identify future directions for post JWST large space telescope systems to operate in the UV Optical and near IR regions of the spectrum. Here we show that the cost of optical surfaces within large aperture telescope/instrument systems can exceed $100M/reflection when expressed in terms of the aperture increase needed to over come internal absorption loss. We recommend a program in innovative optical design to minimize the number of surfaces by considering multiple functions for mirrors. An example is given using the Rowland circle imaging spectrometer systems for UV space science. With few exceptions, current space telescope architectures are based on systems optimized for ground-based astronomy. Both HST and JWST are classical "Cassegrain" telescopes derived from the ground-based tradition to co-locate the massive primary mirror and the instruments at the same end of the metrology structure. This requirement derives from the dual need to minimize observatory dome size and cost in the presence of the Earth's 1-g gravitational field. Space telescopes, however function in the zero gravity of space and the 1- g constraint is relieved to the advantage of astronomers. Here we suggest that a prime focus large aperture telescope system in space may have potentially have higher transmittance, better pointing, improved thermal and structural control, less internal polarization and broader wavelength coverage than Cassegrain telescopes. An example is given showing how UV astronomy telescopes use single optical elements for multiple functions and therefore have a minimum number of reflections.

  19. TESS Follow-up Observing Programs at the University of Wyoming

    Science.gov (United States)

    Jang-Condell, Hannah; Kasper, David; Kar, Aman; Sorber, Rebecca; Hancock, Daniel A.; Leuquire, Jacob D.; Suhaimi, Afiq; Kobulnicky, Henry A.; Pierce, Michael; Pilachowski, Catherine A.

    2018-06-01

    The Transiting Exoplanet Survey Satellite (TESS), launched in Spring 2018, will detect thousands of new exoplanet candidates. These candidates will need to be vetted by ground-based observatories to rule out false positives. The Observatories at the University of Wyoming are well-positioned to take active roles in TESS Follow-Up Observing Program (TFOP) Working Groups. The 0.6-m Red Buttes Observatory has already demonstrated its capability to do precision photometric monitoring of transiting exoplanet targets as a participant in the Kilodegree Extremely Little Telescope Follow-Up Network (KELT-FUN). A new echelle spectrograph, Fiber High-Resolution Echelle (FHiRE), being built for the 2.3-m Wyoming InfraRed Observatory (WIRO), will enable precision radial velocity measurements of exoplanet candidates. Over 180 nights/year at both observatories will be available to our team to undertake follow-up observations of TESS Objects of Interest (TOIs). We anticipate making significant contributions to new exoplanet discoveries in the era of TESS.

  20. CHEMICAL ABUNDANCE EVIDENCE OF ENDURING HIGH STAR FORMATION RATES IN AN EARLY-TYPE GALAXY: HIGH [Ca/Fe] IN NGC 5128 GLOBULAR CLUSTERS

    International Nuclear Information System (INIS)

    Colucci, Janet E.; Durán, María Fernanda; Bernstein, Rebecca A.; McWilliam, Andrew

    2013-01-01

    We present [Fe/H], ages, and Ca abundances for an initial sample of 10 globular clusters in NGC 5128 obtained from high-resolution, high signal-to-noise ratio echelle spectra of their integrated light. All abundances and ages are obtained using our original technique for high-resolution integrated light abundance analysis of globular clusters. The clusters have a range in [Fe/H] between –1.6 and –0.2. In this sample, the average [Ca/Fe] for clusters with [Fe/H] <–0.4 is +0.37 ± 0.07, while the average [Ca/Fe] in our Milky Way (MW) and M31 GC samples is +0.29 ± 0.09 and +0.24 ± 0.10, respectively. This may imply a more rapid chemical enrichment history for NGC 5128 than for either the MW or M31. This sample provides the first quantitative picture of the chemical history of NGC 5128 that is directly comparable to what is available for the MW. Data presented here were obtained with the MIKE echelle spectrograph on the Magellan Clay Telescope

  1. Emission lines of [K V] in the optical spectra of gaseous nebulae.

    Science.gov (United States)

    Keenan, Francis P; Aller, Lawrence H; Espey, Brian R; Exter, Katrina M; Hyung, Siek; Keenan, Michael T C; Pollacco, Don L; Ryans, Robert S I

    2002-04-02

    Recent R-matrix calculations of electron impact excitation rates in K v are used to derive the nebular emission line ratio R = I(4122.6 A)/I(4163.3 A) as a function of electron density (N(e)). This ratio is found to be very sensitive to changes in N(e) over the density range 10(3) to 10(6) cm(-3), but does not vary significantly with electron temperature, and hence in principle should provide an excellent optical N(e) diagnostic for the high-excitation zones of nebulae. The observed value of R for the planetary nebula NGC 7027, measured from a spectrum obtained with the Hamilton Echelle spectrograph on the 3-m Shane Telescope, implies a density in excellent agreement with that derived from [Ne iv], formed in the same region of the nebula as [K v]. This observation provides observational support for the accuracy of the theoretical [K v] line ratios, and hence the atomic data on which they are based. However, the analysis of a high-resolution spectrum of the symbiotic star RR Telescopii, obtained with the University College London Echelle Spectrograph on the 3.9-m Anglo-Australian Telescope, reveals that the [K v] 4122.6 A line in this object is badly blended with Fe ii 4122.6 A. Hence, the [K v] diagnostic may not be used for astrophysical sources that show a strong Fe ii emission line spectrum.

  2. Updates on the Performance and Calibration of HST/STIS

    Science.gov (United States)

    Lockwood, Sean A.; Monroe, TalaWanda R.; Ogaz, Sara; Branton, Doug; Carlberg, Joleen K.; Debes, John H.; Jedrzejewski, Robert I.; Proffitt, Charles R.; Riley, Allyssa; Sohn, Sangmo Tony; Sonnentrucker, Paule; Walborn, Nolan R.; Welty, Daniel

    2018-06-01

    The Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST) has been in orbit for 21 years and continues to produce high quality scientific results using a diverse complement of operating modes. These include spatially resolved spectroscopy in the UV and optical, high spatial resolution echelle spectroscopy in the UV, and solar-blind imaging in the UV. In addition, STIS possesses unique visible-light coronagraphic modes that keep the instrument at the forefront of exoplanet and debris-disk research. As the instrument's characteristics evolve over its lifetime, the instrument team at the Space Telescope Science Institute monitors its performance and works towards improving the quality of its data products. Here we present updates on the status of the STIS CCD and FUV & NUV MAMA detectors, as well as changes to the CalSTIS reduction pipeline. We also discuss progress toward the recalibration of the E140M/1425 echelle mode. The E140M grating blaze function shapes have changed since flux calibration was carried out following SM4, which limits the relative photometric flux accuracy of some spectral orders up to 5-10% at the edges. In Cycle 25 a special calibration program was executed to obtain updated sensitivity curves for the E140M/1425 setting.

  3. Design study of the PEPSI polarimeter for the LBT

    Science.gov (United States)

    Hofmann, A.; Strassmeier, K. G.; Woche, M.

    2002-07-01

    We present the conceptual design of the two polarimetric channels of the PEPSI spectropolarimeter for the Large Binocular Telescope (LBT). The two direct Gregorian f/15 focii of the LBT will take up two identical but independent full-Stokes IQUV polarimeters that themselves fiberfeed a high-resolution Echelle spectrograph (see the accompanying paper by Zerbi et al.). The polarizing units will be based on super-achromatic Fresnel-rhomb retarders and Foster prisms. A total of four fibers are foreseen to simultaneously direct two ordinary and two extraordinary light beams to the Echelle spectrograph. Both polarimetric units are layed out in a modular design, each one optimized to the polarization state in which it is used. A number of observing modes can be chosen that are optimized to the type of polarization that is expected from the target, e.g. circularly and linearly polarized light simultaneously, or linearly polarized light in both polarimeters, or integral light from one and polarized light from the other telescope, a.s.o.. Calibration would be provided for each polarimeter separately.

  4. Optical design of the PEPSI high-resolution spectrograph at LBT

    Science.gov (United States)

    Andersen, Michael I.; Spano, Paolo; Woche, Manfred; Strassmeier, Klaus G.; Beckert, Erik

    2004-09-01

    PEPSI is a high-resolution, fiber fed echelle spectrograph with polarimetric capabilities for the LBT. In order to reach a maximum resolution R=120.000 in polarimetric mode and 300.000 in integral light mode with high efficiency in the spectral range 390-1050~nm, we designed a white-pupil configuration with Maksutov collimators. Light is dispersed by an R4 31.6 lines/mm monolithic echelle grating mosaic and split into two arms through dichroics. The two arms, optimized for the spectral range 390-550~nm and 550-1050~nm, respectively, consist of Maksutov transfer collimators, VPH-grism cross dispersers, optimized dioptric cameras and 7.5K x 7.5K 8~μ CCDs. Fibers of different core sizes coupled to different image-slicers allow a high throughput, comparable to that of direct feed instruments. The optical configuration with only spherical and cylindrical surfaces, except for one aspherical surface in each camera, reduces costs and guarantees high optical quality. PEPSI is under construction at AIP with first light expected in 2006.

  5. Can we use adaptive optics for UHR spectroscopy with PEPSI at the LBT?

    Science.gov (United States)

    Sacco, Germano G.; Pallavicini, Roberto; Spano, Paolo; Andersen, Michael; Woche, Manfred F.; Strassmeier, Klaus G.

    2004-10-01

    We investigate the potential of using adaptive optics (AO) in the V, R, and I bands to reach ultra-high resolution (UHR, R >= 200,000) in echelle spectrographs at 8-10m telescopes. In particular, we investigate the possibility of implementing an UHR mode for the fiber-fed spectrograph PEPSI (Potsdam Echelle Polarimetric and Spectrographic Instrument) being developed for the Large Binocular Telescope (LBT). By simulating the performances of the advanced AO system that will be available at first light at the LBT, and by using first-order estimates of the spectrograph performances, we calculate the total efficiency and signal to noise ratio (SNR) of PEPSI in the AO mode for stars of different magnitudes, different fiber core sizes, and different fractions of incident light diverted to the wavefront sensor. We conclude that AO can provide a significant advantage, of up to a factor ~2 in the V, R and I bands, for stars brighter than mR ~ 12 - 13. However, if these stars are observed at UHR in non-AO mode, slit losses caused by the need to use a very narrow slit can be compensated more effectively by the use of image slicers.

  6. PEPSI spectro-polarimeter for the LBT

    Science.gov (United States)

    Strassmeier, Klaus G.; Hofmann, Axel; Woche, Manfred F.; Rice, John B.; Keller, Christoph U.; Piskunov, N. E.; Pallavicini, Roberto

    2003-02-01

    PEPSI (Postham Echelle Polarimetric and Spectroscopic Instrument) is to use the unique feature of the LBT and its powerful double mirror configuration to provide high and extremely high spectral resolution full-Stokes four-vector spectra in the wavelength range 450-1100nm. For the given aperture of 8.4m in single mirror mode and 11.8m in double mirror mode, and at a spectral resolution of 40,000-300,000 as designed for the fiber-fed Echelle spectrograph, a polarimetric accuracy between 10-4 and 10-2 can be reached for targets with visual magnitudes of up to 17th magnitude. A polarimetric accuracy better than 10-4 can only be reached for either targets brighter than approximately 10th magnitude together wiht a substantial trade-off wiht the spectral resolution or with spectrum deconvolution techniques. At 10-2, however, we will be able to observe the brightest AGNs down to 17th magnitude.

  7. Calibration Efforts and Unique Capabilities of the HST Space Telescope Imaging Spectrograph

    Science.gov (United States)

    Monroe, TalaWanda R.; Proffitt, Charles R.; Welty, Daniel; Branton, Doug; Carlberg, Joleen K.; debes, John Henry; Lockwood, Sean; Riley, Allyssa; Sohn, Sangmo Tony; Sonnentrucker, Paule G.; Walborn, Nolan R.; Jedrzejewski, Robert I.

    2018-01-01

    The Space Telescope Imaging Spectrograph (STIS) continues to offer the astronomy community the ability to carry out innovative UV and optical spectroscopic and imaging studies, two decades after its deployment on the Hubble Space Telescope (HST). Most notably, STIS provides spectroscopy in the FUV and NUV, including high spectral resolution echelle modes, imaging in the FUV, optical spectroscopy, and coronagraphic capabilities. Additionally, spatial scanning on the CCD with the long-slits is now possible to enable very high S/N spectroscopic observations without saturation while mitigating telluric and fringing concerns in the far red and near-IR. This new mode may especially benefit the diffuse interstellar bands and exoplanet transiting communities. We present recent calibration efforts for the instrument, including work to optimize the calibration of the echelle spectroscopic modes by improving the flux agreement of overlapping spectral orders affected by changes in the grating blaze function since HST Servicing Mission 4. We also discuss considerations to maintain the wavelength precision of the spectroscopic modes, and the current capabilities of CCD spectroscopic spatial trails.

  8. CHEMICAL ABUNDANCE EVIDENCE OF ENDURING HIGH STAR FORMATION RATES IN AN EARLY-TYPE GALAXY: HIGH [Ca/Fe] IN NGC 5128 GLOBULAR CLUSTERS

    Energy Technology Data Exchange (ETDEWEB)

    Colucci, Janet E.; Duran, Maria Fernanda; Bernstein, Rebecca A. [Department of Astronomy and Astrophysics, 1156 High Street, UCO/Lick Observatory, University of California, Santa Cruz, CA 95064 (United States); McWilliam, Andrew, E-mail: jcolucci@ucolick.org [Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA 91101-1292 (United States)

    2013-08-20

    We present [Fe/H], ages, and Ca abundances for an initial sample of 10 globular clusters in NGC 5128 obtained from high-resolution, high signal-to-noise ratio echelle spectra of their integrated light. All abundances and ages are obtained using our original technique for high-resolution integrated light abundance analysis of globular clusters. The clusters have a range in [Fe/H] between -1.6 and -0.2. In this sample, the average [Ca/Fe] for clusters with [Fe/H] <-0.4 is +0.37 {+-} 0.07, while the average [Ca/Fe] in our Milky Way (MW) and M31 GC samples is +0.29 {+-} 0.09 and +0.24 {+-} 0.10, respectively. This may imply a more rapid chemical enrichment history for NGC 5128 than for either the MW or M31. This sample provides the first quantitative picture of the chemical history of NGC 5128 that is directly comparable to what is available for the MW. Data presented here were obtained with the MIKE echelle spectrograph on the Magellan Clay Telescope.

  9. Chemical Abundance Evidence of Enduring High Star Formation Rates in an Early-type Galaxy: High [Ca/Fe] in NGC 5128 Globular Clusters

    Science.gov (United States)

    Colucci, Janet E.; Fernanda Durán, María; Bernstein, Rebecca A.; McWilliam, Andrew

    2013-08-01

    We present [Fe/H], ages, and Ca abundances for an initial sample of 10 globular clusters in NGC 5128 obtained from high-resolution, high signal-to-noise ratio echelle spectra of their integrated light. All abundances and ages are obtained using our original technique for high-resolution integrated light abundance analysis of globular clusters. The clusters have a range in [Fe/H] between -1.6 and -0.2. In this sample, the average [Ca/Fe] for clusters with [Fe/H] <-0.4 is +0.37 ± 0.07, while the average [Ca/Fe] in our Milky Way (MW) and M31 GC samples is +0.29 ± 0.09 and +0.24 ± 0.10, respectively. This may imply a more rapid chemical enrichment history for NGC 5128 than for either the MW or M31. This sample provides the first quantitative picture of the chemical history of NGC 5128 that is directly comparable to what is available for the MW. Data presented here were obtained with the MIKE echelle spectrograph on the Magellan Clay Telescope. This Letter includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.

  10. Turbulent conductivity in parallel with iso-velocities in a planar established flow; Conductibilite turbulente parallelement aux isovitesses dans un ecoulement plan en regime etabli

    Energy Technology Data Exchange (ETDEWEB)

    Jullien, F [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires, Direction des piles atomiques

    1968-02-01

    In this thesis are presented the experimental results obtained during the study of the turbulent diffusion of heat using a wire source in a flat air flow. The Taylor statistical theory laws are well respected in the domain studied. The experiments have made it possible to evaluate the influence of the Reynolds number and of the distance from the wall on the quadratic values of velocity fluctuations and on the Lagrange turbulence scales. In particular, the author has found a correlation between the Lagrange scales and the friction coefficient when the Reynolds number varies. A diffusion law is derived from the Taylor theory; it makes it possible to explain more clearly the idea of turbulent conductivity. (author) [French] Cette these presente les resultats experimentaux de l'etude de la diffusion turbulente de la chaleur a partir d'un fil source dans un ecoulement d'air plan. Les lois de la theorie statistique de Taylor sont bien verifiees dans le domaine d'etude. Les experiences ont permis d'evaluer l'influence du nombre de Reynolds et de la distance a la paroi sur les valeurs quadratiques des fluctuations de vitesse et les echelles lagrangiennes de turbulence. En particulier, l'auteur a trouve une correlation entre les echelles lagrangiennes et le coefficient de frottement lorsque le nombre de Reynolds varie. Comme consequences de la theorie de Taylor, une loi de diffusion est etablie et permet de preciser la notion de conductibilite turbulente. (auteur)

  11. Chemical abundances of fast-rotating massive stars. I. Description of the methods and individual results

    Science.gov (United States)

    Cazorla, Constantin; Morel, Thierry; Nazé, Yaël; Rauw, Gregor; Semaan, Thierry; Daflon, Simone; Oey, M. S.

    2017-07-01

    Aims: Recent observations have challenged our understanding of rotational mixing in massive stars by revealing a population of fast-rotating objects with apparently normal surface nitrogen abundances. However, several questions have arisen because of a number of issues, which have rendered a reinvestigation necessary; these issues include the presence of numerous upper limits for the nitrogen abundance, unknown multiplicity status, and a mix of stars with different physical properties, such as their mass and evolutionary state, which are known to control the amount of rotational mixing. Methods: We have carefully selected a large sample of bright, fast-rotating early-type stars of our Galaxy (40 objects with spectral types between B0.5 and O4). Their high-quality, high-resolution optical spectra were then analysed with the stellar atmosphere modelling codes DETAIL/SURFACE or CMFGEN, depending on the temperature of the target. Several internal and external checks were performed to validate our methods; notably, we compared our results with literature data for some well-known objects, studied the effect of gravity darkening, or confronted the results provided by the two codes for stars amenable to both analyses. Furthermore, we studied the radial velocities of the stars to assess their binarity. Results: This first part of our study presents our methods and provides the derived stellar parameters, He, CNO abundances, and the multiplicity status of every star of the sample. It is the first time that He and CNO abundances of such a large number of Galactic massive fast rotators are determined in a homogeneous way. Based on observations obtained with the Heidelberg Extended Range Optical Spectrograph (HEROS) at the Telescopio Internacional de Guanajuato (TIGRE) with the SOPHIE échelle spectrograph at the Haute-Provence Observatory (OHP; Institut Pytheas; CNRS, France), and with the Magellan Inamori Kyocera Echelle (MIKE) spectrograph at the Magellan II Clay telescope

  12. Hanging-wall deformation above a normal fault: sequential limit analyses

    Science.gov (United States)

    Yuan, Xiaoping; Leroy, Yves M.; Maillot, Bertrand

    2015-04-01

    to Dahl, 1987). References: Egholm, D. L., M. Sandiford, O. R. Clausen, and S. B. Nielsen (2007), A new strategy for discrete element numerical models: 2. sandbox applications, Journal of Geophysical Research, 112 (B05204), doi:10.1029/2006JB004558. Groshong, R. H. (1989), Half-graben structures: Balanced models of extensional fault-bend folds, Geological Society of America Bulletin, 101 (1), 96-105. Patton, T. L. (2005), Sandbox models of downward-steepening normal faults, AAPG Bulletin, 89 (6), 781-797. Xiao, H.-B., and J. Suppe (1992), Orgin of rollover, AAPG Bulletin, 76 (4), 509-529.

  13. A Powerful Twin Arrives

    Science.gov (United States)

    1999-11-01

    First Images from FORS2 at VLT KUEYEN on Paranal The first, major astronomical instrument to be installed at the ESO Very Large Telescope (VLT) was FORS1 ( FO cal R educer and S pectrograph) in September 1998. Immediately after being attached to the Cassegrain focus of the first 8.2-m Unit Telescope, ANTU , it produced a series of spectacular images, cf. ESO PR 14/98. Many important observations have since been made with this outstanding facility. Now FORS2 , its powerful twin, has been installed at the second VLT Unit Telescope, KUEYEN . It is the fourth major instrument at the VLT after FORS1 , ISAAC and UVES.. The FORS2 Commissioning Team that is busy installing and testing this large and complex instrument reports that "First Light" was successfully achieved already on October 29, 1999, only two days after FORS2 was first mounted at the Cassegrain focus. Since then, various observation modes have been carefully tested, including normal and high-resolution imaging, echelle and multi-object spectroscopy, as well as fast photometry with millisecond time resolution. A number of fine images were obtained during this work, some of which are made available with the present Press Release. The FORS instruments ESO PR Photo 40a/99 ESO PR Photo 40a/99 [Preview - JPEG: 400 x 345 pix - 203k] [Normal - JPEG: 800 x 689 pix - 563kb] [Full-Res - JPEG: 1280 x 1103 pix - 666kb] Caption to PR Photo 40a/99: This digital photo shows the twin instruments, FORS2 at KUEYEN (in the foreground) and FORS1 at ANTU, seen in the background through the open ventilation doors in the two telescope enclosures. Although they look alike, the two instruments have specific functions, as described in the text. FORS1 and FORS2 are the products of one of the most thorough and advanced technological studies ever made of a ground-based astronomical instrument. They have been specifically designed to investigate the faintest and most remote objects in the universe. They are "multi-mode instruments" that

  14. The Unique Optical Design of the CTI-II Survey Telescope

    Science.gov (United States)

    Ackermann, Mark R.; McGraw, J. T.; MacFarlane, M.

    2006-12-01

    The CCD/Transit Instrument with Innovative Instrumentation (CTI-II) is being developed for precision ground-based astrometric and photometric astronomical observations. The 1.8m telescope will be stationary, near-zenith pointing and will feature a CCD-mosaic array operated in time-delay and integrate (TDI) mode to image a continuous strip of the sky in five bands. The heart of the telescope is a Nasmyth-like bent-Cassegrain optical system optimized to produce near diffraction-limited images with near zero distortion over a circular1.42 deg field. The optical design includes an f/2.2 parabolic ULE primary with no central hole salvaged from the original CTI telescope and adds the requisite hyperbolic secondary, a folding flat and a highly innovative all-spherical, five lens corrector which includes three plano surfaces. The reflective and refractive portions of the design have been optimized as individual but interdependent systems so that the same reflective system can be used with slightly different refractive correctors. At present, two nearly identical corrector designs are being evaluated, one fabricated from BK-7 glass and the other of fused silica. The five lens corrector consists of an air-spaced triplet separated from follow-on air-spaced doublet. Either design produces 0.25 arcsecond images at 83% encircled energy with a maximum of 0.0005% distortion. The innovative five lens corrector design has been applied to other current and planned Cassegrain, RC and super RC optical systems requiring correctors. The basic five lens approach always results in improved performance compared to the original designs. In some cases, the improvement in image quality is small but includes substantial reductions in distortion. In other cases, the improvement in image quality is substantial. Because the CTI-II corrector is designed for a parabolic primary, it might be especially useful for liquid mirror telescopes. We describe and discuss the CTI-II optical design with respect

  15. Testing the Prediction of Iron Alteration Minerals on Low Albedo Asteroids

    Science.gov (United States)

    Jarvis, K. S.; Vilas, Faith; Howell, E.; Kelley, M.; Cochran, A.

    1999-01-01

    Absorption features centered near 0.60 - 0.65 and 0.80 - 0.90 micron were identified in the spectra of three low-albedo main-belt (165, 368, 877) and two low-albedo outer-belt (225, 334) asteroids (Vilas et al., Icarus, v. 109,274,1994). The absorption features were attributed to charge transfer transitions in iron alteration minerals such as goethite, hematite, and jarosite, all products of aqueous alteration. Concurrently, Jarvis et al. (LPSC XXIV, 715, 1993) presented additional spectra of low-albedo asteroids that had absorption features centered near 0.60 - 0.65 micron without the longer wavelength feature. Since these two features in iron oxides originate from the same ground state, and the longer wavelength feature requires less energy to exist, the single shorter wavelength feature cannot be caused by the iron alteration minerals. In addition, spectra of minerals such as hematite and goethite show a rapid increase in reflectance beginning near 0.5 micron absent in the low-albedo asteroid spectra. The absence of this rise has been attributed to its suppresion from opaques in the surface material. Spectra on more than one night were available for only one of these five asteroids, 225 Henrietta, and showed good repeatability of the 0.65-micron feature. We have acquired additional spectra of all five asteroids in order to test the repeatability of the 0.65-micron feature, and the presence and repeatability of the features centered near 0.8 - 0.9 micron. We specifically will test the possibility that longer wavelength features could be caused by incomplete removal of telluric water. Asteroid 877 Walkure is a member of the Nysa-Hertha family, and will be compared to spectra of other members of that family. Data were acquired in 1996 and 1999 on the 2.1-m telescope with a facility cassegrain spectrograph, McDonald Observatory, Univ. Of Texas, and the 1.5-m telescope with facility cassegrain spectrograph at CTIO. This research is supported by the NASA Planetary

  16. High-dispersion observations of H-alpha in the suspected brown dwarf, white dwarf binary system G29-38

    International Nuclear Information System (INIS)

    Liebert, J.; Saffer, R.A.; Pilachowski, C.A.

    1989-01-01

    High-dispersion spectroscopy of the H-alpha absorption line of the cool DA white dwarf G29-38 is reported. This is the star for which a recently detected IR excess has been suggested to be due to a possible brown dwarf companion. Three echelle spectra show no evidence for radial-velocity variations larger than about 1.1 + or - 8.7 km/s and are used to derive a weighted heliocentric radial velocity of 33.7 + or - 4.3 kms/s for the white dwarf. The observations of a sharp absorption-line core restricts the possible rotation of the white dwarf to 40 km/s or less and ensures that any surface magnetic field has a strength of 100,000 G or less. These results make it unlikely that the DA white dwarf has previously been in a cataclysmic variable accretion phase. 18 references

  17. Statistical treatment of data. Application to nuclear electronics; Traitement des informations en regime statistique. Applications a l'electronique nucleaire

    Energy Technology Data Exchange (ETDEWEB)

    Sicard, F [Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    In this report the data of probability calculations are applied to the analyses of counting losses in experiments on chance events encountered in nuclear physics. The distribution of time intervals according to Poisson's law is studied and various applications of this are given: calculation of counting losses on a scale preceded by a fast de-multiplying circuit, decrease of the counting rate on the multichannel selectors, recording of statistical distribution phenomena on magnetic bands. (author) [French] Ce rapport applique les donnees du calcul des probabilites a l'analyse des pertes de comptage dans les experiences sur des evenements aleatoires rencontres en physique nucleaire. La distribution des intervalles de temps suivant une loi de Poisson est etudiee et differentes applications en sont donnees: calcul des pertes de comptage sur une echelle precedee d'un circuit de demultiplication rapide, diminution du taux de comptage sur les selecteurs multicanaux, enregistrement de phenomenes a distribution statistique sur bandes magnetiques. (auteur)

  18. Spectroscopic instrumentation fundamentals and guidelines for astronomers

    CERN Document Server

    Eversberg, Thomas

    2015-01-01

    In order to analyze the light of cosmic objects, particularly at extremely great distances, spectroscopy is the workhorse of astronomy. In the era of very large telescopes, long-term investigations are mainly performed with small professional instruments. Today they can be done using self-designed spectrographs and highly efficient CCD cameras, without the need for large financial investments.   This book explains the basic principles of spectroscopy, including the fundamental optical constraints and all mathematical aspects needed to understand the working principles in detail. It covers the complete theoretical and practical design of standard and Echelle spectrographs. Readers are guided through all necessary calculations, enabling them to engage in spectrograph design. The book also examines data acquisition with CCD cameras and fiber optics, as well as the constraints of specific data reduction and possible sources of error. In closing it briefly highlights some main aspects of the research on massive s...

  19. How to unveil a T Tauri star

    International Nuclear Information System (INIS)

    Hartigan, P.; Hartmann, L.; Kenyon, S.; Hewett, R.; Stauffer, J.

    1989-01-01

    A method for separating the 'veiling' continuum often present in T Tauri stars from the underlying photospheric spectrum is described. Echelle observations from 5100 to 6800 A of the partially veiled T Tauri star BP Tau were analyzed to determine the shape of the veiling spectrum. The residuals of the fit indicate the deviation of the veiling spectrum from a simple continuum and identify the location and strength of any emission-line components. It is shown, by means of goodness-of-fit tests, that the spectrum of BP Tau can be decomposed into a normal stellar spectrum plus a smooth veiling continuum with only a few emission lines superposed. The continuum dominates the veiling spectrum in this spectral region; the veiling does not arise from numerous deep photospheric absorption lines that are filled in by weak emission. 36 refs

  20. PEPSI-feed: linking PEPSI to the Vatican Advanced Technology Telescope using a 450m long fibre

    Science.gov (United States)

    Sablowski, D. P.; Weber, M.; Woche, M.; Ilyin, I.; Järvinen, A.; Strassmeier, K. G.; Gabor, P.

    2016-07-01

    Limited observing time at large telescopes equipped with the most powerful spectrographs makes it almost impossible to gain long and well-sampled time-series observations. Ditto, high-time-resolution observations of bright targets with high signal-to-noise are rare. By pulling an optical fibre of 450m length from the Vatican Advanced Technology Telescope (VATT) to the Large Binocular Telescope (LBT) to connect the Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI) to the VATT, allows for ultra-high resolution time-series measurements of bright targets. This article presents the fibre-link in detail from the technical point-of-view, demonstrates its performance from first observations, and sketches current applications.

  1. Waveguide image-slicers for ultrahigh resolution spectroscopy

    Science.gov (United States)

    Beckert, Erik; Strassmeier, Klaus G.; Woche, Manfred; Eberhardt, Ramona; Tünnermann, Andreas; Andersen, Michael

    2008-07-01

    Waveguide image-slicer prototypes with resolutions up to 310.000 for the fiber fed PEPSI echelle spectrograph at the LBT and single waveguide thicknesses of down to 30 μm have been manufactured. The waveguides were macroscopically prepared, stacked up to an order of 7 and thinned back to square stack cross sections. A high filling ratio was achieved by realizing homogenous adhesive gaps of 4.6 μm, using index matching adhesives for TIR within the waveguides. The image-slicer stacks can be used in immersion mode and are miniaturized to be implemented in a set of four, measurements indicate an overall efficiency of above 80% for them.

  2. Multi-resolution waveguide image slicer for the PEPSI instrument

    Science.gov (United States)

    Beckert, Erik; Strassmeier, Klaus G.; Woche, Manfred; Harnisch, Gerd; Hornaff, Marcel; Weber, Michael; Barnes, Stuart

    2016-07-01

    A waveguide image slicer with resolutions up to 270.000 (planned: 300.000) for the fiber fed PEPSI echelle spectrograph at the LBT and single waveguide thicknesses of down to 70 μm has been manufactured and tested. The waveguides were macroscopically prepared, stacked up to an order of seven and thinned back to square stack cross sections. A high filling ratio was achieved by realizing homogenous adhesive gaps of 3.6 μm, using index matching adhesives for TIR within the waveguides. The image slicer stacks are used in immersion mode and are miniaturized to enable implementation in a set of 2x8. The overall efficiency is between 92 % and 96 %.

  3. Integration of a thermo-structural analysis with an optical model for PEPSI polarimeter

    Science.gov (United States)

    Di Varano, Igor; Strassmeier, Klaus G.; Ilyin, Ilya; Woche, Manfred; Kaercher, Hans J.

    2011-09-01

    The two spectropolarimeters for PEPSI (Potsdam Echelle Polarimetric and Spectroscopic Instrument) have been de¬signed in order to reconstruct the full Stokes vector measuring linear and circular polarization simultaneously with a re¬solving power of 120,000. The polarimeters will be attached to the Gregorian focus of the so far largest LBT 2x8.4m telescope and will feed together with permanent focus stations the spectrograph via 44m long fibers connection. The spectrograph will be located in a pressure-temperature controlled chamber within the telescope pier. We present hereafter the last results from combined structural and CFD analyses in order to fulfill the optical requirements.

  4. First operations of the SOIR occultation infrared spectrometer in Venus orbit.

    Science.gov (United States)

    Nevejans, D.; Neefs, E.; Vandaele, A. C.; Muller, C.; Fussen, D.; Berkenbosch, S.; Clairquin, R.; Korablev, O.; Federova, A.; Bertaux, J. L.

    Since May 2006, the Venus-Express spacecraft is in its nominal orbit around VENUS and the SPICAV optical package has begun to acquire spectra. The SOIR extension to SPICAV is an echelle spectrometer associated to an AOTF (Acousto-Optical Tunable Filter) for the order selection, which performs solar occultation measurements in the IR region (2.2-4.3 µm) at a resolution of 0.1 cm-1 . The detailed optical study and design as well as the manufacturing were performed at the BIRA/IASB in collaboration with its industrial partners OIP and PEDEO. It was funded by the Belgian Federal Science Policy Office under the ESA PRODEX programme. The wavelength range allows a detailed chemical inventory of the Venus atmosphere above the cloud layer with an emphasis on vertical distribution of gases. The first results look promising and will be qualitatively presented.

  5. VizieR Online Data Catalog: Elemental abundances of solar sibling candidates (Ramirez+, 2014)

    Science.gov (United States)

    Ramirez, I.; Bajkova, A. T.; Bobylev, V. V.; Roederer, I. U.; Lambert, D. L.; Endl, M.; Cochran, W. D.; MacQueen, P. J.; Wittenmyer, R. A.

    2017-06-01

    We used the Tull coude spectrograph on the 2.7 m Harlan J. Smith Telescope at McDonald Observatory (Tull et al. 1995PASP..107..251T) to observe most of our targets (23). All but three of them were observed in 2012 December; the others were observed in 2013 March. The rest of our targets (seven) have too-low declinations to be observed from McDonald Observatory. Instead, they were observed using the Magellan Inamori Kyocera Echelle (MIKE) spectrograph on the 6.5 m Telescope at Las Campanas Observatory (Bernstein et al. 2003SPIE.4841.1694B) in 2013 April. Slit sizes were chosen so that the spectral resolution of the data is about 60000 in the visible part of the spectrum. We targeted a S/N per pixel of at least 200 at 6000 Å. Only one of our targets (HD 46100) has a significantly lower S/N spectrum. (2 data files).

  6. The dynamics of Herbig-Haro objects HH46 and 47A and their remarkable connecting filament HH47B

    International Nuclear Information System (INIS)

    Meaburn, J.; Dyson, J.E.

    1987-01-01

    Echelle observations of the Hα and [S II] line profiles have been made with the Anglo-Australian Telescope along the emission-line filament (HH47B) which connects the Herbig-Haro objects HH46 and 47A. A red continuum source between HH46 and the 10μm peak has a +-200kms -1 wide Hα component centred on the rest velocity of the parent globule. Scattered radiation from an embedded T Tauri star is suggested. HH46 and 47A are receding away from the observer but the connecting filament exhibits some form of velocity ellipse. The bipolar configuration had been previously suggested by the discovery of the counter object HH47C with Vsub(HEL) = 100kms -1 . (author)

  7. Iron abundance in the hot DA white dwarfs Feige 24 and G191 B2B

    Science.gov (United States)

    Vennes, Stephane; Chayer, Pierre; Thorstensen, John R.; Bowyer, Stuart; Shipman, Harry L.

    1992-01-01

    Attention is given to model calculations of the far- and extreme-UV line spectra of highly ionized Fe species (Fe IV, Fe V, and Fe VI) for hot high-gravity H-rich stars. A spectral analysis of 31 hr of exposure of the DA white dwarf Feige 24 with IUE in the echelle mode reveals the presence of Fe with an abundance relative to H by number of (5-10) x 10 exp -6 with an uncertainty dominated by the determination of stellar parameters. An analysis of IUE data from the white dwarf G191 B2B results in a similar Fe abundance if this star shares similar atmospheric parameters (Teff, g) with Feige 24. Fe is thus the second most abundant photospheric element in hot DA white dwarfs.

  8. VizieR Online Data Catalog: Abundances of 8 RR Lyrae subclass C variable stars (Govea+, 2014)

    Science.gov (United States)

    Govea, J.; Gomez, T.; Preston, G. W.; Sneden, C.

    2016-02-01

    We chose 10 candidate RR Lyrae variable stars of subclass c (RRc) stars for spectroscopic observation. Many of these stars were first identified as RRc variables by the All Sky Automated Survey (ASAS) of Pojmanski 2003 (cat. II/264). The target star list included ASAS 144154-0324.7 and ASAS 204440-2402.7. But our spectroscopic study suggest that these two stars are probably W UMa binaries instead of RR Lyrae stars Our spectra were obtained with the echelle spectrograph of the du Pont 2.5m telescope at the Las Campanas Observatory. Four observing runs during 2009-2010 were partly devoted to this project. The spectrograph was used with the 1.5*4'' entrance slit, which translates to a resolving power of R=λ/Δλ~27000 at the MgI b lines near 5180Å. The total continuous wavelength coverage of the spectra was 3500-9000Å. (6 data files).

  9. Assessment of pain in children with cerebral palsy focused on translation and clinical feasibility of the revised FLACC score

    DEFF Research Database (Denmark)

    Pedersen, Line Kjeldgaard; Rahbek, Ole; Nikolajsen, Lone

    2015-01-01

    AbstractBackground and aims Assessment of pain in children with cognitive impairment (CI) including cerebral palsy (CP) is difficult. Several pain assessment tools have been developed and validated for use in children with CI. The revised Face, Legs, Activity, Cry and Consolability score (r......). Both the Noncommunicating Childrens's Pain Checklist – Postoperative version (NCCPC-PV) and the Echelle Douleur Enfant San Salvador (DESS) are developed from core pain behaviours for children with CI but have no possibility for individualisation. For successful clinical application a pain assessment......-FLACC) includes core behaviours of children with CI and adds an open-ended descriptor for individualisation (5 items assigned 0–2 points, total range 0–10). Other pain assessment tools including individual pain behaviours are the Individualised Numeric Rating Scale (INRS) and the Paediatric Pain Profile (PPP...

  10. The Wolf-Rayet nebula NGC 6888 as a pressure driven bubble

    International Nuclear Information System (INIS)

    Marston, A.P.; Meaburn, J.

    1988-01-01

    Profiles of the Hα and [NII] emission lines have been obtained across the major axis of the Wolf-Rayet ring nebula NGC6888 with the Manchester echelle spectrometer combined with the Isaac Newton Telescope. Although triple profiles are found, this nebula is shown to approximate to a shell of radius 3pc expanding at 85 km s -1 . The ionized mass in the shell is 3.5 ± 1.2 M solar masses . IRAS survey maps also reveal a shell of neutral material containing 40 M solar masses , assuming the far infrared continuum emission from warm dust dominates the line emission. If it is assumed that this mass is also expanding at 85 km s -1 it is shown that the nebula is a pressure driven bubble, which conserves the kinetic energy of the driving stellar wind. (author)

  11. Effect of water vapour absorption on hydroxyl temperatures measured from Svalbard

    Directory of Open Access Journals (Sweden)

    J. M. Chadney

    2017-03-01

    Full Text Available We model absorption by atmospheric water vapour of hydroxyl airglow emission using the HIgh-resolution TRANsmission molecular absorption database (HITRAN2012. Transmission coefficients are provided as a function of water vapour column density for the strongest OH Meinel emission lines in the (8–3, (5–1, (9–4, (8–4, and (6–2 vibrational bands. These coefficients are used to determine precise OH(8–3 rotational temperatures from spectra measured by the High Throughput Imaging Echelle Spectrograph (HiTIES, installed at the Kjell Henriksen Observatory (KHO, Svalbard. The method described in this paper also allows us to estimate atmospheric water vapour content using the HiTIES instrument.

  12. Correcting groove error in gratings ruled on a 500-mm ruling engine using interferometric control.

    Science.gov (United States)

    Mi, Xiaotao; Yu, Haili; Yu, Hongzhu; Zhang, Shanwen; Li, Xiaotian; Yao, Xuefeng; Qi, Xiangdong; Bayinhedhig; Wan, Qiuhua

    2017-07-20

    Groove error is one of the most important factors affecting grating quality and spectral performance. To reduce groove error, we propose a new ruling-tool carriage system based on aerostatic guideways. We design a new blank carriage system with double piezoelectric actuators. We also propose a completely closed-loop servo-control system with a new optical measurement system that can control the position of the diamond relative to the blank. To evaluate our proposed methods, we produced several gratings, including an echelle grating with 79  grooves/mm, a grating with 768  grooves/mm, and a high-density grating with 6000  grooves/mm. The results show that our methods effectively reduce groove error in ruled gratings.

  13. VizieR Online Data Catalog: HeI 5876 & 10830Å EWs of solar-type stars (Andretta+, 2017)

    Science.gov (United States)

    Andretta, V.; Giampapa, M. S.; Covino, E.; Reiners, A.; Beeck, B.

    2017-11-01

    A total of 134 FEROS spectra (R=48000) of our targets (including telluric standards) were acquired on the night of UT 2011 December 6-7; spectral coverage from 3500 to 9200Å. The Fiber Extended-range Optical Spectrograph (FEROS) was mounted at the 2.2m Max-Planck Gesellschaft/European Southern Observatory (MPG/ESO) telescope at La Silla (Chile). The HeIλ10830 spectroscopic observations were carried out on the same night as the FEROS D3 observations, using the CRyogenic high-resolution InfraRed Echelle Spectrograph (CRIRES), mounted at Unit Telescope 1 (Antu) of the VLT array at Cerro Paranal. The details of the observations is given in table 1. (3 data files).

  14. The electroreduction of pentavalent protactinium; Reduction electrolytique du protactinium pentavalent

    Energy Technology Data Exchange (ETDEWEB)

    Musikas, C [Commissariat a l' Energie Atomique, Centre d' Etudes Nucleaires de Fontenay-aux-Roses, 92 (France)

    1966-05-01

    The reduction of pentavalent protactinium to tetravalent protactinium, in sulfuric and hydrochloric media, on a milligram scale was demonstrated by electrolysis in a separate-compartment cell. There was no indication that protactinium may exist at the trivalent state in these solutions. Polarograms in fluoride solutions showed only one reduction wave. The principle of a volumetric method for the titration of protactinium is given. (author) [French] La reduction du protactinium pentavalent en protactinium tetravalent, dans des solutions sulfuriques et chlorhydriques a ete realisee a l'echelle du milligramme, par electrolyse, dans une cellule a compartiments separes. Aucun indice ne permet de penser que le protactinium puisse exister dans ces solutions a l'etat trivalent. De plus les polarogrammes traces en milieu fluorhydrique ne font apparaitre qu'une seule vague de reduction. Le principe d'une methode volumetrique de dosage du protactinium est donne. (auteur)

  15. PROJECTED ROTATIONAL VELOCITIES OF 136 EARLY B-TYPE STARS IN THE OUTER GALACTIC DISK

    Energy Technology Data Exchange (ETDEWEB)

    Garmany, C. D.; Glaspey, J. W. [National Optical Astronomy Observatory, 950 N. Cherry Ave., Tucson, AZ 85719 (United States); Bragança, G. A.; Daflon, S.; Fernandes, M. Borges; Cunha, K. [Observatório Nacional-MCTI, Rua José Cristino, 77. CEP: 20921-400, Rio de Janeiro, RJ (Brazil); Oey, M. S. [University of Michigan, Department of Astronomy, 311 West Hall, 1085 S. University Ave., Ann Arbor, MI: 48109-1107 (United States); Bensby, T., E-mail: garmany@noao.edu [Lund Observatory, Department of Astronomy and Theoretical Physics, Box 43, SE-22100, Lund (Sweden)

    2015-08-15

    We have determined projected rotational velocities, v sin i, from Magellan/MIKE echelle spectra for a sample of 136 early B-type stars having large Galactocentric distances. The target selection was done independently of their possible membership in clusters, associations or field stars. We subsequently examined the literature and assigned each star as Field, Association, or Cluster. Our v sin i results are consistent with a difference in aggregate v sin i with stellar density. We fit bimodal Maxwellian distributions to the Field, Association, and Cluster subsamples representing sharp-lined and broad-lined components. The first two distributions, in particular, for the Field and Association are consistent with strong bimodality in v sin i. Radial velocities are also presented, which are useful for further studies of binarity in B-type stars, and we also identify a sample of possible new double-lined spectroscopic binaries. In addition, we find 18 candidate Be stars showing emission at Hα.

  16. VizieR Online Data Catalog: Spectral atlas of HD 50138 (Borges Fernandes+, 2009)

    Science.gov (United States)

    Borges Fernandes, M.; Kraus, M.; Chesneau, O.; Domiciano de Souza, A.; de Araujo, F. X.; Stee, P.; Meilland, A.

    2009-09-01

    In this table, it is described the lines identified, with their radial velocities and equivalent widths in the high-resolution FEROS spectra obtained in 1999 and 2007. FEROS is a bench-mounted Echelle spectrograph with fibers, which covers a sky area of 2" of diameter, with a wavelength coverage from 360nm to 920nm and a spectral resolution of R=55000 (in the region around 600nm). The spectrum of 1999 was obtained with an exposure time of 180 seconds and has a S/N ratio of approximately 80 in the 550nm region. In 2007, we were able to take two consecutive spectra of the star, both with 180 seconds of exposure time. Since these spectra do not show significant differences, we added them up for a better S/N ratio, which is around 250. (1 data file).

  17. VizieR Online Data Catalog: Abundance of nine beta Cephei stars (Morel+, 2006)

    Science.gov (United States)

    Morel, T.; Butler, K.; Aerts, C.; Neiner, C.; Briquet, M.

    2006-07-01

    The equivalent widths (EWs) were measured on high-resolution spectra obtained with various echelle spectrographs (see Table 2 of paper for further details). Our EWs are systematically larger than the values quoted by Gies & Lambert (1992ApJ...387..673G) for the seven stars in common, but a similar trend is evident when comparing their values with previous measurements in the literature (see their Fig.4). This is likely to result from their use of Gaussian fitting instead of the direct integration used in our case. The same conclusion holds for the EWs of xi1 CMa presented by Hambly et al. (1996MNRAS.278..811H). (1 data file).

  18. RR LYRAE ATMOSPHERICS: WRINKLES OLD AND NEW. A PREVIEW

    International Nuclear Information System (INIS)

    Preston, George W.

    2011-01-01

    I report some results of an echelle spectroscopic survey of RR Lyrae stars begun in 2006 that I presented in my Henry Norris Lecture of 2010 January 4. Topics include (1) atmospheric velocity gradients, (2) phase-dependent envelope turbulence as it relates to Peterson's discoveries of axial rotation on the horizontal branch and to Stothers' explanation of the Blazhko effect, (3) the three apparitions of hydrogen emission during a pulsation cycle, (4) the occurrence of He I lines in emission and absorption, (5) detection of He II emission and metallic line doubling in Blazhko stars, and finally (6) speculation about what helium observations of RR Lyrae stars in omega Centauri might tell us about the putative helium populations and the horizontal branch of that strange globular cluster.

  19. Neutron-Capture Element Abundances in the Globular Cluster M15.

    Science.gov (United States)

    Sneden; Johnson; Kraft; Smith; Cowan; Bolte

    2000-06-20

    High-resolution, high signal-to-noise ratio, blue-violet spectra of three red giant branch tip stars in M15 have been obtained with the Keck I High-Resolution Echelle Spectrograph. These spectra have been analyzed to determine the abundances of several neutron-capture elements, including the radioactive chronometer element thorium. There are two principal results of this study. First, the abundances of the heavier (Z>/=56) elements for each of the three stars is well matched by a scaled solar system r-process abundance distribution. Second, a weighted mean-observed Th/Eu ratio for the stars implies an age for the neutron-capture material in M15 stars of 14+/-3 Gyr, in reasonable agreement with other recent age estimates for Galactic globular clusters.

  20. Analysis of LiSn alloy at several depths using LIBS

    Energy Technology Data Exchange (ETDEWEB)

    Suchoňová, M., E-mail: maria.suchonova@fmph.uniba.sk [Dept. of Experimental Physics, Faculty of Mathematics Physics and Informatics, Comenius University in Bratislava, Mlynská dolina F2, 842 48 Bratislava (Slovakia); Krištof, J.; Pribula, M. [Dept. of Experimental Physics, Faculty of Mathematics Physics and Informatics, Comenius University in Bratislava, Mlynská dolina F2, 842 48 Bratislava (Slovakia); Veis, M. [Dept. of Inorganic Chemistry, Faculty of Natural Science, Comenius University, Mlynská dolina, Ilkovičova 6, 842 15 Bratislava 4 (Slovakia); Tabarés, F.L. [Fusion Department, Ciemat, Av Complutense 40, 28040 Madrid (Spain); Veis, P., E-mail: pavel.veis@fmph.uniba.sk [Dept. of Experimental Physics, Faculty of Mathematics Physics and Informatics, Comenius University in Bratislava, Mlynská dolina F2, 842 48 Bratislava (Slovakia)

    2017-04-15

    The difference between the composition of the surface and the inner part of the LiSn sample was studied using Calibration Free Laser Induced Breakdown Spectroscopy (CF-LIBS) method. The sample was analysed under the low pressure (1330 Pa) in Ar atmosphere. The spectra were record using Echelle spectrometer (Mechelle ME5000). Gate delay and gate width was optimised and set to 300 ns. In order to analyse depth profile the LIBS spectra was recorded after each laser shot. The electron density analysed by laser induced plasma was determined separately for each laser shot, which means for each ablated layer of investigated sample. The difference between the individual shots taken at distinct sites of the sample are shown. The CF-LIBS method was used to determine the elemental composition near the surface and in the central part of the LiSn sample.

  1. EG ANDROMEDAE: A NEW ORBIT AND ADDITIONAL EVIDENCE FOR A PHOTOIONIZED WIND

    International Nuclear Information System (INIS)

    Kenyon, Scott J.; Garcia, Michael R.

    2016-01-01

    We analyze a roughly 20 yr set of spectroscopic observations for the symbiotic binary EG And. Radial velocities derived from echelle spectra are best fit with a circular orbit having an orbital period of P = 483.3 ± 1.6 days and semi-amplitude K = 7.34 ± 0.07 km s −1 . Combined with previous data, these observations rule out an elliptical orbit at the 10 σ level. Equivalent widths of H i Balmer emission lines and various absorption features vary in phase with the orbital period. Relative to the radius of the red giant primary, the apparent size of the H ii region is consistent with a model where a hot secondary star with effective temperature T h ≈ 75,000 K ionizes the wind from the red giant.

  2. Optical design for CETUS: a wide-field 1.5m aperture UV payload being studied for a NASA probe class mission study

    Science.gov (United States)

    Woodruff, Robert; Robert Woodruff, Goddard Space Flight Center, Kendrick Optical Consulting

    2018-01-01

    We are developing a NASA Headquarters selected Probe-class mission concept called the Cosmic Evolution Through UV Spectroscopy (CETUS) mission, which includes a 1.5-m aperture diameter large field-of-view (FOV) telescope optimized for UV imaging, multi-object spectroscopy, and point-source spectroscopy. The optical system includes a Three Mirror Anastigmatic (TMA) telescope that simultaneously feeds three separate scientific instruments: the near-UV (NUV) Multi-Object Spectrograph (MOS) with a next-generation Micro-Shutter Array (MSA); the two-channel camera covering the far-UV (FUV) and NUV spectrum; and the point-source spectrograph covering the FUV and NUV region with selectable R~ 40,000 echelle modes and R~ 2,000 first order modes. The optical system includes fine guidance sensors, wavefront sensing, and spectral and flat-field in-flight calibration sources. This paper will describe the current optical design of CETUS.

  3. Qui sera le nouvel Einstein ? Vers une nouvelle theorie de la gravitation

    Science.gov (United States)

    Bonnet-Bidaud, J. M.

    1999-10-01

    Un debat de plus d'un siecle a resurgi ces toutes dernieres annees avec une vigueur nouvelle. L'enjeu ? Mettre fin, ni plus ni moins, a l'une des contradictions les plus inouies de la physique fondamentale, en reconciliant mecanique quantique et relativite generale. En effet, a l'heure ou la gravitation semble enfin sur le point de fusionner avec les trois autres forces de la nature. il est certain que la relativite d'Einstein doit etre bientot remplacer par une autre theorie... Reste quye tous les physiciens sont loin de s'accorder sur la marche a suivree. Gravitation quantique, relativite d'echelle, supersymetrie, les candidates ne manquent pas.

  4. Evaluation of laser induced breakdown spectroscopy for the determination of macronutrients in plant materials

    Energy Technology Data Exchange (ETDEWEB)

    Trevizan, Lilian Cristina [Centro de Energia Nuclear na Agricultura, Universidade de Sao Paulo, Av. Centenario 303, 13416-000, Piracicaba-SP (Brazil)], E-mail: lilian@conectcor.com.br; Santos, Dario [Universidade Federal de Sao Paulo - UNIFESP, Rua Prof. Artur Riedel 275, 09972-270, Diadema-SP (Brazil); Elgul Samad, Ricardo; Dias Vieira, Nilson [Centro de Lasers e Aplicacoes, IPEN/CNEN-SP, Av. Prof. Lineu Prestes 2242, 05508-000, Sao Paulo-SP (Brazil); Seimi Nomura, Cassiana [Centro de Ciencias Naturais e Humanas, Universidade Federal do ABC, Rua Santa Adelia 166, 09210-170, Santo Andre-SP (Brazil); Nunes, Lidiane Cristina [Departamento de Quimica, Universidade Federal de Sao Carlos, Rod. Washington Luis, km 235, 13565-905, Sao Carlos-SP (Brazil); Rufini, Iolanda Aparecida; Krug, Francisco Jose [Centro de Energia Nuclear na Agricultura, Universidade de Sao Paulo, Av. Centenario 303, 13416-000, Piracicaba-SP (Brazil)

    2008-10-15

    Laser induced breakdown spectroscopy (LIBS) has become an analytical tool for the direct analysis of a large variety of materials in order to provide qualitative and/or quantitative information. However, there is a lack of information for LIBS analysis of agricultural and environmental samples. In this work a LIBS system has been evaluated for the determination of macronutrients (P, K, Ca, Mg) in pellets of vegetal reference materials. An experimental setup was designed by using a Nd:YAG laser operating at 1064 nm and an Echelle spectrometer with ICCD detector. The plasma temperature was estimated by Boltzmann plots and instrumental parameters such as delay time, lens-to-sample distance and pulse energy were evaluated. Certified reference materials as well as reference materials were used for analytical calibrations of P, K, Ca, and Mg. Most results of the direct analysis of plant samples by LIBS were in reasonable agreement with those obtained by ICP OES after wet acid decomposition.

  5. Evaluation of laser induced breakdown spectroscopy for the determination of macronutrients in plant materials

    International Nuclear Information System (INIS)

    Trevizan, Lilian Cristina; Santos, Dario; Elgul Samad, Ricardo; Dias Vieira, Nilson; Seimi Nomura, Cassiana; Nunes, Lidiane Cristina; Rufini, Iolanda Aparecida; Krug, Francisco Jose

    2008-01-01

    Laser induced breakdown spectroscopy (LIBS) has become an analytical tool for the direct analysis of a large variety of materials in order to provide qualitative and/or quantitative information. However, there is a lack of information for LIBS analysis of agricultural and environmental samples. In this work a LIBS system has been evaluated for the determination of macronutrients (P, K, Ca, Mg) in pellets of vegetal reference materials. An experimental setup was designed by using a Nd:YAG laser operating at 1064 nm and an Echelle spectrometer with ICCD detector. The plasma temperature was estimated by Boltzmann plots and instrumental parameters such as delay time, lens-to-sample distance and pulse energy were evaluated. Certified reference materials as well as reference materials were used for analytical calibrations of P, K, Ca, and Mg. Most results of the direct analysis of plant samples by LIBS were in reasonable agreement with those obtained by ICP OES after wet acid decomposition

  6. Contribution to the study of the sintering of uranium oxide; Contribution a l'etude du frittage de l'oxyde d'uranium

    Energy Technology Data Exchange (ETDEWEB)

    Bel, A; Carteret, Y [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1958-07-01

    The sintering ofnium oxide has been considered and the following factors have been particularly taken in consideration: - the particle size and the particles in shape of the initial powder, - the specific area of the initial powder, - the chemical composition of the oxide, - and the medium in which the sintering was carried out. A method of sintering uranium oxide on semi-industrial scale is presented. (author)Fren. [French] On xamine l'influence de differents facteurs sur le frittage de l'oxyde d'uranium. Sont particulierement prises en consideration: - la taille et la forme des grains de la poudre initiale, - la surface specifique de la poudre initiale, - la composition chimique de l'oxyde, - ainsi que la nature de l'atmosphere durant le frittage. D'autre part, une technique de frittage de l'oxyde d'uranium a l'echelle semi-industrielle est presentee. (auteur)

  7. Thirty Years, One Million Spectra: Public Access to the SAO Spectral Archives

    Science.gov (United States)

    Mink, J.; Moran, S.

    2015-09-01

    Over the last 30 years, the SAO Telescope Data Center has reduced and archived over 1,000,000 spectra, consisting of 287,000 spectra from five high dispersion Echelle spectrographs and 717,000 spectra from four low dispersion spectrographs, across three telescopes. 151,000 spectra from six instruments are currently online and publicly available, covering many interesting objects in the northern sky, including most of the galaxies in the Updated Zwicky Catalog which are reachable through NED or Simbad. A majority of the high dispersion spectra will soon be made public, as will more data from the MMT multi-fiber spectrographs. Many objects in the archive have multiple spectra over time, which make them a valuable resource for archival time-domain studies. We are now developing a system to make all of the public spectra more easily searchable and viewable through the Virtual Observatory.

  8. Improving IUE High Dispersion Extraction

    Science.gov (United States)

    Lawton, Patricia J.; VanSteenberg, M. E.; Massa, D.

    2007-01-01

    We present a different method to extract high dispersion International Ultraviolet Explorer (IUE) spectra from the New Spectral Image Processing System (NEWSIPS) geometrically and photometrically corrected (SI HI) images of the echellogram. The new algorithm corrects many of the deficiencies that exist in the NEWSIPS high dispersion (SIHI) spectra . Specifically, it does a much better job of accounting for the overlap of the higher echelle orders, it eliminates a significant time dependency in the extracted spectra (which can be traced to the background model used in the NEWSIPS extractions), and it can extract spectra from echellogram images that are more highly distorted than the NEWSIPS extraction routines can handle. Together, these improvements yield a set of IUE high dispersion spectra whose scientific integrity is sign ificantly better than the NEWSIPS products. This work has been supported by NASA ADP grants.

  9. The STELLA Robotic Observatory on Tenerife

    Directory of Open Access Journals (Sweden)

    Klaus G. Strassmeier

    2010-01-01

    Full Text Available The Astrophysical Institute Potsdam (AIP and the Instituto de Astrofísica de Canarias (IAC inaugurated the robotic telescopes STELLA-I and STELLA-II (STELLar Activity on Tenerife on May 18, 2006. The observatory is located on the Izaña ridge at an elevation of 2400 m near the German Vacuum Tower Telescope. STELLA consists of two 1.2 m alt-az telescopes. One telescope fiber feeds a bench-mounted high-resolution echelle spectrograph while the other telescope feeds a wide-field imaging photometer. Both scopes work autonomously by means of artificial intelligence. Not only that the telescopes are automated, but the entire observatory operates like a robot, and does not require any human presence on site.

  10. EG ANDROMEDAE: A NEW ORBIT AND ADDITIONAL EVIDENCE FOR A PHOTOIONIZED WIND

    Energy Technology Data Exchange (ETDEWEB)

    Kenyon, Scott J. [Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 (United States); Garcia, Michael R., E-mail: skenyon@cfa.harvard.edu, E-mail: michael.r.garcia@nasa.gov [NASA Headquarters, Mail Suite 3Y28, 300 E Street SW, Washington, DC 20546-0001 (United States)

    2016-07-01

    We analyze a roughly 20 yr set of spectroscopic observations for the symbiotic binary EG And. Radial velocities derived from echelle spectra are best fit with a circular orbit having an orbital period of P = 483.3 ± 1.6 days and semi-amplitude K = 7.34 ± 0.07 km s{sup −1}. Combined with previous data, these observations rule out an elliptical orbit at the 10 σ level. Equivalent widths of H i Balmer emission lines and various absorption features vary in phase with the orbital period. Relative to the radius of the red giant primary, the apparent size of the H ii region is consistent with a model where a hot secondary star with effective temperature T{sub h} ≈ 75,000 K ionizes the wind from the red giant.

  11. Rotation and chromospheric emission among F, G, and K dwarfs of the Pleiades

    Science.gov (United States)

    Soderblom, David R.; Stauffer, John R.; Hudon, J. D.; Jones, Burton F.

    1993-01-01

    High-resolution echelle spectra of more than 100 F, G, and K dwarfs in the Pleiades are reported. Chromospheric activity in these stars is measured via comparisons of the profiles of H-alpha and the Ca II IR triplet to chromospherically inactive field stars. Consistent dereddened colors are determined from the available photometry and temperatures are derived. Most G and K dwarfs in the Pleiades rotate slowly, but about 20 percent of the stars are ultrafast rotators (UFRs). That fraction of UFRs is independent of color, and the highest rotation rates are found among the K dwarfs. The Pleiades exhibit a broad range in the strength of chromospheric emission at any one color. Most G and K dwarfs in the Pleiades show H-alpha and the IR triple in absorption, with filling in of the line cores.

  12. EG Andromedae: A New Orbit and Additional Evidence for a Photoionized Wind

    Science.gov (United States)

    Kenyon, Scott J.; Garcia, Michael R.

    2016-07-01

    We analyze a roughly 20 yr set of spectroscopic observations for the symbiotic binary EG And. Radial velocities derived from echelle spectra are best fit with a circular orbit having an orbital period of P = 483.3 ± 1.6 days and semi-amplitude K = 7.34 ± 0.07 km s-1. Combined with previous data, these observations rule out an elliptical orbit at the 10σ level. Equivalent widths of H I Balmer emission lines and various absorption features vary in phase with the orbital period. Relative to the radius of the red giant primary, the apparent size of the H II region is consistent with a model where a hot secondary star with effective temperature T h ≈ 75,000 K ionizes the wind from the red giant.

  13. Relation between radius and expansion velocity in planetary nebulae

    International Nuclear Information System (INIS)

    Chu, Y.H.; Kwitter, K.B.; Kaler, J.B.

    1984-01-01

    The expansion velocity-radius (R-V) relation for planetary nebulae is examined using the existing measurements of expansion velocities and recent calculations of radii. It is found that some of the previously alleged R-V relations for PN are not convincingly established. The scatter in the R-V plots may be due largely to stratification of ions in individual nebulae and to heterogeneity in the planetary nebula population. In addition, from new echelle/CCD observations of planetary nebulae, it is found that spatial information is essential in deriving the internal kinematic properties. Future investigations of R-V relations should be pursued separately for groups of planetaries with similar physical properties, and they should employ observations of appropriate low excitation lines in order to measure the expansion velocity at the surface of the nebula. 26 references

  14. Some aspects of ICP-AES analysis of high purity rare earths

    International Nuclear Information System (INIS)

    Murty, P.S.; Biswas, S.S.

    1991-01-01

    Inductively coupled plasma atomic emission spectrometry (ICP-AES) is a technique capable of giving high sensitivity in trace elemental analysis. While the technique possesses high sensitivity, it lacks high selectivity. Selectivity is important where substances emitting complex spectra are to be analysed for trace elements. Rare earths emit highly complex spectra in a plasma source and the determination of adjacent rare earths in a high purity rare earth matrix, with high sensitivity, is not possible due to the inadequate selectivity of ICP-AES. One approach that has yielded reasonably good spectral selectivity in the high purity rare earth analysis by ICP-AES is by employing a combination of wavelength modulation techniques and high resolution echelle grating. However, it was found that by using a high resolution monochromator senstitivities either comparable to or better than those reported by the wavelength modulation technique could be obtained. (author). 2 refs., 2 figs., 2 tabs

  15. Primordial lithium abundance from interstellar lithium lines towards SN 1987A

    International Nuclear Information System (INIS)

    Sahu, K.C.; Pottasch, S.R.; Sahu, M.

    1989-01-01

    The primoridal lithium abundance is known to be one of the best probes to test the standard as well as the non-standard Big Bang nucleosynthesis theories, and to measure the nucleon abundance in the early universe in the standard Big Bang (SSB) model. We have obtained high-resolution ((λ)/(δλ)congruent 100,000), high signal-to-noise (S/N approx-gt 1,500) spectra of SN 1987A around the Li:I λ6708 A region, using the ESO 1.4m CAT and the Coude Echelle Spectrograph. The non-detection of any lithium feature in our sepctra places an upper limit on the lithium abundance

  16. [CII] At 1 Universe with Zeus (1 and 2)

    Science.gov (United States)

    Ferkinhoff, Carl; Hailey-Dunsheath, S.; Nikola, T.; Oberst, T.; Parshley, S.; Stacey, G.; Benford, D.; staguhn, J.

    2010-01-01

    We report the detection of the [CII] 158 micron fine structure line from six submillimeter galaxies with redshifts between 1.12 and 1.73. This more than doubles the total number of [CII] 158 micron detections reported from high redshift sources. These observations were made with the Redshift(z) and Early Universe Spectrometer(ZEUS) at the Caltech Submillimeter Observatory on Mauna Kea, Hawaii between December 2006 and March 2009. ZEUS is a background limited submm echelle grating spectrometer (Hailey-Dunsheath 2009). Currently we are constructing ZEUS-2. This new instrument will utilize the same grating but will feature a two dimensional transition-edge sensed bolometer array with SQUID multiplexing readout system enabling simultaneous background limited observations in the 200, 340,450 and 650 micron telluric windows. ZEUS-2 will allow for long slit imaging spectroscopy in nearby galaxies and a [CII] survey from z 0.25 to 2.5.

  17. VizieR Online Data Catalog: Orphan stream high-resolution spectroscopic study (Casey+, 2014)

    Science.gov (United States)

    Casey, A. R.; Keller, S. C.; da Costa, G.; Frebel, A.; Maunder, E.

    2017-06-01

    High-resolution spectra for five Orphan stream candidates and seven well-studied standard stars have been obtained with the Magellan Inamori Kyocera Echelle spectrograph (Bernstein et al. 2003SPIE.4841.1694B) on the Magellan Clay telescope. These objects were observed in 2011 March using a 1" wide slit in mean seeing of 0.9". This slit configuration provides continuous spectral coverage from 333 nm to 915 nm, with a spectral resolution of R=25000 in the blue arm and R=28000 in the red arm. A minimum of 10 exposures of each calibration type (biases, flat fields, and diffuse flats) were observed in the afternoon of each day, with additional flat-field and Th-Ar arc lamp exposures performed throughout the night to ensure an accurate wavelength calibration. (3 data files).

  18. 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)

  19. Lithium in old open clusters - NGC 188

    International Nuclear Information System (INIS)

    Hobbs, L.M.; Pilachowski, C.

    1988-01-01

    Echelle spectra which include the Li I line at 6707 A are reported for seven main-sequence stars and one subgiant in NGC 188. The Li I line is detected in five of the six dwarfs which are highly probable cluster members. The derived atmospheric Li/H ratios exceed the solar value by factors ranging approximately from 10 to 40, although these apparently closely solarlike stars are about twice as old as the sun. The variation of the lithium abundance with stellar mass along the main sequences of the Pleiades, the Hyades, NGC 752, and NGC 188 are compared. The resulting evolutionary pattern indicates that the lithium fraction in the Galactic gas has shown no appreciable change from Li/H of roughly 10 to the -9th since the birth of NGC 188 about 10 Gyr ago, except that the abundance could have been higher by an uncertain but possibly appreciable factor at the beginning of that epoch. 51 references

  20. Second generation spectrograph for the Hubble Space Telescope

    Science.gov (United States)

    Woodgate, B. E.; Boggess, A.; Gull, T. R.; Heap, S. R.; Krueger, V. L.; Maran, S. P.; Melcher, R. W.; Rebar, F. J.; Vitagliano, H. D.; Green, R. F.; Wolff, S. C.; Hutchings, J. B.; Jenkins, E. B.; Linsky, J. L.; Moos, H. W.; Roesler, F.; Shine, R. A.; Timothy, J. G.; Weistrop, D. E.; Bottema, M.; Meyer, W.

    1986-01-01

    The preliminary design for the Space Telescope Imaging Spectrograph (STIS), which has been selected by NASA for definition study for future flight as a second-generation instrument on the Hubble Space Telescope (HST), is presented. STIS is a two-dimensional spectrograph that will operate from 1050 A to 11,000 A at the limiting HST resolution of 0.05 arcsec FWHM, with spectral resolutions of 100, 1200, 20,000, and 100,000 and a maximum field-of-view of 50 x 50 arcsec. Its basic operating modes include echelle model, long slit mode, slitless spectrograph mode, coronographic spectroscopy, photon time-tagging, and direct imaging. Research objectives are active galactic nuclei, the intergalactic medium, global properties of galaxies, the origin of stellar systems, stelalr spectral variability, and spectrographic mapping of solar system processes.

  1. Introducing Research Methods to Undergraduate Majors Through an On-Campus Observatory with The University of Toledo's Ritter Observatory

    Science.gov (United States)

    Richardson, Noel; Hardegree-Ullman, Kevin; Bjorkman, Jon Eric; Bjorkman, Karen S.; Ritter Observing Team

    2017-01-01

    With a 1-m telescope on the University of Toledo (OH) main campus, we have initiated a grad student-undergraduate partnership to help teach the undergraduates observational methods and introduce them to research through peer mentorship. For the last 3 years, we have trained up to 21 undergraduates (primarily physics/astronomy majors) in a given academic semester, ranging from freshman to seniors. Various projects are currently being conducted by undergraduate students with guidance from graduate student mentors, including constructing three-color images, observations of transiting exoplanets, and determination of binary star orbits from echelle spectra. This academic year we initiated a large group research project to help students learn about the databases, journal repositories, and online observing tools astronomers use for day-to-day research. We discuss early inclusion in observational astronomy and research of these students and the impact it has on departmental retention, undergraduate involvement, and academic success.

  2. Nebular and auroral emission lines of [Cl III] in the optical spectra of planetary nebulae.

    Science.gov (United States)

    Keenan, F P; Aller, L H; Ramsbottom, C A; Bell, K L; Crawford, F L; Hyung, S

    2000-04-25

    Electron impact excitation rates in Cl III, recently determined with the R-matrix code, are used to calculate electron temperature (T(e)) and density (N(e)) emission line ratios involving both the nebular (5517.7, 5537.9 A) and auroral (8433.9, 8480.9, 8500.0 A) transitions. A comparison of these results with observational data for a sample of planetary nebulae, obtained with the Hamilton Echelle Spectrograph on the 3-m Shane Telescope, reveals that the R(1) = I(5518 A)/I(5538 A) intensity ratio provides estimates of N(e) in excellent agreement with the values derived from other line ratios in the echelle spectra. This agreement indicates that R(1) is a reliable density diagnostic for planetary nebulae, and it also provides observational support for the accuracy of the atomic data adopted in the line ratio calculations. However the [Cl iii] 8433.9 A line is found to be frequently blended with a weak telluric emission feature, although in those instances when the [Cl iii] intensity may be reliably measured, it provides accurate determinations of T(e) when ratioed against the sum of the 5518 and 5538 A line fluxes. Similarly, the 8500.0 A line, previously believed to be free of contamination by the Earth's atmosphere, is also shown to be generally blended with a weak telluric emission feature. The [Cl iii] transition at 8480.9 A is found to be blended with the He i 8480.7 A line, except in planetary nebulae that show a relatively weak He i spectrum, where it also provides reliable estimates of T(e) when ratioed against the nebular lines. Finally, the diagnostic potential of the near-UV [Cl iii] lines at 3344 and 3354 A is briefly discussed.

  3. Elementary operations on histograms - translation - contraction - expansion; Operations elementaires sur histogrammes translation, contraction, dilatation

    Energy Technology Data Exchange (ETDEWEB)

    Becker, A [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1968-07-01

    A simple model is proposed for describing the working of analyzer systems which carry out successively the transformations from a physical system to its analogue expression, and then finally to a numerical scale. The model leads to a process for determining the physical zero in which, intentionally, only instrumental adjustments of immediate access are made to intervene. When it is possible to consider that the indispensable knowledge of the correspondence between the physical origin and the numerical scale has been acquired, one can correct by numerical treatment the possible deformations, which affect the recorded distributions in spite of the use of electronic stabilizing systems. With this in view, a programme of very general structure has been written which makes it possible to carry out simple operations of the translation type and homothetic transformations with constant area; the major part of is this report is devoted to a description of this programme and to its expression in MAGE II and FORTRAN IV. (author) [French] Pour la description du fonctionnement des systemes analyseurs realisant successivement les transformations faisant passer d'un systeme physique a son expression analogique, puis enfin, a une echelle numerique, on propose un modele simple. Ce dernier conduit a un procede de determination de zero physique, dans lequel, c'est a dessein, que l'on ne fait intervenir que des reglages instrumentaux d'acces immediat. Lorsque l'indispensable connaissance de la correspondance entre l'origine physique et l'echelle numerique peut etre consideree comme acquise, les eventuelles deformations qui, malgre l'utilisation de systemes stabilisateurs electroniques, affectent les distributions enregistrees peuvent etre corrigees par des traitements numeriques. Dans ce dernier but, il a ete ecrit un programme de structure tres generale, capable d'effectuer des operations simples du type translation et homotheties avec conservation d'aires; sa description et son

  4. Quantitative analysis of manganese concentration in manganese-doped glasses by laser-induced breakdown spectroscopy using a nanosecond ultraviolet Nd:YAG laser

    International Nuclear Information System (INIS)

    Unnikrishnan, V.K.; Nayak, Rajesh; Kartha, V.B.; Santhosh, C.; Sonavane, M.S.; Yeotikar, R.G.; Gupta, G.P.; Suri, B.M.

    2012-01-01

    Laser-induced breakdown spectroscopy (LIBS) has been well recognized as a simple, fast and direct analytical technique for the analysis of elemental analysis of multi-element materials by a number of research groups all over the world. It is based on the focusing of a high-power pulsed laser beam with a power density > 100 MW/cm 2 onto a sample surface followed by optical emission spectroscopy of the plasma produced over the surface. During the last two decades, LIBS has attracted a lot of attention, leading to an ever increasing list of applications, both in laboratory and in industry. In this work, the quantitative analysis of manganese in manganese-doped glass samples in air at atmospheric pressure has been carried out by the LIBS system assembled and optimized in the laboratory. The plasma is generated using a nanosecond ultraviolet Nd:YAG laser with an irradiance of 1x10 9 W/cm 2 on the sample surface. The spatially integrated plasma light emission was collected and imaged on to the spectrograph slit using an optical-fibre-based collection system. An Echelle spectrograph-ICCD system (Andor Mechelle ME5000-DH734-18U-03PS150) was used to record the emission spectrum. The spectrograph with an Echelle grating covers 200-975 nm spectral range in a single shot with a good wavelength resolution (0.05 nm). The detector was gated in synchronization with the laser pulse to get maximum signal-to-background (S/B) ratio. The detector gate width of 2 μs and the detector gate delay of 2 μs were chosen for recording the plasma emission signals, discriminating the continuum radiation which is intense at initial delay time less than 300 ns and decreases at later time

  5. Atmospheric boundary layer response to sea surface temperatures during the SEMAPHORE experiment

    Science.gov (United States)

    Giordani, Hervé; Planton, Serge; Benech, Bruno; Kwon, Byung-Hyuk

    1998-10-01

    The sensitivity of the marine atmospheric boundary layer (MABL) subjected to sea surface temperatures (SST) during the Structure des Echanges Mer-Atmosphere, Proprietes des Heterogeneites Oceaniques: Recherche Experimentale (SEMAPHORE) experiment in 1993 has been studied. Atmospheric analyses produced by the Action de Recherche, Petite Echelle, Grande Echelle (ARPEGE) operational model at the French meteorological weather service assimilated data sets collected between October 7 and November 17, 1993, merged with the Global Telecommunication System (GTS) data. Analyses were validated against independent data from aircraft instruments collected along a section crossing the Azores oceanic front, not assimilated into the model. The responses of the mean MABL in the aircraft cross section to changes in SST gradients of about 1°C/100 km were the presence of an atmospheric front with horizontal gradients of 1°C/100 km and an increase of the wind intensity from the cold to the warm side during an anticyclonic synoptic situation. The study of the spatiotemporal characteristics of the MABL shows that during 3 days of an anticyclonic synoptic situation the SST is remarkably stationary because it is principally controlled by the Azores ocean current, which has a timescale of about 10 days. However, the temperature and the wind in the MABL are influenced by the prevailing atmospheric conditions. The ocean does not appear to react to the surface atmospheric forcing on the timescale of 3 days, whereas the atmospheric structures are modified by local and synoptic-scale advection. The MABL response appears to be much quicker than that of the SSTs. The correlation between the wind and the thermal structure in the MABL is dominated by the ageostrophic and not by the geostrophic component. In particular, the enhancement of the wind on either side of the SST front is mainly due to the ageostrophic component. Although the surface heat fluxes are not the only cause of ageostrophy, the

  6. THE RUNAWAYS AND ISOLATED O-TYPE STAR SPECTROSCOPIC SURVEY OF THE SMC (RIOTS4)

    Energy Technology Data Exchange (ETDEWEB)

    Lamb, J. B.; Oey, M. S.; Segura-Cox, D. M.; Graus, A. S.; Golden-Marx, J. B. [Astronomy Department, University of Michigan, 1085 S. University Ave., Ann Arbor, MI 48109-1107 (United States); Kiminki, D. C. [Department of Astronomy, University of Arizona, Tucson, AZ 85721 (United States); Parker, J. Wm., E-mail: joellamb@umich.edu [Southwest Research Institute, Department of Space Studies, Suite 300, 1050 Walnut Street, Boulder, CO 80302-5150 (United States)

    2016-02-01

    We present the Runaways and Isolated O-Type Star Spectroscopic Survey of the SMC (RIOTS4), a spatially complete survey of uniformly selected field OB stars that covers the entire star-forming body of the Small Magellanic Cloud (SMC). Using the IMACS (Inamori-Magellan Areal Camera and Spectrograph) multislit spectrograph and MIKE (Magellan Inamori Kyocera Echelle) echelle spectrograph on the Magellan telescopes, we obtained spectra of 374 early-type field stars that are at least 28 pc from any other OB candidates. We also obtained spectra of an additional 23 field stars in the SMC bar identified from slightly different photometric criteria. Here, we present the observational catalog of stars in the RIOTS4 survey, including spectral classifications and radial velocities. For three multi-slit fields covering 8% of our sample, we carried out monitoring observations over 9–16 epochs to study binarity, finding a spectroscopic, massive binary frequency of at least ∼60% in this subsample. Classical Oe/Be stars represent a large fraction of RIOTS4 (42%), occurring at much higher frequency than in the Galaxy, consistent with expectation at low metallicity. RIOTS4 confirmed a steep upper initial mass function in the field, apparently caused by the inability of the most massive stars to form in the smallest clusters. Our survey also yields evidence for in situ field OB star formation, and properties of field emission-line star populations, including sgB[e] stars and classical Oe/Be stars. We also discuss the radial velocity distribution and its relation to SMC kinematics and runaway stars. RIOTS4 presents a first quantitative characterization of field OB stars in an external galaxy, including the contributions of sparse, but normal, star formation; runaway stars; and candidate isolated star formation.

  7. An Extremely Lithium-rich Bright Red Giant in the Globular Cluster M3

    Science.gov (United States)

    Kraft, Robert P.; Peterson, Ruth C.; Guhathakurta, Puragra; Sneden, Christopher; Fulbright, Jon P.; Langer, G. Edward

    1999-06-01

    We have serendipitously discovered an extremely lithium-rich star on the red giant branch of the globular cluster M3 (NGC 5272). An echelle spectrum obtained with the Keck I High-Resolution Echelle Spectrograph reveals a Li I λ6707 resonance doublet of 520 mÅ equivalent width, and our analysis places the star among the most Li-rich giants known: logε(Li)~=+3.0. We determine the elemental abundances of this star, IV-101, and three other cluster members of similar luminosity and color and conclude that IV-101 has abundance ratios typical of giants in M3 and M13 that have undergone significant mixing. We discuss mechanisms by which a low-mass star may be so enriched in Li, focusing on the mixing of material processed by the hydrogen-burning shell just below the convective envelope. While such enrichment could conceivably happen only rarely, it may in fact regularly occur during giant-branch evolution but be rarely detected because of rapid subsequent Li depletion. Based on observations obtained with the Keck I Telescope of the W. M. Keck Observatory, which is operated by the California Association for Research in Astronomy (CARA), Inc., on behalf of the University of California and the California Institute of Technology. This Letter is dedicated to the memory of our beloved colleague Ed Langer, who died after a brief illness on February 16, 1999. Ed brought a unique theoretical perspective to our globular cluster abundance studies. His career truly embodied the academic ideals of inspiration in both teaching and research. He made friends wherever he traveled, and was an inspiration to students. We will miss him greatly.

  8. The Detailed Chemical Properties of M31 Star Clusters. I. Fe, Alpha and Light Elements

    Science.gov (United States)

    Colucci, Janet E.; Bernstein, Rebecca A.; Cohen, Judith G.

    2014-12-01

    We present ages, [Fe/H] and abundances of the α elements Ca I, Si I, Ti I, Ti II, and light elements Mg I, Na I, and Al I for 31 globular clusters (GCs) in M31, which were obtained from high-resolution, high signal-to-noise ratio >60 echelle spectra of their integrated light (IL). All abundances and ages are obtained using our original technique for high-resolution IL abundance analysis of GCs. This sample provides a never before seen picture of the chemical history of M31. The GCs are dispersed throughout the inner and outer halo, from 2.5 kpc < R M31 < 117 kpc. We find a range of [Fe/H] within 20 kpc of the center of M31, and a constant [Fe/H] ~ - 1.6 for the outer halo clusters. We find evidence for at least one massive GC in M31 with an age between 1 and 5 Gyr. The α-element ratios are generally similar to the Milky Way GC and field star ratios. We also find chemical evidence for a late-time accretion origin for at least one cluster, which has a different abundance pattern than other clusters at similar metallicity. We find evidence for star-to-star abundance variations in Mg, Na, and Al in the GCs in our sample, and find correlations of Ca, Mg, Na, and possibly Al abundance ratios with cluster luminosity and velocity dispersion, which can potentially be used to constrain GC self-enrichment scenarios. Data presented here were obtained with the HIRES echelle spectrograph on the Keck I telescope. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

  9. THE DETAILED CHEMICAL PROPERTIES OF M31 STAR CLUSTERS. I. Fe, ALPHA AND LIGHT ELEMENTS

    Energy Technology Data Exchange (ETDEWEB)

    Colucci, Janet E.; Bernstein, Rebecca A. [The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101 (United States); Cohen, Judith G., E-mail: jcolucci@obs.carnegiescience.edu [Palomar Observatory, Mail Stop 105-24, California Institute of Technology, Pasadena, CA 91125 (United States)

    2014-12-20

    We present ages, [Fe/H] and abundances of the α elements Ca I, Si I, Ti I, Ti II, and light elements Mg I, Na I, and Al I for 31 globular clusters (GCs) in M31, which were obtained from high-resolution, high signal-to-noise ratio >60 echelle spectra of their integrated light (IL). All abundances and ages are obtained using our original technique for high-resolution IL abundance analysis of GCs. This sample provides a never before seen picture of the chemical history of M31. The GCs are dispersed throughout the inner and outer halo, from 2.5 kpc < R {sub M31} < 117 kpc. We find a range of [Fe/H] within 20 kpc of the center of M31, and a constant [Fe/H] ∼ – 1.6 for the outer halo clusters. We find evidence for at least one massive GC in M31 with an age between 1 and 5 Gyr. The α-element ratios are generally similar to the Milky Way GC and field star ratios. We also find chemical evidence for a late-time accretion origin for at least one cluster, which has a different abundance pattern than other clusters at similar metallicity. We find evidence for star-to-star abundance variations in Mg, Na, and Al in the GCs in our sample, and find correlations of Ca, Mg, Na, and possibly Al abundance ratios with cluster luminosity and velocity dispersion, which can potentially be used to constrain GC self-enrichment scenarios. Data presented here were obtained with the HIRES echelle spectrograph on the Keck I telescope.

  10. Exoplanet Transits of Stellar Active Regions

    Science.gov (United States)

    Giampapa, Mark S.; Andretta, Vincenzo; Covino, Elvira; Reiners, Ansgar; Esposito, Massimiliano

    2018-01-01

    We report preliminary results of a program to obtain high spectral- and temporal-resolution observations of the neutral helium triplet line at 1083.0 nm in transiting exoplanet systems. The principal objective of our program is to gain insight on the properties of active regions, analogous to solar plages, on late-type dwarfs by essentially using exoplanet transits as high spatial resolution probes of the stellar surface within the transit chord. The 1083 nm helium line is a particularly appropriate diagnostic of magnetized areas since it is weak in the quiet photosphere of solar-type stars but appears strongly in absorption in active regions. Therefore, during an exoplanet transit over the stellar surface, variations in its absorption equivalent width can arise that are functions of the intrinsic strength of the feature in the active region and the known relative size of the exoplanet. We utilized the Galileo Telescope and the GIANO-B near-IR echelle spectrograph to obtain 1083 nm spectra during transits in bright, well-known systems that include HD 189733, HD 209458, and HD 147506 (HAT-P-2). We also obtained simultaneous auxiliary data on the same telescope with the HARPS-N UV-Visible echelle spectrograph. We will present preliminary results from our analysis of the observed variability of the strength of the He I 1083 nm line during transits.Acknowledgements: Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The NSO is operated by AURA under a cooperative agreement with the NSF.

  11. GIARPS@TNG: GIANO-B and HARPS-N together for a wider wavelength range spectroscopy

    Science.gov (United States)

    Claudi, R.; Benatti, S.; Carleo, I.; Ghedina, A.; Guerra, J.; Micela, G.; Molinari, E.; Oliva, E.; Rainer, M.; Tozzi, A.; Baffa, C.; Baruffolo, A.; Buchschacher, N.; Cecconi, M.; Cosentino, R.; Fantinel, D.; Fini, L.; Ghinassi, F.; Giani, E.; Gonzalez, E.; Gonzalez, M.; Gratton, R.; Harutyunyan, A.; Hernandez, N.; Lodi, M.; Malavolta, L.; Maldonado, J.; Origlia, L.; Sanna, N.; Sanjuan, J.; Scuderi, S.; Seemann, U.; Sozzetti, A.; Perez Ventura, H.; Hernandez Diaz, M.; Galli, A.; Gonzalez, C.; Riverol, L.; Riverol, C.

    2017-08-01

    Since 2012, thanks to the installation of the high-resolution echelle spectrograph in the optical range HARPS-N, the Italian telescope TNG (La Palma) became one of the key facilities for the study of the extrasolar planets. In 2014 TNG also offered GIANO to the scientific community, providing a near-infrared (NIR) cross-dispersed echelle spectroscopy covering 0.97-2.45μm at a resolution of 50000. GIANO, although designed for direct light-feed from the telescope at the Nasmyth-B focus, was provisionally mounted on the rotating building and connected via fibers to only available interface at the Nasmyth-A focal plane. The synergy between these two instruments is particularly appealing for a wide range of science cases, especially for the search of exoplanets around young and active stars and the characterisation of their atmosphere. Through the funding scheme "WOW" (a Way to Others Worlds), the Italian National Institute for Astrophysics (INAF) proposed to position GIANO at the focal station for which it was originally designed and the simultaneous use of these spectrographs with the aim to achieve high-resolution spectroscopy in a wide wavelength range (0.383-2.45μm) obtained in a single exposure, giving rise to the project called GIARPS (GIANO-B & HARPS-N). Because of its characteristics, GIARPS can be considered the first and unique worldwide instrument providing not only high resolution in a large wavelength band, but also a high-precision radial velocity measurement both in the visible and in the NIR arm, since in the next future GIANO-B will be equipped with gas absorption cells.

  12. SO2 Spectroscopy with A Tunable UV Laser

    Science.gov (United States)

    Morey, W. W.; Penney, C. M.; Lapp, M.

    1973-01-01

    A portion of the fluorescence spectrum of SO2 has been studied using a narrow wavelength doubled dye laser as the exciting source. One purpose of this study is to evaluate the use of SO2 resonance re-emission as a probe of SO2 in the atmosphere. When the SO2 is excited by light at 300.2 nm, for example, a strong reemission peak is observed which is Stokes-shifted from the incident light wavelength by the usual Raman shift (the VI symmetric vibration frequency 1150.5/cm ). The intensity of this peak is sensitive to small changes (.01 nm) in the incident wavelength. Measurements of the N2 quenching and self quenching of this re-emission have been obtained. Preliminary analysis of this data indicates that the quenching is weak but not negligible. The dye laser in our system is pumped by a pulsed N2 laser. Tuning 'and spectral narrowing are accomplished using a telescope-echelle grating combination. In a high power configuration the resulting pulses have a spectral width of about 5 x 10(exp -3) nm and a time duration of about 6 nsec. The echelle grating is rotated by a digital stepping motor, such that each step shifts the wavelength by 6 x 10(exp -4) nm. In addition to the tunable, narrow wavelength uv source and spectral analysis of the consequent re-emission, the system also provides time resolution of the re-emitted light to 6 nsec resolution. This capability is being used to study the lifetime of low pressure S02 fluorescence at different wavelengths and pressures.

  13. The mass of the black hole in LMC X-3

    Energy Technology Data Exchange (ETDEWEB)

    Orosz, Jerome A. [Department of Astronomy, San Diego State University, 5500 Campanile Drive, San Diego, CA 92182-1221 (United States); Steiner, James F.; McClintock, Jeffrey E. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Buxton, Michelle M.; Bailyn, Charles D. [Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101 (United States); Steeghs, Danny [Department of Physics, University of Warwick, Coventry, CV4 7AL, UK and Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Guberman, Alec [Byram Hills High School, 12 Tripp Lane, Armonk, NY 10504 (United States); Torres, Manuel A. P., E-mail: jorosz@mail.sdsu.edu, E-mail: jsteiner@cfa.harvard.edu, E-mail: jem@cfa.harvard.edu, E-mail: michelle.buxton@yale.edu, E-mail: charles.bailyn@yale.edu, E-mail: D.T.H.Steeghs@warwick.ac.uk, E-mail: alec.guberman@stonybrook.edu, E-mail: M.Torres@sron.nl [SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht (Netherlands)

    2014-10-20

    We analyze a large set of new and archival photometric and spectroscopic observations of LMC X-3 to arrive at a self-consistent dynamical model for the system. Using echelle spectra obtained with the Magellan Inamori Kyocera Echelle instrument on the 6.5 m Magellan Clay telescope and the UVES instrument on the second 8.2 m Very Large Telescope, we find a velocity semiamplitude for the secondary star of K {sub 2} = 241.1 ± 6.2 km s{sup –1}, where the uncertainty includes an estimate of the systematic error caused by X-ray heating. Using the spectra, we also find a projected rotational velocity of V {sub rot}sin i = 118.5 ± 6.6 km s{sup –1}. From an analysis of archival B and V light curves as well as new B and V light curves from the SMARTS 1.3 m telescope, we find an inclination of i = 69.°84 ± 0.°37 for models that do not include X-ray heating and an inclination of i = 69.°24 ± 0.°72 for models that incorporate X-ray heating. Adopting the latter inclination measurement, we find masses of 3.63 ± 0.57 M {sub ☉} and 6.98 ± 0.56 M {sub ☉} for the companion star and the black hole, respectively. We briefly compare our results with earlier work and discuss some of their implications.

  14. Robotic Astronomy and the BOOTES Network of Robotic Telescopes

    Directory of Open Access Journals (Sweden)

    A. J. Castro-Tirado

    2011-01-01

    Full Text Available The Burst Observer and Optical Transient Exploring System (BOOTES, started in 1998 as a Spanish-Czech collaboration project, devoted to a study of optical emissions from gamma ray bursts (GRBs that occur in the Universe. The first two BOOTES stations were located in Spain, and included medium size robotic telescopes with CCD cameras at the Cassegrain focus as well as all-sky cameras, with the two stations located 240 km apart. The first observing station (BOOTES-1 is located at ESAt (INTA-CEDEA in Mazag´on (Huelva and the first light was obtained in July 1998. The second observing station (BOOTES-2 is located at La Mayora (CSIC in M´alaga and has been operating fully since July 2001. In 2009 BOOTES expanded abroad, with the third station (BOOTES-3 being installed in Blenheim (South Island, New Zealand as result of a collaboration project with several institutions from the southern hemisphere. The fourth station (BOOTES-4 is on its way, to be deployed in 2011.

  15. Stand-off detection of chemicals by UV Raman spectroscopy

    International Nuclear Information System (INIS)

    Wu, Ming; Ray, Mark; Hang Fung, K.; Ruckman, Mark W.; Harder, David; Sedlacek, Arthur J. III

    2000-01-01

    Experimental results are reported on a mobile, stand-alone, solar-blind ultraviolet (UV) Raman lidar system for the stand-off detection and identification of liquid and solid targets at ranges of hundreds of meters. The lidar is a coaxial system capable of performing range-resolved measurements of gases and aerosols, as well as solids and liquids. The transmitter is a flash lamp pumped 30 Hz Nd:YAG laser with quadrupled output at 266 nm. The receiver subsystem is comprised of a 40 cm Cassegrain telescope, a holographic UV edge filter for suppressing the elastic channel, a 0.46 m Czerny-Turner spectrometer, and a time gated intensified charge-coupled device (CCD) detector. The rejection of elastic light scattering by the edge filter is better than one part in 10 5 , while the transmittance 500 cm-1 to the red of the laser line is greater than 50%. Raman data are shown for selected solids, neat liquids, and mixtures down to the level of 1% volume ratio. On the basis of the strength of the Raman returns, a stand-off detection limit of ∼500 g/m2 for liquid spills of common solvents at the range of one half of a kilometer is possible. (c) 2000 Society for Applied Spectroscopy

  16. The VLA Low-band Ionosphere and Transient Experiment (VLITE)

    Science.gov (United States)

    Clarke, Tracy; Peters, Wendy; Brisken, Walter; Giacintucci, Simona; Kassim, Namir; Polisensky, Emil; Helmboldt, Joseph; Richards, Emily E.; Erickson, Alan; Ray, Paul S.; Kerr, Matthew T.; Deneva, Julia; Coburn, William; Huber, Robert; Long, Jeff

    2018-01-01

    The VLA Low-band Ionosphere and Transient Experiment (VLITE, http://vlite.nrao.edu/ ) is a commensal low-frequency observing system that has been operational on the National Radio Astronomy Observatory's Karl G. Jansky Very Large Array (VLA) since late 2014. The separate optical paths of the prime-focus sub-GHz dipole feeds and the Cassegrain-focus 1-50 GHz feeds allow both systems to operate simultaneously with independent correlators. The initial 2.5 years of VLITE operation provided real-time correlation of 10 antennas across the 320-384 MHz band with a total observing time approaching 12,000 hours. During the summer of 2017, VLITE was upgraded to a total of 16 antennas (more than doubling the number of baselines) with enhanced correlator capabilities to enable correlation of the on-the-fly observing mode being used for the new NRAO VLA Sky Survey (VLASS).We present an overview of the VLITE system, including highlights of the complexities of a commensal observing program, sparse-array challenges, and scientific capabilities from our science-ready data pipeline. In the longer term, we seek a path to broadband expansion across all VLA antennas to develop a powerful new LOw Band Observatory (LOBO).

  17. Performance Evaluation of Irbene RT-16 Radio Telescope Receiving System

    Directory of Open Access Journals (Sweden)

    Bleiders M.

    2017-12-01

    Full Text Available In the present paper, recent measurement results of refurbished Irbene RT-16 radio telescope receiving system performance are presented. The aim of the research is to evaluate characteristics of RT-16, which will allow carrying out necessary amplitude calibration in both single dish and VLBI observations, to improve the performance of existing system as well as to monitor, control and compare performance if possible changes in the receiving system will occur in future. The evaluated receiving system is 16 m Cassegrain antenna equipped with a cryogenic receiver with frequency range from 4.5 to 8.8 GHz, which is divided into four sub-bands. Multiple calibration sessions have been carried out by observing stable astronomical sources with known flux density by using in-house made total power registration backend. First, pointing offset calibration has been carried out and pointing model coefficients calculated and applied. Then, amplitude calibration, namely antenna sensitivity, calibration diode equivalent flux density and gain curve measurements have been carried out by observing calibration sources at different antenna elevations at each of the receiver sub-bands. Beam patterns have also been evaluated at different frequency bands. As a whole, acquired data will serve as a reference point for comparison in future performance evaluation of RT-16.

  18. Solar Observations at Submillimeter Wavelengths

    Science.gov (United States)

    Kaufmann, P.

    We review earlier to recent observational evidences and theoretical motivations leading to a renewed interest to observe flares in the submillimeter (submm) - infrared (IR) range of wavelengths. We describe the new solar dedicated submillimeter wave telescope which began operations at El Leoncito in the Argentina Andes: the SST project. It consists of focal plane arrays of two 405 GHz and four 212 GHz radiometers placed in a 1.5-m radome-enclosed Cassegrain antenna, operating simultaneously with one millisecond time resolution. The first solar events analyzed exhibited the onset of rapid submm-wave spikes (100-300 ms), well associated to other flare manifestations, especially at X-rays. The spikes positions were found scattered over the flaring source by tens of arcseconds. For one event an excellent association was found between the gamma-ray emission time profile and the rate of occurrence of submm-wave rapid spikes. The preliminary results favour the idea that bulk burst emissions are a response to numerous fast energetic injections, discrete in time, produced at different spatial positions over the flaring region. Coronal mass ejections were associated to the events studied. Their trajectories extrapolated to the solar surface appear to correspond to the onset time of the submm-wave spikes, which might represent an early signature of the CME's initial acceleration process.

  19. High-precision optical systems with inexpensive hardware: a unified alignment and structural design approach

    Science.gov (United States)

    Winrow, Edward G.; Chavez, Victor H.

    2011-09-01

    High-precision opto-mechanical structures have historically been plagued by high costs for both hardware and the associated alignment and assembly process. This problem is especially true for space applications where only a few production units are produced. A methodology for optical alignment and optical structure design is presented which shifts the mechanism of maintaining precision from tightly toleranced, machined flight hardware to reusable, modular tooling. Using the proposed methodology, optical alignment error sources are reduced by the direct alignment of optics through their surface retroreflections (pips) as seen through a theodolite. Optical alignment adjustments are actualized through motorized, sub-micron precision actuators in 5 degrees of freedom. Optical structure hardware costs are reduced through the use of simple shapes (tubes, plates) and repeated components. This approach produces significantly cheaper hardware and more efficient assembly without sacrificing alignment precision or optical structure stability. The design, alignment plan and assembly of a 4" aperture, carbon fiber composite, Schmidt-Cassegrain concept telescope is presented.

  20. Towards eye-safe standoff Raman imaging systems

    Science.gov (United States)

    Glimtoft, Martin; Bââth, Petra; Saari, Heikki; Mäkynen, Jussi; Näsilä, Antti; Östmark, Henric

    2014-05-01

    Standoff Raman imaging systems have shown the ability to detect single explosives particles. However, in many cases, the laser intensities needed restrict the applications where they can be safely used. A new generation imaging Raman system has been developed based on a 355 nm UV laser that, in addition to eye safety, allows discrete and invisible measurements. Non-dangerous exposure levels for the eye are several orders of magnitude higher in UVA than in the visible range that previously has been used. The UV Raman system has been built based on an UV Fabry-Perot Interferometer (UV-FPI) developed by VTT. The design allows for precise selection of Raman shifts in combination with high out-of-band blocking. The stable operation of the UV-FPI module under varying environmental conditions is arranged by controlling the temperature of the module and using a closed loop control of the FPI air gap based on capacitive measurement. The system presented consists of a 3rd harmonics Nd:YAG laser with 1.5 W average output at 1000 Hz, a 200 mm Schmidt-Cassegrain telescope, UV-FPI filter and an ICCD camera for signal gating and detection. The design principal leads to a Raman spectrum in each image pixel. The system is designed for field use and easy manoeuvring. Preliminary results show that in measurements of <60 s on 10 m distance, single AN particles of <300 μm diameter can be identified.

  1. Improving pointing of Toruń 32-m radio telescope: effects of rail surface irregularities

    Science.gov (United States)

    Lew, Bartosz

    2018-03-01

    Over the last few years a number of software and hardware improvements have been implemented to the 32-m Cassegrain radio telescope located near Toruń. The 19-bit angle encoders have been upgraded to 29-bit in azimuth and elevation axes. The control system has been substantially improved, in order to account for a number of previously-neglected, astrometric effects that are relevant for milli-degree pointing. In the summer 2015, as a result of maintenance works, the orientation of the secondary mirror has been slightly altered, which resulted in worsening of the pointing precision, much below the nominal telescope capabilities. In preparation for observations at the highest available frequency of 30-GHz, we use One Centimeter Receiver Array (OCRA), to take the most accurate pointing data ever collected with the telescope, and we analyze it in order to improve the pointing precision. We introduce a new generalized pointing model that, for the first time, accounts for the rail irregularities, and we show that the telescope can have root mean square pointing accuracy at the level < 8″ and < 12″ in azimuth and elevation respectively. Finally, we discuss the implemented pointing improvements in the light of effects that may influence their long-term stability.

  2. Progress towards an Autonomous Field Deployable Diode-Laser-Based Differential Absorption Lidar (DIAL for Profiling Water Vapor in the Lower Troposphere

    Directory of Open Access Journals (Sweden)

    Kevin S. Repasky

    2013-11-01

    Full Text Available A laser transmitter has been developed and incorporated into a micro-pulse differential absorption lidar (DIAL for water vapor profiling in the lower troposphere as an important step towards long-term autonomous field operation. The laser transmitter utilizes two distributed Bragg reflector (DBR diode lasers to injection seed a pulsed tapered semiconductor optical amplifier (TSOA, and is capable of producing up to 10 mJ of pulse energy with a 1 ms pulse duration and a 10 kHz pulse repetition frequency. The on-line wavelength of the laser transmitter can operate anywhere along the water vapor absorption feature centered at 828.187 nm (in vacuum depending on the prevailing atmospheric conditions, while the off-line wavelength operates at 828.287 nm. This laser transmitter has been incorporated into a DIAL instrument utilizing a 35.6 cm Schmidt-Cassegrain telescope and fiber coupled avalanche photodiode (APD operating in the photon counting mode. The performance of the DIAL instrument was demonstrated over a ten-day observation period. During this observation period, data from radiosondes were used to retrieve water vapor number density profiles for comparisons with the number density profiles retrieved from the DIAL data.

  3. The hatfield SCT lunar atlas photographic atlas for Meade, Celestron and other SCT telescopes

    CERN Document Server

    Cook, Jeremy

    2005-01-01

    Schmitt-Cassegrain Telescopes (SCT) and Schmitt-Maksutov telescopes - which include the best-selling models from Meade, Celestron, and other important manufacturers - reverse the visual image left for right, giving a "mirror image". This makes it extremely difficult for observers to identify lunar features at the eyepiece of one of these instruments, using conventional atlases which show the Moon "upside-down" with south at the top. The human brain just doesn't cope well with trying to compare the real thing with a map that is a mirror-image of it!The Hatfield SCT Lunar Atlas solves the problem. Photographs and the detailed key maps are exactly as the Moon appears through the eyepiece of an SCT or Maksutov telescope. Smaller IAU-standard reference photographs are included on each page, to make it simple to compare the mirrored SCT photographs and maps with those that appear in other conventional atlases.Every owner of an SCT - and that's most amateur astronomers - will want this!.

  4. Space-qualified optical thin films by ion-beam-assisted deposition

    International Nuclear Information System (INIS)

    Hsiao, C.N.; Chen, H.P.; Chiu, P.K.; Lin, Y.W.; Chen, F.Z.; Tsai, D.P.

    2013-01-01

    Optical interference coatings designed for use in a space-grade multispectral assembly in a complementary metal-oxide‐semiconductor sensor were deposited on glass by ion-beam-assisted deposition for a Cassegrain-type space-based remote-sensing platform. The patterned multispectral assembly containing blue, green, red, near infrared, and panchromatic multilayer high/low alternated dielectric band-pass filter arrays in a single chip was fabricated by a mechanical mask and the photolithography process. The corresponding properties of the films were investigated by in situ optical monitoring and spectrometry. It was found that the optical properties were significantly improved by employing ion-beam-assisted deposition. The average transmittances were above 88% for the multispectral assembly, with a rejection transmittance of less than 1% in the spectral range 350–1100 nm. To estimate the optical stability of optical coatings for aerospace applications, a space environment assuming a satellite orbiting the Earth at an altitude of near 800 km was simulated by a Co 60 gamma (γ) radiation test. - Highlights: ►Parameters of optical filters were optimized by using admittance loci analysis. ►Higher index of refraction of films prepared by ion beam assisted deposition. ►The dielectric filters have acceptable resistance after γ radiation exposure

  5. Optical overview and qualification of the LLCD space terminal

    Science.gov (United States)

    DeVoe, C. E.; Pillsbury, A. D.; Khatri, F.; Burnside, J. M.; Raudenbush, A. C.; Petrilli, L. J.; Williams, T.

    2017-11-01

    In October 2013 the Lunar Laser Communications Demonstration (LLCD) made communications history by successfully demonstrating 622 megabits per second laser communication from the moon's orbit to earth. The LLCD consisted of the Lunar Laser Communication Space Terminal (LLST), developed by MIT Lincoln Laboratory, mounted on NASA's Lunar Atmosphere and Dust Environment Explorer (LADEE) spacecraft and a primary ground terminal located in New Mexico, the Lunar Laser Communications Ground Terminal (LLGT), and two alternate ground terminals. This paper presents the optical layout of the LLST, the approach for testing the optical subsystems, and the results of the optical qualification of the LLST. Also described is the optical test set used to qualify the LLST. The architecture philosophy for the optics was to keep a small, simple optical backend that provided excellent boresighting and high isolation between the optical paths, high quality wavefront on axis, with minimal throughput losses on all paths. The front end large optics consisted of a Cassegrain 107mm telescope with an f/0.7 parabolic primary mirror and a solar window to reduce the thermal load on the telescope and to minimize background light received at the sensors.

  6. Observations of Bright Massive Stars Using Small Size Telescopes

    Science.gov (United States)

    Beradze, Sopia; Kochiashvili, Nino

    2017-11-01

    The size of a telescope determines goals and objects of observations. During the latest decades it becomes more and more difficult to get photometric data of bright stars because most of telescopes of small sizes do not operate already. But there are rather interesting questions connected to the properties and evolution ties between different types of massive stars. Multi-wavelength photometric data are needed for solution of some of them. We are presenting our observational plans of bright Massive X-ray binaries, WR and LBV stars using a small size telescope. All these stars, which are presented in the poster are observational targets of Sopia Beradze's future PhD thesis. We already have got very interesting results on the reddening and possible future eruption of the massive hypergiant star P Cygni. Therefore, we decided to choose some additional interesting massive stars of different type for future observations. All Massive stars play an important role in the chemical evolution of galaxies because of they have very high mass loss - up to 10-4M⊙/a year. Our targets are on different evolutionary stages and three of them are the members of massive binaries. We plan to do UBVRI photometric observations of these stars using the 48 cm Cassegrain telescope of the Abastumani Astrophisical Observatory.

  7. Searching for MHz Transients with the VLA Low-band Ionosphere and Transient Experiment (VLITE)

    Science.gov (United States)

    Polisensky, Emil; Peters, Wendy; Giacintucci, Simona; Clarke, Tracy; Kassim, Namir E.; hyman, Scott D.; van der Horst, Alexander; Linford, Justin; Waldron, Zach; Frail, Dale

    2018-01-01

    NRL and NRAO have expanded the low frequency capabilities of the VLA through the VLA Low-band Ionosphere and Transient Experiment (VLITE, http://vlite.nrao.edu/ ), effectively making the instrument two telescopes in one. VLITE is a commensal observing system that harvests data from the prime focus in parallel with normal Cassegrain focus observing on a subset of VLA antennas. VLITE provides over 6000 observing hours per year in a > 5 square degree field-of-view using 64 MHz bandwidth centered on 352 MHz. By operating in parallel, VLITE offers invaluable low frequency data to targeted observations of transient sources detected at higher frequencies. With arcsec resolution and mJy sensitivity, VLITE additionally offers great potential for blind searches of rarer radio-selected transients. We use catalog matching software on the imaging products from the daily astrophysics pipeline and the LOFAR Transients Pipeline (TraP) on repeated observations of the same fields to search for coherent and incoherent astronomical transients on timescales of a few seconds to years. We present the current status of the VLITE transient science program from its initial deployment on 10 antennas in November 2014 through its expansion to 16 antennas in the summer of 2017. Transient limits from VLITE’s first year of operation (Polisensky et al. 2016) are updated per the most recent analysis.

  8. "LOSA-S" - basic lidar of the CSF "ATMOSPHERE" IAO SB RAS for tropospheric studies

    Science.gov (United States)

    Balin, Yu. S.; Kokhanenko, G. P.; Klemasheva, M. G.; Penner, I. E.; Nasonov, S. V.; Samoilova, S. V.

    2017-11-01

    Stationary lidar "LOSA-S" of the center of shared facilities (CSF) "ATMOSPHERE" IAO SB RAS is intended for the study of aerosol fields in the boundary layer of the troposphere in the height range 0.5 up to 15 km, as well as for the study of crystal clouds using the polarization unit with linear and circular polarization of radiation. The scheme of simultaneous observation of the elastic and Raman scattering signals when irradiating the medium at the wavelengths of 1064, 532 and 355 nm is realized in the lidar. The lidar is based on the LOTIS-2135 Nd:YAG laser and the receiving specular telescope of the Cassegrain system with the diameter of 300 mm. In addition to the return signals of elastic scattering recorded in analog mode, the lidar records the Raman scattering signals on molecular nitrogen (387 and 607 nm) and water vapor (407 nm) in the photon counting mode. To realize the aforementioned height range, two receiving telescopes are used in the lidar for near and far zones, the signals are recorded by the same photodetectors.

  9. Medium-sized aperture camera for Earth observation

    Science.gov (United States)

    Kim, Eugene D.; Choi, Young-Wan; Kang, Myung-Seok; Kim, Ee-Eul; Yang, Ho-Soon; Rasheed, Ad. Aziz Ad.; Arshad, Ahmad Sabirin

    2017-11-01

    Satrec Initiative and ATSB have been developing a medium-sized aperture camera (MAC) for an earth observation payload on a small satellite. Developed as a push-broom type high-resolution camera, the camera has one panchromatic and four multispectral channels. The panchromatic channel has 2.5m, and multispectral channels have 5m of ground sampling distances at a nominal altitude of 685km. The 300mm-aperture Cassegrain telescope contains two aspheric mirrors and two spherical correction lenses. With a philosophy of building a simple and cost-effective camera, the mirrors incorporate no light-weighting, and the linear CCDs are mounted on a single PCB with no beam splitters. MAC is the main payload of RazakSAT to be launched in 2005. RazakSAT is a 180kg satellite including MAC, designed to provide high-resolution imagery of 20km swath width on a near equatorial orbit (NEqO). The mission objective is to demonstrate the capability of a high-resolution remote sensing satellite system on a near equatorial orbit. This paper describes the overview of the MAC and RarakSAT programmes, and presents the current development status of MAC focusing on key optical aspects of Qualification Model.

  10. NIMBUS-7 CZCS. Coastal Zone Color Scanner Imagery for Selected Coastal Regions. North America - Europe. South America - Africa - Antarctica. Level 2 Photographic Product

    Science.gov (United States)

    1984-01-01

    The Nimbus-7 Coastal Zone Color Scanner (CZCS) is the first spacecraft instrument devoted to the measurement of ocean color. Although instruments on other satellites have sensed ocean color, their spectral bands, spatial resolution, and dynamic range were optimized for geographical or meteorological use. In the CZCS, every parameter is optimized for use over water to the exclusion of any other type of sensing. The signal-to-noise ratios in the spectral channels sensing reflected solar radiance are higher than those required in the past. These ratios need to be high because the ocean is such a poor reflecting surface that the majority of the signal seen by the reflected energy channels at spacecraft altitudes is backscattered solar radiation from the atmosphere rather than reflected solar energy from the ocean. The CZCS is a conventional multichannel scanning radiometer utilizing a rotating plane mirror at a 45 deg angle to the optic axis of a Cassegrain telescope. The mirror scans 360 deg; however, only 80 deg of data centered on the spacecraft nadir is collected for ocean color measurements. Spatial resolution at spacecraft nadir is 825x825 m with some degradation at the edges of the scan swath. The useful swath width from a spacecraft altitude of 955 km is 1600 km.

  11. Roger Hayward and the Invention of the Two-Mirror Schmidt

    Science.gov (United States)

    Bell, T. E.

    2005-12-01

    Roger Hayward (1899-1979), now virtually unknown, was a multitalented architect, scientific illustrator, and optical inventor. Remembered primarily for illustrating Scientific American magazine's Amateur Scientist column between 1949 and 1974, he also illustrated more than a dozen textbooks in optics, physics, geology, oceanography, and chemistry, several of which became classics in their fields. He designed façades with astronomical themes for major buildings in Los Angeles, California, and sculpted mammoth, realistic models of the moon for Griffith Observatory, Adler Planetarium, and Disneyland. Throughout his life, he recreationally painted watercolors and oils that at least one critic likened to the work of John Singer Sargent. Hayward is least known as an optical designer, yet he made significant contributions to the DU spectrophotometer that established the multimillion-dollar company Beckman Instruments. During the pre-radar days of World War II at Mount Wilson Observatory, Hayward invented a classified Cassegrain version of the Schmidt telescope especially adapted for nighttime infrared aerial photography, plus extraordinarily simple machines that allowed inexperienced soldiers to grind, polish, and test accurate aspheric Schmidt correcting plates at speeds compatible with mass production - and later received U.S. patents for them all. This paper, drawn in part from unpublished letters between Hayward and Albert G. Ingalls, will feature little-known images of Hayward's work.

  12. Optical Alignment of the Chromospheric Lyman-Alpha SpectroPolarimeter using Sophisticated Methods to Minimize Activities under Vacuum

    Science.gov (United States)

    Giono, G.; Katsukawa, Y.; Ishikawa, R.; Narukage, N.; Kano, R.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.; hide

    2016-01-01

    The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a sounding-rocket instrument developed at the National Astronomical Observatory of Japan (NAOJ) as a part of an international collaboration. The in- strument main scientific goal is to achieve polarization measurement of the Lyman-alpha line at 121.56 nm emitted from the solar upper-chromosphere and transition region with an unprecedented 0.1% accuracy. For this purpose, the optics are composed of a Cassegrain telescope coated with a "cold mirror" coating optimized for UV reflection and a dual-channel spectrograph allowing for simultaneous observation of the two orthogonal states of polarization. Although the polarization sensitivity is the most important aspect of the instrument, the spatial and spectral resolutions of the instrument are also crucial to observe the chromospheric features and resolve the Ly- pro les. A precise alignment of the optics is required to ensure the resolutions, but experiments under vacuum conditions are needed since Ly-alpha is absorbed by air, making the alignment experiments difficult. To bypass this issue, we developed methods to align the telescope and the spectrograph separately in visible light. We will explain these methods and present the results for the optical alignment of the CLASP telescope and spectrograph. We will then discuss the combined performances of both parts to derive the expected resolutions of the instrument, and compare them with the flight observations performed on September 3rd 2015.

  13. Chromospheric Lyman-alpha spectro-polarimeter (CLASP)

    Science.gov (United States)

    Kano, Ryouhei; Bando, Takamasa; Narukage, Noriyuki; Ishikawa, Ryoko; Tsuneta, Saku; Katsukawa, Yukio; Kubo, Masahito; Ishikawa, Shin-nosuke; Hara, Hirohisa; Shimizu, Toshifumi; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Sakao, Taro; Goto, Motoshi; Kato, Yoshiaki; Imada, Shinsuke; Kobayashi, Ken; Holloway, Todd; Winebarger, Amy; Cirtain, Jonathan; De Pontieu, Bart; Casini, Roberto; Trujillo Bueno, Javier; Štepán, Jiří; Manso Sainz, Rafael; Belluzzi, Luca; Asensio Ramos, Andres; Auchère, Frédéric; Carlsson, Mats

    2012-09-01

    One of the biggest challenges in heliophysics is to decipher the magnetic structure of the solar chromosphere. The importance of measuring the chromospheric magnetic field is due to both the key role the chromosphere plays in energizing and structuring the outer solar atmosphere and the inability of extrapolation of photospheric fields to adequately describe this key boundary region. Over the last few years, significant progress has been made in the spectral line formation of UV lines as well as the MHD modeling of the solar atmosphere. It is found that the Hanle effect in the Lyman-alpha line (121.567 nm) is a most promising diagnostic tool for weaker magnetic fields in the chromosphere and transition region. Based on this groundbreaking research, we propose the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) to NASA as a sounding rocket experiment, for making the first measurement of the linear polarization produced by scattering processes and the Hanle effect in the Lyman-alpha line (121.567 nm), and making the first exploration of the magnetic field in the upper chromosphere and transition region of the Sun. The CLASP instrument consists of a Cassegrain telescope, a rotating 1/2-wave plate, a dual-beam spectrograph assembly with a grating working as a beam splitter, and an identical pair of reflective polarization analyzers each equipped with a CCD camera. We propose to launch CLASP in December 2014.

  14. Measurement of liquid film flow on nuclear rod bundle in micro-scale by using very high speed camera system

    Science.gov (United States)

    Pham, Son; Kawara, Zensaku; Yokomine, Takehiko; Kunugi, Tomoaki

    2012-11-01

    Playing important roles in the mass and heat transfer as well as the safety of boiling water reactor, the liquid film flow on nuclear fuel rods has been studied by different measurement techniques such as ultrasonic transmission, conductivity probe, etc. Obtained experimental data of this annular two-phase flow, however, are still not enough to construct the physical model for critical heat flux analysis especially at the micro-scale. Remain problems are mainly caused by complicated geometry of fuel rod bundles, high velocity and very unstable interface behavior of liquid and gas flow. To get over these difficulties, a new approach using a very high speed digital camera system has been introduced in this work. The test section simulating a 3×3 rectangular rod bundle was made of acrylic to allow a full optical observation of the camera. Image data were taken through Cassegrain optical system to maintain the spatiotemporal resolution up to 7 μm and 20 μs. The results included not only the real-time visual information of flow patterns, but also the quantitative data such as liquid film thickness, the droplets' size and speed distributions, and the tilt angle of wavy surfaces. These databases could contribute to the development of a new model for the annular two-phase flow. Partly supported by the Global Center of Excellence (G-COE) program (J-051) of MEXT, Japan.

  15. Concept Design of a Multi-Band Shared Aperture Reflectarray/Reflector Antenna

    Science.gov (United States)

    Spence, Thomas; Cooley, Michael; Stenger, Peter; Park, Richard; Li, Lihua; Racette, Paul; Heymsfield, Gerald; Mclinden, Matthew

    2016-01-01

    A scalable dual-band (KaW) shared-aperture antenna system design has been developed as a proposed solution to meet the needs of the planned NASA Earth Science Aerosol, Clouds, and Ecosystem (ACE) mission. The design is comprised of a compact Cassegrain reflector/reflectarray with a fixed pointing W-band feed and a cross track scanned Ka-band Active Electronically Scanned Array (AESA). Critical Sub-scale prototype testing and flight tests have validated some of the key aspects of this innovative antenna design, including the low loss reflector/reflectarray surface.More recently the science community has expressed interest in a mission that offers the ability to measure precipitation in addition to clouds and aerosols. In this paper we present summaries of multiple designs that explore options for realizing a tri-frequency (KuKaW), shared-aperture antenna system to meet these science objectives. Design considerations include meeting performance requirements while emphasizing payload size, weight, prime power, and cost. The extensive trades and lessons learned from our previous dual-band ACE system development were utilized as the foundation for this work.

  16. Design and performance of an ultraviolet resonance Raman spectrometer for proteins and nucleic acids.

    Science.gov (United States)

    Russell, M P; Vohník, S; Thomas, G J

    1995-04-01

    We describe an ultraviolet resonance Raman (UVRR) spectrometer appropriate for structural studies of biological macromolecules and their assemblies. Instrument design includes the following features: a continuous wave, intracavity doubled, ultraviolet laser source for excitation of the Raman spectrum; a rotating cell (or jet source) for presentation of the sample to the laser beam; a Cassegrain optic with f/1.0 aperture for collection of the Raman scattering; a quartz prism dispersing element for rejection of stray light and Rayleigh scattering; a 0.75-m single grating monochromator for dispersion of the Raman scattering; and a liquid-nitrogen-cooled, charge-coupled device for detection of the Raman photons. The performance of this instrument, assessed on the basis of the observed signal-to-noise ratios, the apparent resolution of closely spaced spectral bands, and the wide spectrometer bandpass of 2200 cm-1, is believed superior to previously described UVRR spectrometers of similar design. Performance characteristics of the instrument are demonstrated in UVRR spectra obtained from standard solvents, p-ethylphenol, which serves as a model for the tyrosine side chain, the DNA nucleotide deoxyguanosine-5'-monophosphate, and the human tumor necrosis factor binding protein, which is considered representative of soluble globular proteins.

  17. The Reappearance of Venus Observed 8 October 2015

    Science.gov (United States)

    Dunham, David W.; Dunham, Joan B.

    2018-01-01

    The reappearance of Venus on October 8, 2015 offered a unique opportunity to attempt observation of the ashen light of Venus as the unlit side of Venus emerged from behind the dark side of the Moon. The dark side of Venus would be offered to observers without interference from the bright side of Venus or of the Moon. Observations were made from Alice Springs, Australia visually with a 20-cm Schmidt-Cassegrain and with a low-light level surveillance camera on a 25-cm reflector. No evidence of the dark side was noted by the visual observer, the video shows little indication of Venus prior to the bright side reappearance. The conclusion reached is that the ashen light, as it was classically defined, is not observable visually or with small telescopes in the visual regime.The presentation describes the prediction, observation technique, and various analyses by the authors and others to draw conclusions from the data.To date, the authors have been unable to locate any reports of others attempting to observe this unique event. That is a pity since, not only was it interesting for an attempt to verify past observations of the ashen light, it was also a visually stunning event.

  18. Electrical Rating of Concentrated Photovoltaic (CPV) Systems: Long-Term Performance Analysis and Comparison to Conventional PV Systems

    KAUST Repository

    Burhan, Muhammad

    2016-02-29

    The dynamic nature of meteorological data and the commercial availability of diverse photovoltaic systems, ranging from single-junction silicon-based PV panels to concentrated photovoltaic (CPV) systems utilizing multi-junction solar cells and a two-axis solar tracker, demand a simple but accurate methodology for energy planners and PV system designers to understand the economic feasibility of photovoltaic or renewable energy systems. In this paper, an electrical rating methodology is proposed that provides a common playing field for planners, consumers and PV manufacturers to evaluate the long-term performance of photovoltaic systems, as long-term electricity rating is deemed to be a quick and accurate method to evaluate economic viability and determine plant sizes and photovoltaic system power production. A long-term performance analysis based on monthly and electrical ratings (in kWh/m2/year) of two developed CPV prototypes, the Cassegrain mini dish and Fresnel lens CPVs with triple-junction solar cells operating under the meteorological conditions of Singapore, is presented in this paper. Performances are compared to other conventional photovoltaic systems.

  19. Extrasolar Planetary Imaging Coronagraph (EPIC)

    Science.gov (United States)

    Clampin, Mark

    2009-01-01

    The Extrasolar Planetary Imaging Coronagraph (EPIC) is a proposed NASA Exoplanet Probe mission to image and characterize extrasolar giant planets. EPIC will provide insights into the physical nature and architecture of a variety of planets in other solar systems. Initially, it will detect and characterize the atmospheres of planets identified by radial velocity surveys, determine orbital inclinations and masses and characterize the atmospheres around A and F type stars which cannot be found with RV techniques. It will also observe the inner spatial structure of exozodiacal disks. EPIC has a heliocentric Earth trailing drift-away orbit, with a 5 year mission lifetime. The robust mission design is simple and flexible ensuring mission success while minimizing cost and risk. The science payload consists of a heritage optical telescope assembly (OTA), and visible nulling coronagraph (VNC) instrument. The instrument achieves a contrast ratio of 10^9 over a 5 arcsecond field-of-view with an unprecedented inner working angle of 0.13 arcseconds over the spectral range of 440-880 nm. The telescope is a 1.65 meter off-axis Cassegrain with an OTA wavefront error of lambda/9, which when coupled to the VNC greatly reduces the requirements on the large scale optics.

  20. Optical design of CCAT

    Science.gov (United States)

    Cortés-Medellín, Germán; Herter, Terry

    2006-06-01

    The Cornell Caltech Atacama Telescope (CCAT) is a 25m-class sub-millimeter radio telescope capable of operating from 300GHz up to 1.5 THz. The CCAT optical design is an f/8 Ritchey-Chretien (RC) system in a dual Nasmyth focus configuration and a 20 arc-min FOV (diffraction limited imaging performance better than 0.31" at the edge of the field). The large FOV is capable to accommodate up to 1200x1200 (Nyquist Sampled) Pixels at 200 microns, with better than 96% Strehl ratio. The telescope pedestal assembly is a counterbalanced elevation over azimuth design. The main reflector surface is segmented and actively controlled to attain diffraction-limited operation up to 200 microns. A flat Mirror located behind the main reflector vertex provides the optical path relay to either of the two Nasmyth platforms and to a bent-Cassegrain focus for surface calibration. We present the imaging characteristics of the CCAT over the 20arc-min FOV at 200 microns at the Nasmyth focal plane, as well as the positioning sensitivity analysis of CCAT's 3.2m-diameter sub-reflector given in terms of the telescope optical performance, antenna pointing requirements and sub-reflector chopping characteristics.

  1. Mirrors design, analysis and manufacturing of the 550mm Korsch telescope experimental model

    Science.gov (United States)

    Huang, Po-Hsuan; Huang, Yi-Kai; Ling, Jer

    2017-08-01

    In 2015, NSPO (National Space Organization) began to develop the sub-meter resolution optical remote sensing instrument of the next generation optical remote sensing satellite which follow-on to FORMOSAT-5. Upgraded from the Ritchey-Chrétien Cassegrain telescope optical system of FORMOSAT-5, the experimental optical system of the advanced optical remote sensing instrument was enhanced to an off-axis Korsch telescope optical system which consists of five mirrors. It contains: (1) M1: 550mm diameter aperture primary mirror, (2) M2: secondary mirror, (3) M3: off-axis tertiary mirror, (4) FM1 and FM2: two folding flat mirrors, for purpose of limiting the overall volume, reducing the mass, and providing a long focal length and excellent optical performance. By the end of 2015, we implemented several important techniques including optical system design, opto-mechanical design, FEM and multi-physics analysis and optimization system in order to do a preliminary study and begin to develop and design these large-size lightweight aspheric mirrors and flat mirrors. The lightweight mirror design and opto-mechanical interface design were completed in August 2016. We then manufactured and polished these experimental model mirrors in Taiwan; all five mirrors ware completed as spherical surfaces by the end of 2016. Aspheric figuring, assembling tests and optical alignment verification of these mirrors will be done with a Korsch telescope experimental structure model in 2018.

  2. THE FIRST HIGH-REDSHIFT QUASAR FROM Pan-STARRS

    International Nuclear Information System (INIS)

    Morganson, Eric; De Rosa, Gisella; Decarli, Roberto; Walter, Fabian; Rix, Hans-Walter; Chambers, Ken; Burgett, William; Flewelling, Heather; Hodapp, Klaus; Kaiser, Nick; Magnier, Eugene; Sweeney, Bill; Waters, Christopher; McGreer, Ian; Fan, Xiaohui; Greiner, Jochen; Price, Paul

    2012-01-01

    We present the discovery of the first high-redshift (z > 5.7) quasar from the Panoramic Survey Telescope and Rapid Response System 1 (Pan-STARRS1 or PS1). This quasar was initially detected as an i P1 dropout in PS1, confirmed photometrically with the SAO Wide-field InfraRed Camera at Arizona's Multiple Mirror Telescope (MMT) and the Gamma-Ray Burst Optical/Near-Infrared Detector at the MPG 2.2 m telescope in La Silla. The quasar was verified spectroscopically with the MMT Spectrograph, Red Channel and the Cassegrain Twin Spectrograph at the Calar Alto 3.5 m telescope. Its near-infrared spectrum was taken at the Large Binocular Telescope Observatory (LBT) with the LBT Near-Infrared Spectroscopic Utility with Camera and Integral Field Unit for Extragalactic Research. It has a redshift of 5.73, an AB z P1 magnitude of 19.4, a luminosity of 3.8 × 10 47 erg s –1 , and a black hole mass of 6.9 × 10 9 M ☉ . It is a broad absorption line quasar with a prominent Lyβ peak and a very blue continuum spectrum. This quasar is the first result from the PS1 high-redshift quasar search that is projected to discover more than 100 i P1 dropout quasars and could potentially find more than 10 z P1 dropout (z > 6.8) quasars.

  3. 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.

  4. 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.

  5. Metodologias para o ensino de astronomia e Física através da construção de telescópios

    Directory of Open Access Journals (Sweden)

    Tamara de O. Bernardes

    2008-09-01

    Full Text Available This work contemplates the construction of reflecting telescopes as didactic tool for Physics and Astronomy teaching. Each stage of the construction can be linked with the contents of geometric optics and optical physics with different approaches, depending on the education level of working: Fundamental, High-School or Graduation. It was possible to verify that the construction of reflecting telescopes of the Newtonian type shows up as accessible and easily understood by graduated students involved in the project, turning the learning of Physics and other related sciences as motivating and efficient. In the other hand, the construction of the reflecting telescope of Cassegrain type must be considered only when involving students of graduation level, because it concerns more complex processes in the accomplishment and analysis of the primary and secondary mirror surfaces. Moreover, the development of the apparatus construction yields the creation of the Group of Studies of Astronomy in the Department of Physics of the Unesp, campus of Bauru, where subjects related to astronomy education have been treated and discussed jointly with students and teachers of Fundamental and High School levels. Our conclusion is that the use of the telescopes to teach students of Fundamental and High School levels has been a great incentive to the observation of the sky and to the comprehension of many celestial phenomena, relating them to contents of Physics and also other sciences, such as Mathematics, Geography, Environmental education and Meteorology.

  6. TMAP: A NEO follow-up program utilizing undergraduate observers

    Science.gov (United States)

    Ramirez, C.; Deaver, D.; Martinez, R.; Foster, J.; Kuang, L.; Ates, A.; Anderson, M.; Mijac, M.; Gillam, S.; Hicks, M. D.

    2000-10-01

    In the spring of 2000 we began TMAP (Table Mountain Astrometry Project), a program designed to provide timely astrometric followup of newly discovered near-Earth asteroids. Relying on undergraduate observers from the local California State Universities, we have to date been involved with the over 50 NEO and new comet discoveries. This is a significant fraction of all near-Earth asteroids discovered over the time period. All observations are performed at JPL's Table Mountain Facility near Wrightwood California using the 0.6-meter telescope equipped with a Photometrics LN cooled 1k CCD mounted at the cassegrain focus. With this system we can routinely detect objects to R=20.5. We have typically scheduled two runs per month on weekends bracketing the new moon. The student observers man the telescope are trained to select and obtain R-band images of candidates from the Minor Planet Center's NEO Confirmation Page (http://cfa-www.harvard.edu/cfa/ps/NEO/TheNEOPage.html). The astrometry is then reduced and submitted to the Minor Planet Center the following day. TMAP has proven to be an efficient way both to obtain much needed astrometric measurements of newly discovered small bodies as well as to involve undergraduate researchers in planetary research. The limiting magnitudes provided by the 0.6-meter partially fills the gap between the extremely helpful and dedicated amateur astromitrists and the followup that the NEO detection programs do themselves. This work is supported by NASA.

  7. Development and Deployment of a Compact Eye-Safe Scanning Differential absorption Lidar (DIAL) for Spatial Mapping of Carbon Dioxide for Monitoring/Verification/Accounting at Geologic Sequestration Sites

    Energy Technology Data Exchange (ETDEWEB)

    Repasky, Kevin

    2014-03-31

    A scanning differential absorption lidar (DIAL) instrument for monitoring carbon dioxide has been developed. The laser transmitter uses two tunable discrete mode laser diodes (DMLD) operating in the continuous wave (cw) mode with one locked to the online absorption wavelength and the other operating at the offline wavelength. Two in-line fiber optic switches are used to switch between online and offline operation. After the fiber optic switch, an acousto- optic modulator (AOM) is used to generate a pulse train used to injection seed an erbium doped fiber amplifier (EDFA) to produce eye-safe laser pulses with maximum pulse energies of 66 {micro}J, a pulse repetition frequency of 15 kHz, and an operating wavelength of 1.571 {micro}m. The DIAL receiver uses a 28 cm diameter Schmidt-Cassegrain telescope to collect that backscattered light, which is then monitored using a photo-multiplier tube (PMT) module operating in the photon counting mode. The DIAL instrument has been operated from a laboratory environment on the campus of Montana State University, at the Zero Emission Research Technology (ZERT) field site located in the agricultural research area on the western end of the Montana State University campus, and at the Big Sky Carbon Sequestration Partnership site located in north-central Montana. DIAL data has been collected and profiles have been validated using a co-located Licor LI-820 Gas Analyzer point sensor.

  8. Thermal Stability of a 4 Meter Primary Reflector for the Scanning Microwave Limb Sounder

    Science.gov (United States)

    Cofield, Richard E.; Kasl, Eldon P.

    2011-01-01

    The Scanning Microwave Limb Sounder (SMLS) is a space-borne heterodyne radiometer which will measure pressure, temperature and atmospheric constituents from thermal emission in [180,680] GHz. SMLS, planned for the NRC Decadal Survey's Global Atmospheric Composition Mission, uses a novel toric Cassegrain antenna to perform both elevation and azimuth scanning. This provides better horizontal and temporal resolution and coverage than were possible with elevation-only scanning in the two previous MLS satellite instruments. SMLS is diffraction-limited in the vertical plane but highly astigmatic in the horizontal (beam aspect ratio approx. 1:20). Nadir symmetry ensures that beam shape is nearly invariant over plus or minus 65 deg azimuth. A low-noise receiver FOV is swept over the reflector system by a small azimuth-scanning mirror. We describe the fabrication and thermal-stability test of a composite demonstration primary reflector, having full 4m height and 1/3 the width planned for flight. Using finite-element models of reflectors and structure, we evaluate thermal deformations and optical performance for 4 orbital environments and isothermal soak. We compare deformations with photogrammetric measurements made during soak tests in a chamber. The test temperature range exceeds predicted orbital ranges by large factors, implying in-orbit thermal stability of 0.21 micron rms (root mean square)/C, which meets SMLS requirements.

  9. Gamma Bang Time/Reaction History Diagnostics for the National Ignition Facility (NIF) Using 900 Off-axis Parabolic Mirrors

    International Nuclear Information System (INIS)

    H.W. Herrmann; R.M. Malone; W. Stoeffl; J.M. Mack; C.S. Young

    2008-01-01

    Gas Cherenkov detectors (GCD) have been used to convert fusion gamma into photons to achieve gamma bang time (GBT) and reaction history measurements. The GCD designed for Omega used Cassegrain reflector optics in order to fit inside a ten-inch manipulator. A novel design for the National Ignition Facility (NIF) using 90 o Off-Axis Parabolic (OAP) mirrors will increase light collection efficiency from fusion gammas and achieve minimum time dispersion. The broadband Cherenkov light (from 200 to 800 nm) is relayed into a high-speed detector using three parabolic mirrors. Because light is collected from many source planes throughout the CO2 gas volume, the detector is positioned at the stop position rather than an image position. The stop diameter and its position are independent of the light-generation location along the gas cell. The current design collects light from a 100-mm diameter by 500-mm-long gas volume. Optical ray tracings demonstrate how light can be collected from different angled trajectories of the Compton electrons as they fly through the CO2 gas volume. A cluster of four channels will allow for increased dynamic range as well as different gamma energy threshold sensitivities

  10. Gamma bang time/reaction history diagnostics for the National Ignition Facility using 90 degrees off-axis parabolic mirrors.

    Science.gov (United States)

    Malone, R M; Herrmann, H W; Stoeffl, W; Mack, J M; Young, C S

    2008-10-01

    Gas Cherenkov detectors (GCDs) have been used to convert fusion gamma into photons to achieve gamma bang time and reaction history measurements. The GCDs designed for OMEGA used Cassegrain reflector optics in order to fit inside a 10 in. manipulator. A novel design for the National Ignition Facility using 90 degrees off-axis parabolic mirrors will increase light collection efficiency from fusion gammas and achieve minimum time dispersion. The broadband Cherenkov light (from 200 to 800 nm) is relayed into a high-speed detector using three parabolic mirrors. Because light is collected from many source planes throughout the CO(2) gas volume, the detector is positioned at the stop position rather than at an image position. The stop diameter and its position are independent of the light-generation location along the gas cell. The current design collects light from a 100 mm diameter by 500 mm long gas volume. Optical ray tracings demonstrate how light can be collected from different angled trajectories of the Compton electrons as they fly through the CO(2) gas volume. A cluster of four channels will allow for increased dynamic range as well as for different gamma energy threshold sensitivities.

  11. Spectrophotometry of Pluto from 3500 to 7350 A

    International Nuclear Information System (INIS)

    Barker, E.S.; Cochran, W.D.; Cochran, A.L.; Texas, University, Austin, Tex.)

    1980-01-01

    Spectra of Pluto have been obtained on six nights during February 1979 by the use of the Cassegrain Digicon spectrograph on the 2.1-m Struve reflector and the IDS spectrograph on the 2.7-m reflector of McDonald Observatory. These spectra, with nominal resolution of 6-7 A, have been reduced to relative fluxes. Relative albedos were then calculated using the solar irradiances of Arvesen et al. (1969). The spectra taken in the blue show no indication of the upturn in albedo at wavelengths less than 3800 A previously reported by Fix, et al. (1970). The lack of a UV upturn cannot be interpreted in terms of a Rayleigh scattering atmosphere unless the albedo of the underlying surface is known. From the lack of methane absorption at the wavelength of the 6190- or 7270-A methane bands, an upper limit of 1-3 m-am of gaseous CH4 is derived. The albedo curve has a constant slope between 3500 and 7300 A. The only other solar system body which has this feature is an S-type asteroid

  12. Extending the McDonald Observatory Serendipitous Survey of UV/Blue Asteroid Spectra

    Science.gov (United States)

    Vilas, Faith; Cochran, A. L.

    1999-01-01

    Moderate resolution asteroid spectra in the 350 - 650 nm spectral range acquired randomly over many years (Cochran and Vilas, Icarus v 127, 121, 1997) identified absorption features in spectra of some of the asteroids. A feature centered at 430 nm was identified in the spectra of some low-albedo asteroids (C class and subclass), similar to the feature identified by Vilas et al. (Icarus, v. 102, 225,1993) in other low-albedo asteroid spectra and attributed to a ferric iron spin-forbidden transition in iron alteration minerals such as jarosite. Features at 505 nm and 430 nm were identified in the spectrum of 4 Vesta. The 505-nm feature is highly diagnostic of the amount and form of calcium in pyroxenes. This suggested further research on the sharpness and spectral placement of this feature in the spectra of Vesta and Vestoids (e.g., Cochran and Vilas, Icarus v. 134, 207, 1998). In 1997 and 1998, additional UV/blue spectra were obtained at the 2.7-m Harlan J. Smith telescope with a facility cassegrain spectrograph. These included spectra of low-albedo asteroids, the R-class asteroid 349 Dembowska, and the M-class asteroid 135 Hertha. These spectra will be presented and identified features will be discussed.

  13. Petawatt laser system for the fast ignition studies at ILE, Osaka University

    International Nuclear Information System (INIS)

    Izawa, Y.

    2002-01-01

    We have developed a PW Nd:glass laser system, which can deliver 1 PW output with 500 J in 0.5 ps, to study a fast ignitor concept in laser fusion. In the front end of this system, the optical parametric chirped-pulse amplifier (OPCPA) was introduced. The OPCPA solves several problems arising in an existing Ti:sapphire regenerative amplifier, such as low single-pass gain, high prepulse and output fluctuation. A booster amplifier is a Cassegrain-type three pass disk system having a 350 mm clear aperture, which generated 1.1 kJ output energy with the spectral width of 3.7 nm corresponding to 0.5 ps in Fourier transform limited pulse. The spatial phase aberration mainly caused in the booster amplifier is corrected using a deformable mirror. The laser pulse is compressed by a pair of 1-m diffraction gratings and focused by a parabolic mirror. The timing jitter between PW laser and GEKKO XII is less than 10 ps, which was attained by injecting a weak pulse splitted out from the front end into the preamplifier of GEKKO XII. (author)

  14. A NEXT GENERATION MULTI-BEAM FOCAL PLANE ARRAY RECEIVER OF TRAO FOR 86-115 GHZ BAND

    Directory of Open Access Journals (Sweden)

    Moon-Hee Chung

    2006-03-01

    Full Text Available The noise temperature of existing millimeter-wave receivers is already within two or three times quantum noise limit. One of practical ways to increase the observation speed of single dish radio telescope without longer integration time is use of multi-beam focal plane array receiver as demonstrated in several large single dish radio telescopes. In this context the TRAO (Taeduk Radio Astronomy Observatory, which operates a 143n Cassegrain radio telescope, is planning to develop a 4 x 4 beams focal plane array SIS receiver system for 86-115 GHz band. Even though millimeter-wave HEMT LNA-based receivers approach the noise temperature comparable to the SIS receiver at W-band, it is believed that the receiver based on SIS mixer seems to offer a bit more advantages. The critical part of the multi-beam array receiver will be sideband separating SIS mixers. Employing such a type of SIS mixer makes it possible to simplify the quasi-optics of receiver. Otherwise, an SSB filter should be used in front of the mixer or some sophisticated post-processing of observation data is needed. In this paper we will present a preliminary design concept and components needed for the development of a new 3 mm band multi-beam focal plane array receiver.

  15. Long-term performance potential of concentrated photovoltaic (CPV) systems

    KAUST Repository

    Burhan, Muhammad

    2017-07-17

    Owing to the diverse photovoltaic (PV) systems’ design and technology, as well as the dynamic nature of insolation data received on the aperture surfaces, the instantaneous output from a PV system fluctuates greatly. For accurate performance estimation of a large PV field, the long term performance as electrical output is a more rational approach over the conventional testing methods, such as at Standard Testing Conditions (STC) and at the Nominal Operating Cell Temperature (NOCT) available hitherto. In this paper, the long-term performances of concentrated PVs (Cassegrain reflectors and Fresnel lens) with 2-axes tracking and a variety of PV systems, namely the stationary flat-plate PV (mono-crystalline, poly-crystalline and thin-films CIS types), is presented over a period of one year for the merit comparison of system design, under the tropical weather conditions of Singapore. From the measured field performances, the total energy output of 240.2 kW h/m/year is recorded for CPV operation in Singapore, which is nearly two folds higher than the stationary PV panels.

  16. VizieR Online Data Catalog: Galactic outer disk: a field toward Tombaugh 1 (Carraro+, 2017)

    Science.gov (United States)

    Carraro, G.; Sales Silva, J. V.; Moni Bidin, C.; Vazquez, R. A.

    2018-04-01

    The region of interest has been observed with the Y4KCAM camera attached to the 1.0 m telescope operated by the SMARTS consortium (http://www.astro.yale.edu/smarts/) and located at the Cerro Tololo Inter-American Observatory (CTIO). This camera is equipped with an STA 4064x4064 CCD with 15 μm pixels, yielding a scale of 0.289"/pixel and a field of view (FOV) of 20'x20' at the Cassegrain focus of the CTIO 1.0 m telescope. The observational data were acquired on the night of 2008 January 30. We observed Landolt's SA 98 UBV(RI)KC standard star area (Landolt 1992AJ....104..372L) to tie our UBVRI instrumental system to the standard system. The average seeing was 1.0". During the nights of 2010 January 5, 6, 9, and 10, we observed 40 stars of the field toward the open cluster Tombaugh 1 (10 stars from boxes A and B, 11 stars from box C, and 9 stars from box D) on Cerro Manqui at the Las Campanas Observatory using the Inamori-Magellan Areal Camera & Spectrograph (IMACS; Dressler et al. 2006SPIE.6269E..0FD), attached to the 6.5 m Magellan Telescope. (7 data files).

  17. Analysis of polarization introduced due to the telescope optics of the Thirty Meter Telescope

    Science.gov (United States)

    Anche, Ramya Manjunath; Sen, Asoke Kumar; Anupama, Gadiyara Chakrapani; Sankarasubramanian, Kasiviswanathan; Skidmore, Warren

    2018-01-01

    An analytical model has been developed to estimate the polarization effects, such as instrumental polarization (IP), crosstalk (CT), and depolarization, due to the optics of the Thirty Meter Telescope. These are estimated for the unvignetted field-of-view and the wavelengths of interest. The model estimates an IP of 1.26% and a CT of 44% at the Nasmyth focus of the telescope at the wavelength of 0.6 μm at field angle zero with the telescope pointing to zenith. Mueller matrices have been estimated for the primary, secondary, and Nasmyth mirrors. It is found that some of the Mueller matrix elements of the primary and secondary mirrors show a fourfold azimuthal antisymmetry, which indicates that the polarization at the Cassegrain focus is negligible. At the inclined Nasmyth mirror, there is no azimuthal antisymmetry in the matrix elements, and this results in nonzero values for IP and CT, which would negatively impact the polarization measurements at the telescope focus. The averaged Mueller matrix is estimated at the Nasmyth focus at different instrument ports and various zenith angles of the telescope. The variation in the Mueller matrix elements for different coatings is also estimated. The impact of this polarization effect on the science case requirements has been discussed. This analysis will help in achieving precise requirements for future instruments with polarimetric capability.

  18. Kepler-77b: a very low albedo, Saturn-mass transiting planet around a metal-rich solar-like star

    Science.gov (United States)

    Gandolfi, D.; Parviainen, H.; Fridlund, M.; Hatzes, A. P.; Deeg, H. J.; Frasca, A.; Lanza, A. F.; Prada Moroni, P. G.; Tognelli, E.; McQuillan, A.; Aigrain, S.; Alonso, R.; Antoci, V.; Cabrera, J.; Carone, L.; Csizmadia, Sz.; Djupvik, A. A.; Guenther, E. W.; Jessen-Hansen, J.; Ofir, A.; Telting, J.

    2013-09-01

    We report the discovery of Kepler-77b (alias KOI-127.01), a Saturn-mass transiting planet in a 3.6-day orbit around a metal-rich solar-like star. We combined the publicly available Kepler photometry (quarters 1-13) with high-resolution spectroscopy from the Sandiford at McDonald and FIES at NOT spectrographs. We derived the system parameters via a simultaneous joint fit to the photometric and radial velocity measurements. Our analysis is based on the Bayesian approach and is carried out by sampling the parameter posterior distributions using a Markov chain Monte Carlo simulation. Kepler-77b is a moderately inflated planet with a mass of Mp = 0.430 ± 0.032 MJup, a radius of Rp = 0.960 ± 0.016 RJup, and a bulk density of ρp = 0.603 ± 0.055 g cm-3. It orbits a slowly rotating (Prot = 36 ± 6 days) G5 V star with M⋆ = 0.95 ± 0.04 M⊙, R⋆ = 0.99 ± 0.02 R⊙, Teff = 5520 ± 60 K, [M/H] = 0.20 ± 0.05 dex, that has an age of 7.5 ± 2.0 Gyr. The lack of detectable planetary occultation with a depth higher than ~10 ppm implies a planet geometric and Bond albedo of Ag ≤ 0.087 ± 0.008 and AB ≤ 0.058 ± 0.006, respectively, placing Kepler-77b among the gas-giant planets with the lowest albedo known so far. We found neither additional planetary transit signals nor transit-timing variations at a level of ~0.5 min, in accordance with the trend that close-in gas giant planets seem to belong to single-planet systems. The 106 transitsobserved in short-cadence mode by Kepler for nearly 1.2 years show no detectable signatures of the planet's passage in front of starspots. We explored the implications of the absence of detectable spot-crossing events for the inclination of the stellar spin-axis, the sky-projected spin-orbit obliquity, and the latitude of magnetically active regions. Based on observations obtained with the 2.1-m Otto Struve telescope at McDonald Observatory, Texas, USA.Based on observations obtained with the Nordic Optical Telescope, operated on the

  19. Experiments prior to construction of the Rapsodie reactor (1962); Experiences preliminaires a la construction de la pile rapsodie (1962)

    Energy Technology Data Exchange (ETDEWEB)

    Vautrey, L; Zaleski, C P [Commissariat a l' Energie Atomique, Cadarache (France). Centre d' Etudes Nucleaires

    1962-07-01

    ', maintes etudes experimentales, d'ordre hydraulique, thermique et mecanique ont ete faites ou sont envisagees pour verifier la validite des principes adoptes dans l'avant rojet. Ce memoire traite des plus importants: 1. Etudes d'elements de circuits de refroidissement: pompes a sodium (mecaniques ou electromagnetiques), eohangeurs Na-Nak et Nak-air, appareils de mesures (debits, temperatures), circuits de purification du sodium, etc. 2. Etudes de refroidissement des assemblages combustibles et fertiles; a) etude du refroidissement par le sodium, menee a l'aide de maquettes hydrauliques (echelle 1 ou superieure a 1), reproduisant l'ecoulement du fluide de refroidissement dans les tuyauteries, a l'amont des elements combustibles et fertiles et a l'interieur de ceux i; b) etude du refroidissement par gaz et par immersion dans le plomb, utilise pendant les operations de la manutention et de stockage. 3. Etudes de dispositifs speciaux du reacteur: joint tournant liquefiable, parties de mecanismes des barres de controle. 4. Etude du bloc pile et des circuits de refroidissement dans leur ensemble. Cette etude doit commencer a la fin de cette annee. Les installations, en cours d'achevement, reproduisent, a l'echelle 1, celles prevues dans le projet et comportent: le bloc pile auquel est associe un circuit de sodium a grand debit permettant les essais de duree et la realisation de chocs thermiques et, en annexe, un circuit d'essai de barres de controle; l'installation complete des circuits de refroidissement de 1 MW et de 10 MW dont les performances, dans les differents cas de fonctionnement, pourront etre verifiees. 5. Etude de securite effectuee sur une maquette a 1 echelle 3/10 de l'ensemble du bloc pile et de ses protections, dont l'objet est la limitation des consequences d'une hypothetique liberation d'energie accidentelle, d'allure explosive. (auteurs)

  20. Autoradiographic methods for studying marked volatile substances (1961); Methode.d'etude autoradiographique de substances marquees volatiles (1961)

    Energy Technology Data Exchange (ETDEWEB)

    Cohen, Y; Wepierre, J [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1961-07-01

    de Pellerin (1957) evite cette dessication, mais la comparaison a l'echelle histologique de l'autoradiographie avec le document biologique lui-meme est difficile sinon impossible. Cependant, nous nous sommes inspire de certains points de chacune des deux methodes pour proposer la technique suivante d'etude autoradiographique de molecules marquees volatiles: 1- nous preparons la surface du bloc congele a autoradiographier a l'aide d'un microtome a congelation; 2- la derniere coupe de 20 {mu} d'epaisseur, dont les elements histologiques font face a ceux du bloc, est dessechee au froid et sert de document biologique de reference a l'autoradiographie obtenue, comme il est indique en 3; 3- les films radiographiques sont appliques sur le bloc congele a -30 deg. C. Les autoradiographies correspondent a la radioactivite de la molecule volatile et de ses produits de degradation non volatils. 4- De plus, le film radiographique est applique sur la coupe de 20 {mu} prealablement dessechee a -20 deg. C. Cette autoradiographie correspond a la radioactivite des produits de degradation non volatils de la molecule. 5- Nous nous sommes assuree de l'absence de diffusion de la molecule volatile et d'effets pseudo-radiographiques (photochimiques et autres). Cette methode qui nous a permis d'etudier la distribution d'un carbure, le paracymene ({sup 14}C) 7 a l'echelle macroscopique sur la souris entiere et a l'echelle microscopique sur la peau de chien, est susceptible d'une application generale. (auteurs)

  1. Le modele de Hubbard bidimensionnel a faible couplage: Thermodynamique et phenomenes critiques

    Science.gov (United States)

    Roy, Sebastien

    Une etude systematique du modele de Hubbard en deux dimensions a faible couplage a l'aide de la theorie Auto-Coherente a Deux Particules (ACDP) dans le diagramme temperature-dopage-interaction-sauts permet de mettre en evidence l'influence des fluctuations magnetiques sur les proprietes thermodynamiques du systeme electronique sur reseau. Le regime classique renormalise a temperature finie pres du dopage nul est marque par la grandeur de la longueur de correlation de spin comparee a la longueur thermique de de Broglie et est caracterisee par un accroissement drastique de la longueur de correlation de spin. Cette croissance exponentielle a dopage nul marque la presence d'un pic de chaleur specifique en fonction de la temperature a basse temperature. Une temperature de crossover est alors associee a la temperature a laquelle la longueur de correlation de spin est egale a la longueur thermique de de Broglie. C'est a cette temperature caracteristique, ou est observee l'ouverture du pseudogap dans le poids spectral, que se situe le maximum du pic de chaleur specifique. La presence de ce pic a des consequences sur l'evolution du potentiel chimique avec le dopage lorsque l'uniformite thermodynamique est respectee. Les contraintes imposees par les lois de la thermodynamique font en sorte que l'evolution du potentiel chimique avec le dopage est non triviale. On demontre entre autres que le potentiel chimique est proportionnel a la double occupation qui est reliee au moment local. Par ailleurs, une derivation de la fonction de mise a l'echelle de la susceptibilite de spin a frequence nulle au voisinage d'un point critique marque sans equivoque la presence d'un point critique quantique en dopage pour une valeur donnee de l'interaction. Ce point critique, associe a une transition de phase magnetique en fonction du dopage a temperature nulle, induit un comportement non trivial sur les proprietes physiques du systeme a temperature finie. L'approche quantitative ACDP permet de

  2. Studying the Mars atmosphere using a SOIR Instrument

    Science.gov (United States)

    Drummond, R.; Vandaele, A.; Daerden, F.; Neefs, E.; Mahieux, A.; Wilquet, V.; Montmessin, F.; Bertaux, J.; McConnell, J. C.; Kaminski, J. W.

    2009-05-01

    SOIR (Solar Occultation InfraRed spectrometer) is currently part of the SPICAV/SOIR instrument on board the Venus Express orbiter (VEX). SOIR, an Echelle infrared spectrometer using an acousto-optic tunable filter (AOTF) for the order selection, is probing the atmosphere by solar occultation, operating between 2.2 and 4.3 μm, with a resolution of 0.15 cm-1. This spectral range is suitable for the detection of several key components of planetary atmospheres, including H2O and its isotopologue HDO, CH4 and other trace species. The SOIR instrument was designed to have a minimum of moving parts, to be light and compact in order to fit on top of the SPICAV instrument. The AOTF allows a narrow range of wavelengths to pass, according to the radio frequency applied to the TeO2 crystal; this selects the order. The advantage of the AOTF is that different orders can be observed quickly and easily during one occultation. To obtain a compact optical scheme, a Littrow configuration was implemented in which the usual collimating and imaging lenses are merged into a single off-axis parabolic mirror. The light is diffracted on the echelle grating, where orders overlap and addition occurs, and finally is recorded by the detector. The detector is 320x256 pixels and is cooled to 88K during an occultation measurement, to maximise the signal to noise ratio. SOIR on VEX has been in orbit around Venus since April 2006, allowing us to characterise the instrument and study its performance. These data have allowed the engineering team to devise several instrumental improvements. The next step in further improving the readiness for Martian atmospheric studies comes in close collaboration with the Mars Atmospheric Modelling group at BIRA-IASB. A General Circulation Model is used to simulate the Martian atmosphere. Currently work is underway with SPICAM data to verify the GCM inputs and outputs. Later the GCM output will be used as feedback for instrumental design of both an improved version

  3. Structure of the marine atmospheric boundary layer over an oceanic thermal front: SEMAPHORE experiment

    Science.gov (United States)

    Kwon, B. H.; BéNech, B.; Lambert, D.; Durand, P.; Druilhet, A.; Giordani, H.; Planton, S.

    1998-10-01

    The Structure des Echanges Mer-Atmosphere, Proprietes des Heterogeneites Oceaniques: Recherche Experimentale (SEMAPHORE) experiment, the third phase of which took place between October 4 and November 17, 1993, was conducted over the oceanic Azores Current located in the Azores basin and mainly marked at the surface by a thermal front due to the gradient of the sea surface temperature (SST) of about 1° to 2°C per 100 km. The evolution of the marine atmospheric boundary layer (MABL) over the SST front was studied with two aircraft and a ship in different meteorological conditions. For each case, the influence of the incoming air direction with respect to the orientation of the oceanic front was taken into account. During the campaign, advanced very high resolution radiometer pictures did not show any relation between the SST field and the cloud cover. The MABL was systematically thicker on the warm side than on the cold side. The mean MABL structure described from aircraft data collected in a vertical plane crossing the oceanic front was characterized by (1) an atmospheric horizontal gradient of 1° to 2°C per 100 km in the whole depth of the mixed layer and (2) an increase of the wind intensity from the cold to the warm side when the synoptic wind blew from the cold side. The surface sensible heat (latent heat) flux always increased from the cold to the warm sector owing to the increase of the wind and of the temperature (specific humidity) difference between the surface and the air. Turbulence increased from the cold to the warm side in conjunction with the MABL thickening, but the normalized profiles presented the same structure, regardless of the position over the SST front. In agreement with the Action de Recherche Programme te Petite Echelle and Grande Echelle model, the mean temperature and momentum budgets were highly influenced by the horizontal temperature gradient. In particular, the strong ageostrophic influence in the MABL above the SST front seems

  4. Study of the aqueous chemical treatment of uranium zirconium fuels; Etude du traitement chimique des combustibles uraniumzirconium par voie seche

    Energy Technology Data Exchange (ETDEWEB)

    Bourgeois, M; Nollet, P [Commissariat a l' Energie Atomique, Fontenay-aux-Roses (France). Centre d' Etudes Nucleaires

    1964-07-01

    A dry process has been studied for separating the uranium from the zirconium-either for recovering the enriched uranium from fuel element production waste, or with a view to treating this waste after irradiation. In this process the alloy is treated with hydrochloric acid at 400 deg. C in a fluidized corundum bed which causes the zirconium to volatilize as tetrachloride and the uranium to form the trichloride. This latter is then converted to the hexafluoride by attack with fluorure. After the laboratory tests, a first pilot plant with a capacity of 1 kg of alloy was tried out at the Fontenay-aux-Roses Nuclear Research Centre; this made it possible to fix the operational conditions for the process. An industrial scale plant was then built with the collaboration of the from Kuhlmann, and operated until a satisfactory process had been developed for treating the waste. This installation treats 3 kg/h of alloy with a yield for the hydrochloric acid of about 50 per cent and with a uranium loss in the zirconium tetrachloride of about 0.1 per cent. An active pilot plant capable of treating of treating a few kilos of irradiated alloy is now being studied. (authors) [French] On a etudie un procede de voie seche pour effectuer la separation de l'uranium et du zirconium - soit en vue de la recuperation de l'uranium enrichi contenu dans les dechets de fabrication des elements combustibles - soit en vue du traitement de ceux-ci apres irradiation. Ce procede consiste a attaquer l'alliage par l'acide chlorhydrique a 400 deg. C dans un lit fluidise de corindon, ce qui a pour effet de volatiliser le zirconium sous forme de tetrachlorure et de transformer l'uranium en trichlorure. Ce dernier est ensuite converti en hexafluorure par action du fluor. Apres des essais de laboratoire, un premier pilote a l'echelle de 1 kg d'alliage a ete experimente au Centre d'Etudes Nucleaires de Fontenay-aux-Roses et a permis de determiner les conditions operatoires du procede. En collaboration avec

  5. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

    Science.gov (United States)

    Korablev, O.; Montmessin, F.; Trokhimovskiy, A.; Fedorova, A. A.; Shakun, A. V.; Grigoriev, A. V.; Moshkin, B. E.; Ignatiev, N. I.; Forget, F.; Lefèvre, F.; Anufreychik, K.; Dzuban, I.; Ivanov, Y. S.; Kalinnikov, Y. K.; Kozlova, T. O.; Kungurov, A.; Makarov, V.; Martynovich, F.; Maslov, I.; Merzlyakov, D.; Moiseev, P. P.; Nikolskiy, Y.; Patrakeev, A.; Patsaev, D.; Santos-Skripko, A.; Sazonov, O.; Semena, N.; Semenov, A.; Shashkin, V.; Sidorov, A.; Stepanov, A. V.; Stupin, I.; Timonin, D.; Titov, A. Y.; Viktorov, A.; Zharkov, A.; Altieri, F.; Arnold, G.; Belyaev, D. A.; Bertaux, J. L.; Betsis, D. S.; Duxbury, N.; Encrenaz, T.; Fouchet, T.; Gérard, J.-C.; Grassi, D.; Guerlet, S.; Hartogh, P.; Kasaba, Y.; Khatuntsev, I.; Krasnopolsky, V. A.; Kuzmin, R. O.; Lellouch, E.; Lopez-Valverde, M. A.; Luginin, M.; Määttänen, A.; Marcq, E.; Martin Torres, J.; Medvedev, A. S.; Millour, E.; Olsen, K. S.; Patel, M. R.; Quantin-Nataf, C.; Rodin, A. V.; Shematovich, V. I.; Thomas, I.; Thomas, N.; Vazquez, L.; Vincendon, M.; Wilquet, V.; Wilson, C. F.; Zasova, L. V.; Zelenyi, L. M.; Zorzano, M. P.

    2018-02-01

    The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7-1.6 μm spectral range with a resolving power of ˜20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2-4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7-17 μm with apodized resolution varying from 0.2 to 1.3 cm-1. TIRVIM is primarily dedicated to profiling temperature from the surface up to ˜60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of

  6. The opto-mechanical design of the GMT-Consortium Large Earth Finder (G-CLEF)

    Science.gov (United States)

    Mueller, Mark; Szentgyorgyi, Andrew; Baldwin, Daniel; Bean, Jacob; Ben-Ami, Sagi; Brennan, Patricia; Budynkiewicz, J.; Chun, Moo-Yung; Crane, Jeffrey D.; Epps, Harland; Evans, Ian; Evans, Janet; Foster, Jeff; Frebel, Anna; Gauron, Thomas; Glenday, Alex; Hare, Tyson; Jang, Bi-Ho; Jang, Jeong-Gyun; Jordan, Andreas; Kim, Jihun; Kim, Kang-Min; Mendes de Oliveira, Claudia; Lopez-Morales, Mercedes; McCracken, Kenneth; McMuldroch, Stuart; Miller, Joseph; Oh, Jae Sok; Onyuksel, Cem; Ordway, Mark; Park, Chan; Park, Sung-Joon; Paxson, Charles; Phillips, David; Plummer, David; Podgorski, William; Seifahrt, Andreas; Steiner, Joao; Uomoto, Alan; Walsworth, Ronald; Yu, Young-Sam

    2016-08-01

    The GMT-Consortium Large Earth Finder (G-CLEF) is a fiber-fed, optical echelle spectrograph selected as the first light instrument for the Giant Magellan Telescope (GMT) now under construction at the Las Campanas Observatory in Chile. G-CLEF has been designed to be a general-purpose echelle spectrograph with precision radial velocity (PRV) capability for exoplanet detection. The radial velocity (RV) precision goal of G-CLEF is 10 cm/sec, necessary for detection of Earth-sized exoplanets. This goal imposes challenging stability requirements on the optical mounts and the overall spectrograph support structures especially when considering the instrument's operational environment. The accuracy of G-CLEF's PRV measurements will be influenced by minute changes in temperature and ambient air pressure as well as vibrations and micro gravity-vector variations caused by normal telescope slewing. For these reasons we have chosen to enclose G-CLEF's spectrograph in a well-insulated, vibration isolated vacuum chamber in a gravity invariant location on GMT's azimuth platform. Additional design constraints posed by the GMT telescope include: a limited space envelope, a thermal emission ceiling, and a maximum weight allowance. Other factors, such as manufacturability, serviceability, available technology and budget are also significant design drivers. All of the above considerations must be managed while ensuring performance requirements are achieved. In this paper, we discuss the design of G-CLEF's optical mounts and support structures including the choice of a low coefficient of thermal expansion (CTE) carbon-fiber optical bench to minimize the system's sensitivity to thermal soaks and gradients. We discuss design choices made to the vacuum chamber geared towards minimize the influence of daily ambient pressure variations on image motion during observation. We discuss the design of G-CLEF's insulated enclosure and thermal control systems which will maintain the spectrograph at

  7. Controle optique de qubits lies a des centres isoelectroniques d'azote dans le GaAs

    Science.gov (United States)

    Ethier-Majcher, Gabriel

    Le traitement de l'information quantique est un domaine de recherche actuellement en pleine effervescence car il laisse entrevoir une revolution dans notre facon de traiter et d'echanger de l'information. D'une part, l'ordinateur quantique promet de resoudre des problemes comme la factorisation d'un polynome de facon beaucoup plus efficace qu'un ordinateur classique. D'autre part, les communications quantiques promettent l'echange d'information de facon fondamentalement inviolable. Afin de tirer pleinement profit de ces nouvelles technologies, il sera avantageux de construire des reseaux quantiques. Dans un tel reseau, des processeurs quantiques, les noeuds, seront connectes par des photons voyageant dans des fibres optiques. Les reseaux quantiques permettront de deployer les communications quantiques a grande echelle et de creer des super-ordinateurs quantiques. La realisation de reseaux quantiques necessitera des interfaces optiques pouvant echanger l'information de facon coherente entre un qubit (bit d'information quantique) et un photon. L'implementation de telles interfaces dans un systeme physique s'avere un important defi scientifique et technologique. Or, les systemes actuellement envisages a cette fin souffrent d'un faible couplage avec la lumiere ou encore de grandes inhomogeneites, constituant des obstacles a la realisation de reseaux a grande echelle. Dans cette these, le potentiel des centres isoelectroniques pour realiser des interfaces optiques est evalue. Deux types de qubits lies a des paires d'azote dans le GaAs sont consideres : les qubits excitoniques et les qubits de spin electronique, controlables par l'intermediaire d'excitons charges. Le controle optique complet des qubits excitoniques est demontre, ce qui constitue la premiere realisation du genre dans les centres isoelectroniques. L'observation d'excitons charges dans ce systeme, liant a la fois des trous lourds et des trous legers, laisse entrevoir de nouvelles possibilites afin de

  8. VizieR Online Data Catalog: Radial velocity curve of 51 Peg (Birkby+, 2017)

    Science.gov (United States)

    Birkby, J. L.; de Kok, R. J.; Brogi, M.; Schwarz, H.; Snellen, I. A. G.

    2017-07-01

    We observed the bright star 51 Peg (G2.5V, V=5.46mag, K=3.91mag) for 3.7hr during the night beginning 2010 October 21, using the CRyogenic InfraRed Echelle Spectrograph (CRIRES) mounted at Nasmyth A at the VLT (8.2 m UT1/Antu), Cerro Paranal, Chile. The observations were collected as part of the ESO large program 186.C-0289. The instrument setup consisted of a 0.2 arcsec slit centred on 3236nm (order 17), in combination with the Multi-Application Curvature Adaptive Optic system (MACAO). The CRIRES infrared detector is comprised of four Aladdin III InSb-arrays, each with 1024*512 pixels, and separated by a gap of 280 pixels. The resulting wavelength coverage of the observations was 3.1806R{approx}100000 per resolution element. We observed 51 Peg continuously while its hot Jupiter companion passed through orbital phases 0.55data are given in Table 1 and span observing dates from 1994 September 15 to 2014 July 9, resulting in 639 radial velocity measurements over 20 years. The table includes the discovery measurements from the ELODIE spectrograph at Observatoire Haute Provence and subsequent additional monitoring. We took these radial velocity measurements from the Naef et al. 2004 (Cat. J/A+A/414/351) compilation. We also included the legacy data set from Lick Observatory observed with the Hamilton spectrograph, taking measurements from the self-consistent reprocessing of all the Lick spectra presented by Fischer et al. 2014 (Cat. J/ApJS/210/5). Finally, we included more recent additional monitoring from the High Resolution Echelle Spectrometer (HIRES) at the Keck Observatory, and extracted RVs from observations with the High Accuracy Radial velocity Planet Searcher (HARPS) at the ESO-3.6m telescope in 2013 (ESO program ID 091.C-0271, PI: Santos). The reduced HARPS spectra were obtained from the ESO Science Archive (http://archive.eso.org/wdb/wdb/adp/phase3_spectral/query). (1 data file).

  9. The opto-mechanical design of the GMT-consortium large earth finder (G-CLEF)

    Science.gov (United States)

    Mueller, Mark; Baldwin, Daniel; Bean, Jacob; Bergner, Henry; Bigelow, Bruce; Chun, Moo-Young; Crane, Jeffrey; Foster, Jeff; Fżrész, Gabor; Gauron, Thomas; Guzman, Dani; Hertz, Edward; Jordán, Andrés.; Kim, Kang-Min; McCracken, Kenneth; Norton, Timothy; Ordway, Mark; Park, Chan; Park, Sang; Podgorski, William A.; Szentgyorgyi, Andrew; Uomoto, Alan; Yuk, In-Soo

    2014-08-01

    The GMT-Consortium Large Earth Finder (G-CLEF) is a fiber fed, optical echelle spectrograph that has been selected as a first light instrument for the Giant Magellan Telescope (GMT) currently under construction at the Las Campanas Observatory in Chile's Atacama desert region. We designed G-CLEF as a general-purpose echelle spectrograph with precision radial velocity (PRV) capability used for exoplanet detection. The radial velocity (RV) precision goal of GCLEF is 10 cm/sec, necessary for detection of Earth-sized planets orbiting stars like our Sun in the habitable zone. This goal imposes challenging stability requirements on the optical mounts and the overall spectrograph support structures. Stability in instruments of this type is typically affected by changes in temperature, orientation, and air pressure as well as vibrations caused by telescope tracking. For these reasons, we have chosen to enclose G-CLEF's spectrograph in a thermally insulated, vibration isolated vacuum chamber and place it at a gravity invariant location on GMT's azimuth platform. Additional design constraints posed by the GMT telescope include: a limited space envelope, a thermal emission ceiling, and a maximum weight allowance. Other factors, such as manufacturability, serviceability, available technology and budget are also significant design drivers. All of the previously listed considerations must be managed while ensuring that performance requirements are achieved. In this paper, we discuss the design of G-CLEF's optical mounts and support structures including technical choices made to minimize the system's sensitivity to thermal gradients. A more general treatment of the properties of G-CLEF can be found elsewhere in these proceedings1. We discuss the design of the vacuum chamber which houses the irregularly shaped optical bench and optics while conforming to a challenging space envelope on GMT's azimuth platform. We also discuss the design of G-CLEF's insulated enclosure and thermal

  10. Modelling the structure and kinematics of the Firework nebula: The nature of the GK Persei nova shell and its jet-like feature

    Science.gov (United States)

    Harvey, E.; Redman, M. P.; Boumis, P.; Akras, S.

    2016-10-01

    Aims: The shaping mechanisms of old nova remnants are probes for several important and unexplained processes, such as dust formation and the structure of evolved star nebulae. To gain a more complete understanding of the dynamics of the GK Per (1901) remnant, an examination of symmetry of the nova shell is explored, followed by a kinematical analysis of the previously detected jet-like feature in the context of the surrounding fossil planetary nebula. Methods: Faint-object high-resolution echelle spectroscopic observations and imaging were undertaken covering the knots which comprise the nova shell and the surrounding nebulosity. New imaging from the Aristarchos telescope in Greece and long-slit spectra from the Manchester Echelle Spectrometer instrument at the San Pedro Mártir observatory in Mexico were obtained, supplemented with archival observations from several other optical telescopes. Position-velocity arrays are produced of the shell, and also individual knots, and are then used for morpho-kinematic modelling with the shape code. The overall structure of the old knotty nova shell of GK Per and the planetary nebula in which it is embedded is then analysed. Results: Evidence is found for the interaction of knots with each other and with a wind component, most likely the periodic fast wind emanating from the central binary system. We find that a cylindrical shell with a lower velocity polar structure gives the best model fit to the spectroscopy and imaging. We show in this work that the previously seen jet-like feature is of low velocity. Conclusions: The individual knots have irregular tail shapes; we propose here that they emanate from episodic winds from ongoing dwarf nova outbursts by the central system. The nova shell is cylindrical, not spherical, and the symmetry axis relates to the inclination of the central binary system. Furthermore, the cylinder axis is aligned with the long axis of the bipolar planetary nebula in which it is embedded. Thus, the

  11. Reconnaissance invariante d'objets 3-D et correlation SONG

    Science.gov (United States)

    Roy, Sebastien

    Cette these propose des solutions a deux problemes de la reconnaissance automatique de formes: la reconnaissance invariante d'objets tridimensionnels a partir d'images d'intensite et la reconnaissance robuste a la presence de bruit disjoint. Un systeme utilisant le balayage angulaire des images et un classificateur par trajectoires d'espace des caracteristiques permet d'obtenir la reconnaissance invariante d'objets tridimensionnels. La reconnaissance robuste a la presence de bruit disjoint est realisee au moyen de la correlation SONG. Nous avons realise la reconnaissance invariante aux translations, rotations et changements d'echelle d'objets tridimensionnels a partir d'images d'intensite segmentees. Nous utilisons le balayage angulaire et un classificateur a trajectoires d'espace des caracteris tiques. Afin d'obtenir l'invariance aux translations, le centre de balayage angulaire coincide avec le centre geometrique de l'image. Le balayage angulaire produit un vecteur de caracteristiques invariant aux changements d'echelle de l'image et il transforme en translations du signal les rotations autour d'un axe parallele a la ligne de visee. Le classificateur par trajectoires d'espace des caracteristiques represente une rotation autour d'un axe perpendiculaire a la ligne de visee par une courbe dans l'espace. La classification se fait par la mesure de la distance du vecteur de caracteristiques de l'image a reconnaitre aux trajectoires stockees dans l'espace. Nos resultats numeriques montrent un taux de classement atteignant 98% sur une banque d'images composee de 5 vehicules militaires. La correlation non-lineaire generalisee en tranches orthogonales (SONG) traite independamment les niveaux de gris presents dans une image. Elle somme les correlations lineaires des images binaires ayant le meme niveau de gris. Cette correlation est equivalente a compter le nombre de pixels situes aux memes positions relatives et ayant les memes intensites sur deux images. Nous presentons

  12. Elaboration de nouvelles approches micromecaniques pour l'optimisation des performances mecaniques des materiaux heterogenes

    Science.gov (United States)

    Aboutajeddine, Ahmed

    Les modeles micromecaniques de transition d'echelles qui permettent de determiner les proprietes effectives des materiaux heterogenes a partir de la microstructure sont consideres dans ce travail. L'objectif est la prise en compte de la presence d'une interphase entre la matrice et le renforcement dans les modeles micromecaniques classiques, de meme que la reconsideration des approximations de base de ces modeles, afin de traiter les materiaux multiphasiques. Un nouveau modele micromecanique est alors propose pour tenir compte de la presence d'une interphase elastique mince lors de la determination des proprietes effectives. Ce modele a ete construit grace a l'apport de l'equation integrale, des operateurs interfaciaux de Hill et de la methode de Mori-Tanaka. Les expressions obtenues pour les modules globaux et les champs dans l'enrobage sont de nature analytique. L'approximation de base de ce modele est amelioree par la suite dans un nouveau modele qui s'interesse aux inclusions enrobees avec un enrobage mince ou epais. La resolution utilisee s'appuie sur une double homogeneisation realisee au niveau de l'inclusion enrobee et du materiau. Cette nouvelle demarche, permettra d'apprehender completement les implications des approximations de la modelisation. Les resultats obtenus sont exploites par la suite dans la solution de l'assemblage de Hashin. Ainsi, plusieurs modeles micromecaniques classiques d'origines differentes se voient unifier et rattacher, dans ce travail, a la representation geometrique de Hashin. En plus de pouvoir apprecier completement la pertinence de l'approximation de chaque modele dans cette vision unique, l'extension correcte de ces modeles aux materiaux multiphasiques est rendue possible. Plusieurs modeles analytiques et explicites sont alors proposee suivant des solutions de differents ordres de l'assemblage de Hashin. L'un des modeles explicite apparait comme une correction directe du modele de Mori-Tanaka, dans les cas ou celui ci echoue a

  13. Study of the consequences of the rupture of a pressure tube in the tank of a gas-cooled, heavy-water moderated reactor; Etude des consequences de la rupture d'un tube de force dans la cuve d'un reacteur modere a l'eau lourde et refroidi au gaz

    Energy Technology Data Exchange (ETDEWEB)

    Hareux, F; Roche, R; Vrillon, B [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1964-07-01

    Bursting of a pressure tube in the tank of a heavy water moderated-gas cooled reactor is an accident which has been studied experimentally about EL-4. A first test (scale 1) having shown that the burst of a tube does not cause the rupture of adjacent tubes, tests on the tank resistance have been undertaken with a very reduced scale model (1 to 10). It has been found that the tank can endure many bursts of tube without any important deformation. Transient pressure in the tank is an oscillatory weakened wave, the maximum of which (pressure peak) has been the object of a particular experimental study. It appears that the most important parameters which affect the pressure peak are; the pressure of the gas included in the bursting pressure tube, the volume of this gas, the mass of air included in the tank and the nature of the gas. A general method to calculate the pressure peak value in reactor tanks has been elaborated by direct application of experimental data. (authors) [French] L'eclatement d'un tube de force dans la cuve d'un reacteur de puissance modere a l'eau lourde et refroidi par un gaz sous pression est un accident qui a ete etudie experimentalement a propos d'EL-4. Un premier essai a l'echelle 1 ayant montre que l'eclatement d'un tube ne provoque pas celui des tubes voisins, des essais relatifs a la tenue de la cuve ont ete effectues sur maquettes a echelle tres reduite (l/lO). Il a ete trouve que la cuve peut supporter plusieurs eclatements de tubes sans deformations notables. La pression transitoire dans la cuve a une allure oscillatoire amortie dont le maximum (pression de pic) a fait l'objet d'une etude experimentale detaillee. Il apparait que les parametres essentiels influant sur cette pression sont: la pression du gaz contenu dans le tube de force, le volume du gaz qui participe a l'eclatement, la flexibilite de la cuve, la masse d'air empoisonnee dans la cuve, la nature du gaz explosant. Une methode generale d'estimation des pics de pression dans

  14. San Pedro Martir Telescope: Mexican design endeavor

    Science.gov (United States)

    Toledo-Ramirez, Gengis K.; Bringas-Rico, Vicente; Reyes, Noe; Uribe, Jorge; Lopez, Aldo; Tovar, Carlos; Caballero, Xochitl; Del-Llano, Luis; Martinez, Cesar; Macias, Eduardo; Lee, William; Carramiñana, Alberto; Richer, Michael; González, Jesús; Sanchez, Beatriz; Lucero, Diana; Manuel, Rogelio; Segura, Jose; Rubio, Saul; Gonzalez, German; Hernandez, Obed; García, Mary; Lazaro, Jose; Rosales-Ortega, Fabian; Herrera, Joel; Sierra, Gerardo; Serrano, Hazael

    2016-08-01

    The Telescopio San Pedro Martir (TSPM) is a new ground-based optical telescope project, with a 6.5 meters honeycomb primary mirror, to be built in the Observatorio Astronomico Nacional on the Sierra San Pedro Martir (OAN-SPM) located in Baja California, Mexico. The OAN-SPM has an altitude of 2830 meters above sea level; it is among the best location for astronomical observation in the world. It is located 1830 m higher than the atmospheric inversion layer with 70% of photometric nights, 80% of spectroscopic nights and a sky brightness up to 22 mag/arcsec2. The TSPM will be suitable for general science projects intended to improve the knowledge of the universe established on the Official Mexican Program for Science, Technology and Innovation 2014-2018. The telescope efforts are headed by two Mexican institutions in name of the Mexican astronomical community: the Universidad Nacional Autonoma de Mexico and the Instituto Nacional de Astrofisica, Optica y Electronica. The telescope has been financially supported mainly by the Consejo Nacional de Ciencia y Tecnologia (CONACYT). It is under development by Mexican scientists and engineers from the Center for Engineering and Industrial Development. This development is supported by a Mexican-American scientific cooperation, through a partnership with the University of Arizona (UA), and the Smithsonian Astrophysical Observatory (SAO). M3 Engineering and Technology Corporation in charge of enclosure and building design. The TSPM will be designed to allow flexibility and possible upgrades in order to maximize resources. Its optical and mechanical designs are based upon those of the Magellan and MMT telescopes. The TSPM primary mirror and its cell will be provided by the INAOE and UA. The telescope will be optimized from the near ultraviolet to the near infrared wavelength range (0.35-2.5 m), but will allow observations up to 26μm. The TSPM will initially offer a f/5 Cassegrain focal station. Later, four folded Cassegrain and

  15. CosmoQuest: Virtual Star Parties as a Conduit to Citizen Science Research

    Science.gov (United States)

    Lewis, Scott; Gugliucci, N. E.; Gay, P. L.; Amateur Astronomer Team; Commentator Team

    2013-01-01

    CosmoQuest has created an environment that actively engages the public through online star parties while building a growing virtual research center that allows individuals anywhere in the world to participate in and contribute to scientific research. Utilizing the infrastructure of Google+ and YouTube, CosmoQuest has brought optical observational astronomy into homes across the world. Every week astronomers - amateur and professional - meet to share live sky images and to discuss the science behind their beauty during Virtual Star parties. A wide array of optics and digital detectors from varied locations collaborate in a fashion not possible in the standard public star party. Every viewer is able to virtually look through the imaging telescope simultaneously while the equipment owner doesn’t need to worry about accidental mishandling by the public. Digital cameras and CCDs also allow longer exposures of deep-sky objects, something not typical in a standard star party event. Our diversity of equipment - ranging from hand-guided Dobsonian telescopes to 16” Schmidt-Cassegrain telescopes on Paramounts - give viewers the opportunity to experience the sky through different systems. Additional Star Parties focus on special astronomical events, such as eclipses and transits. The annular eclipse of 20 May, 2012 brought together astronomers, space enthusiasts and a curious public into a Google+ Hangout On Air to celebrate the event while advocating safe observing methods and explaining the science behind the phenomenon. Public photos of the eclipse were shared live in the broadcast while video of the event was streamed for thousands of viewers to enjoy. Other special event star parties have focused on the Super Moon, Eros Opposition, and the Venus Transit. In this poster we review the technology behind star parties and the reach of these events.

  16. 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

  17. 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

  18. Mesospheric Na Variability and Dependence on Geomagnetic and Solar Activity over Arecibo

    Science.gov (United States)

    Jain, K.; Raizada, S.; Brum, C. G. M.

    2017-12-01

    The Sodium (Na) resonance lidars located at the Arecibo Observatory offer an excellent opportunity to study the mesosphere/lower thermosphere(MLT) region. Different metals like Fe, Mg, Na, K, Ca and their ions are deposited in the 80 - 120 km altitude range due to the ablation of meteors caused by frictional heating during their entry into the Earth's atmosphere. We present an investigation of the neutral mesospheric Na atom layers over Arecibo. Data on the Na concentrations was collected using a resonance lidar tuned to the of Na wavelength at 589 nm. This wavelength is achieved with a dye-laser pumped by the second harmonic (532 nm) generated from a state-of-the-art commercial Nd:YAG laser. The backscattered signal is received on a 0.8 m (diameter) Cassegrain telescope. The study is based on this data acquired from 1998-2017 and its relation to variations in geomagnetic and solar conditions. We also investigate seasonal and long term trends in the data. The nightly-averaged altitude profiles were modeled as Gaussian curves. From this modeled data we obtain parameters such as the peak, abundance, centroid and width of the main Na layer. Preliminary results show that the Na abundance is more sensitive to changes in geomagnetic and solar variations as compared to the width and centroid height. The seasonal variation exhibits higher peak densities during the local summer and has a secondary maximum during the winter [as shown in the attached figure]. Our analysis demonstrates a decrease in the peak and the abundance of Na atoms with the increase of solar and geomagnetic activity.

  19. Recent Advances and Achievements at The Catalina Sky Survey

    Science.gov (United States)

    Leonard, Gregory J.; Christensen, Eric J.; Fuls, Carson; Gibbs, Alex; Grauer, Al; Johnson, Jess A.; Kowalski, Richard; Larson, Stephen M.; Matheny, Rose; Seaman, Rob; Shelly, Frank

    2017-10-01

    The Catalina Sky Survey (CSS) is a NASA-funded project fully dedicated to discover and track near-Earth objects (NEOs). Since its founding nearly 20 years ago CSS remains at the forefront of NEO surveys, and recent improvements in both instrumentation and software have increased both survey productivity and data quality. In 2016 new large-format (10K x 10K) cameras were installed on both CSS survey telescopes, the 1.5-m reflector and the 0.7-m Schmidt, increasing the field of view, and hence nightly sky coverage by 4x and 2.4x respectively. The new cameras, coupled with improvements in the reduction and detection pipelines, and revised sky-coverage strategies have yielded a dramatic upward trend of NEO discovery rates. CSS has also developed a custom adaptive queue manager for scheduling NEO follow-up astrometry using a remotely operated and recently renovated 1-m Cassegrain reflector telescope, improvements that have increased the production of follow-up astrometry for newly discovered NEOs and arc extensions for previously discovered objects by CSS and other surveys. Additionally, reprocessing of archival CSS data (which includes some 46 million individual astrometric measurements) through the new reduction and detection pipeline will allow for improved orbit determinations and increased arc extensions for hundreds of thousands of asteroids. Reprocessed data will soon feed into a new public archive of CSS images and catalog data products made available through NASA’s Planetary Data System (PDS). For the future, CSS is working towards improved NEO follow-up capabilities through a combination of access to larger telescopes, instrument upgrades and follow-up scheduling tools.

  20. Large Aperture "Photon Bucket" Optical Receiver Performance in High Background Environments

    Science.gov (United States)

    Vilnrotter, Victor A.; Hoppe, D.

    2011-01-01

    The potential development of large aperture groundbased "photon bucket" optical receivers for deep space communications, with acceptable performance even when pointing close to the sun, is receiving considerable attention. Sunlight scattered by the atmosphere becomes significant at micron wavelengths when pointing to a few degrees from the sun, even with the narrowest bandwidth optical filters. In addition, high quality optical apertures in the 10-30 meter range are costly and difficult to build with accurate surfaces to ensure narrow fields-of-view (FOV). One approach currently under consideration is to polish the aluminum reflector panels of large 34-meter microwave antennas to high reflectance, and accept the relatively large FOV generated by state-of-the-art polished aluminum panels with rms surface accuracies on the order of a few microns, corresponding to several-hundred micro-radian FOV, hence generating centimeter-diameter focused spots at the Cassegrain focus of 34-meter antennas. Assuming pulse-position modulation (PPM) and Poisson-distributed photon-counting detection, a "polished panel" photon-bucket receiver with large FOV will collect hundreds of background photons per PPM slot, along with comparable signal photons due to its large aperture. It is demonstrated that communications performance in terms of PPM symbol-error probability in high-background high-signal environments depends more strongly on signal than on background photons, implying that large increases in background energy can be compensated by a disproportionally small increase in signal energy. This surprising result suggests that large optical apertures with relatively poor surface quality may nevertheless provide acceptable performance for deep-space optical communications, potentially enabling the construction of cost-effective hybrid RF/optical receivers in the future.

  1. VizieR Online Data Catalog: SEAMBHs. I. Mrk 142, Mrk 335, and IRAS F12397+3333 (Du+, 2014)

    Science.gov (United States)

    Du, P.; Hu, C.; Lu, K.-X.; Wang, F.; Qiu, J.; Li, Y.-R.; Bai, J.-M.; Kaspi, S.; Netzer, H.; Wang, J.-M.; SEAMBH Collaboration

    2016-03-01

    All the spectroscopy and imaging observations reported here were obtained with the Shangri-La telescope (SLT: IAU site code O44) at the Lijiang Station of the Yunnan Observatory of the Chinese Academy of Sciences. The SLT started its operation in 2008. This is a 2.4m alt-azimuth mounted Ritchey-Chretien telescope. The rms pointing error is about 2arcsec rms, and the tracking accuracy with autoguiding is better than 0.5''/hr. The longitude of the station is 100°01'51''E, the latitude 26°42'32''N, and the altitude 3193m. The annually averaged seeing is ~1.5'' in terms of the FWHM of stars (measured with Yunnan Faint Object Spectrograph and Camera, YFOSC), ranging from 0.7'' to 2.0''. The YFOSC, built in 2010 by the astronomical instrumentation team at the Niels Bohr Institute, is similar to the ESO Faint Object Spectrograph and Camera, but with an additional focal reducer. It started its operation in 2011. YFOSC is a versatile instrument for low resolution spectroscopy and imaging, working at the Cassegrain focus. The CCD chip is an e2v CCD42-90 Back Illuminated Deep Depletion 2048*4608 pixel Scientific CCD Sensor whose pixel size is 13.5mm, pixel scale 0.283''/pixel, covering a 10'*10' field of view (FOV). Our Reverberation Mapping (RM) campaign started in 2012 October. All the spectra were obtained using YFOSC with Grism 14 which provides a resolution of 92Å/mm (1.8Å/pixel) and covers the wavelength range of 3800-7200Å. In this first paper of the series we report the observations of three objects: Mrk 142, Mrk 335, and IRAS F12397+3333. (3 data files).

  2. Ultra-low dispersion spectroscopy of stars and galaxies

    International Nuclear Information System (INIS)

    Bappu, M.K.V.; Parthasarathy, M.

    1977-01-01

    Application of ultra-low dispersion spectroscopy 10,000 A mm - 1 , is described to study the nuclei of elliptical galaxies, the quasi-stellar objects and for the discovery of faint OB stars, reddened stars and red stars. The instrument used is an f/2 slitless spectrograph with a three degree quartz prism at the Cassegrain focus of the 102-cm Ritchey-Chratien reflector at Kavalur. The spectra cover a field of 40 minutes of arc and the dispersion is 10,000 A mm - 1 . Ultra-low dispersion spectra (microspectra) were obtained for fifteen elliptical and three SO galaxies from the list of Ekers and Ekers (1973) who classified them as compact and extended sources from the observations of radio emission at 6 cms. From an analysis of micro-spectra and from direct photographs with graded exposure times, it is found that all compact radio galaxies in the Ekers list also have optically compact nuclei. Some of these elliptical galaxies with compact nuclei show enhancement of intensity in the blue violet region. From an examination of microspectra of forty-three of the known quasi-stellar objects of different redshifts it is found that the most striking characteristic of the spectra is their flat appearance. This characteristic flatness is also noticed in the microspectrum of the large redshift quasi-stellar objects like OH 471 and OQ 172 which do not have UV excess. Because of this characteristic difference in the appearance of the microspectra of the quasi-stellar objects and stellar objects, it is possible to detect new OSO's with this technique. An application of this technique to detect red stars in our galaxy and in the Large Magellanic cloud is discussed. (author)

  3. Thermal control modeling approach for GRAPE (GRAntecan PolarimEter)

    Science.gov (United States)

    Di Varano, I.; Woche, M.; Strassmeier, K. G.

    2016-08-01

    GRAPE is the polarimeter planned to be installed on the main Cassegrain focus of GTC (Gran Telescopio Canarias), having an equivalent entrance pupil of 10.4 m, located at the Observatorio del Roque de los Muchachos (ORM) , in La Palma, Canary Islands. It's meant to deliver full Stokes (IQUV) polarimetry covering the spectral range 0.420-1.6 μ, in order to feed the HORS instrument (High Optical Resolution Spectrograph), mounted on the Nasmyth platform, which has a FWHM resolving power of about 25,000 (5 pixel) designed for the wavelength range of 380-800 nm. Two calcite blocks and a BK-7 prism arranged in a Foster configuration are splitting the Ø12.5mm collimated beam into the ordinary and extraordinary components. The entire subunit from the Foster prisms down to the input fibers is rotated by steps of 45 degrees in order to retrieve Q, U components. By inserting a quarter wave retarder plate before the entrance to the Foster unit circular polarization is measured too. The current paper consist of two main parts: at first CFD simulations are introduced, which have been run compliant to the specifications derived by the environmental conditions and the transient thermal gradients taking into account the presence of the electronic cabinets installed, which are triggering the boundary conditions for the outer structure of the instrument; then a thermal control model is proposed based on heat exchangers to stabilize the inner temperature when compensation via passive insulation is not enough. The tools that have been adopted to reach for such goal are Ansys Multiphysics, in particular CFX package and Python scripts.

  4. The afocal telescope optical design and tolerance analysis for the ESA ARIEL mission

    Science.gov (United States)

    Da Deppo, Vania; Middleton, Kevin; Focardi, Mauro; Morgante, Gianluca; Grella, Samuele; Claudi, Riccardo; Pace, Emanuele; Ficai Veltroni, Iacopo; Micela, Giuseppina

    2017-11-01

    ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) is one of the three present candidates for the next ESA medium-class science mission (M4) to be launched in 2026. During its 3.5 years of scientific operations from L2 orbit, this mission will observe spectroscopically in the infrared (IR) a large population of known transiting planets in the neighbourhood of the Solar System. The aim is to enable a deep understanding of the physics and chemistry of these exoplanets. ARIEL is based on a 1-m class telescope ahead of a suite of instruments: two spectrometer channels covering the band 1.95 to 7.80 µm and four photometric channels (two wide and two narrow band) in the range 0.5 to 1.9 μm. The ARIEL optical design is conceived as a fore-module common afocal telescope that will feed the spectrometer and photometric channels. The telescope optical design is based on an eccentric pupil two-mirror classic Cassegrain configuration coupled to a tertiary paraboloidal mirror. An all-aluminum structure has been considered for the telescope layout, and a detailed tolerance analysis has been conducted to assess the telescope feasibility. This analysis has been done including the different parts of the realization and life of the instrument, from integration on-ground to in-flight stability during the scientific acquisitions. The primary mirror (M1) temperature will be monitored and finely tuned via an active thermal control system based on thermistors and heaters. The heaters will be switched on and off to maintain the M1 temperature within ±1K thanks to a proportional-integral-derivative (PID) controller.

  5. Polarization modeling and predictions for DKIST part 3: focal ratio and thermal dependencies of spectral polarization fringes and optic retardance

    Science.gov (United States)

    Harrington, David M.; Sueoka, Stacey R.

    2018-01-01

    Data products from high spectral resolution astronomical polarimeters are often limited by fringes. Fringes can skew derived magnetic field properties from spectropolarimetric data. Fringe removal algorithms can also corrupt the data if the fringes and object signals are too similar. For some narrow-band imaging polarimeters, fringes change the calibration retarder properties and dominate the calibration errors. Systems-level engineering tools for polarimetric instrumentation require accurate predictions of fringe amplitudes, periods for transmission, diattenuation, and retardance. The relevant instabilities caused by environmental, thermal, and optical properties can be modeled and mitigation tools developed. We create spectral polarization fringe amplitude and temporal instability predictions by applying the Berreman calculus and simple interferometric calculations to optics in beams of varying F/ number. We then apply the formalism to superachromatic six-crystal retarders in converging beams under beam thermal loading in outdoor environmental conditions for two of the world's largest observatories: the 10-m Keck telescope and the Daniel K. Inouye Solar Telescope (DKIST). DKIST will produce a 300-W optical beam, which has imposed stringent requirements on the large diameter six-crystal retarders, dichroic beamsplitters, and internal optics. DKIST retarders are used in a converging beam with F/ ratios between 8 and 62. The fringe spectral periods, amplitudes, and thermal models of retarder behavior assisted DKIST optical designs and calibration plans with future application to many astronomical spectropolarimeters. The Low Resolution Imaging Spectrograph with polarimetry instrument at Keck also uses six-crystal retarders in a converging F / 13 beam in a Cassegrain focus exposed to summit environmental conditions providing observational verification of our predictions.

  6. Update on the Commensal VLA Low-band Ionospheric and Transient Experiment (VLITE)

    Science.gov (United States)

    Kassim, Namir E.; Clarke, Tracy E.; Ray, Paul S.; Polisensky, Emil; Peters, Wendy M.; Giacintucci, Simona; Helmboldt, Joseph F.; Hyman, Scott D.; Brisken, Walter; Hicks, Brian; Deneva, Julia S.

    2017-01-01

    The JVLA Low-band Ionospheric and Transient Experiment (VLITE) is a commensal observing system on the NRAO JVLA. The separate optical path of the prime-focus sub-GHz dipole feeds and the Cassegrain-focus GHz feeds provided an opportunity to expand the simultaneous frequency operation of the JVLA through joint observations across both systems. The low-band receivers on 10 JVLA antennas are outfitted with dedicated samplers and use spare fibers to transport the 320-384 MHz band to the VLITE correlator. The initial phase of VLITE uses a custom-designed real-time DiFX software correlator to produce autocorrelations, as well as parallel and cross-hand cross-correlations from the linear dipole feeds. NRL and NRAO have worked together to explore the scientific potential of the commensal low frequency system for ionospheric remote sensing, astrophysics and transients. VLITE operates at nearly 70% wall time with roughly 6200 hours of JVLA time recorded each year.VLITE data are used in real-time for ionospheric research and are transferred daily to NRL for processing in the astrophysics and transient pipelines. These pipelines provide automated radio frequency interference excision, calibration, imaging and self-calibration of data.We will review early scientific results from VLITE across all three science focus areas, including the ionosphere, slow (> 1 sec) transients, and astrophysics. We also discuss the future of the project, that includes its planned expansion to eVLITE including the addition of more antennas, and a parallel capability to search for fast (complement NRAO’s 3 GHz VLA Sky Survey (VLASS). Revised pipelines are under development for operation during the on-the-fly operation mode of the sky survey.

  7. The afocal telescope of the ESA ARIEL mission: analysis of the layout

    Science.gov (United States)

    Da Deppo, Vania; Middleton, Kevin; Focardi, Mauro; Morgante, Gianluca; Corso, Alain Jody; Pace, Emanuele; Claudi, Riccardo; Micela, Giuseppina

    2017-09-01

    ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) is one of the three present candidates as an M4 ESA mission to be launched in 2026. During its foreseen 3.5 years operation, it will observe spectroscopically in the infrared a large population of known transiting planets in the neighborhood of the Solar System. The aim is to enable a deep understanding of the physics and chemistry of these exoplanets. ARIEL is based on a 1-m class telescope ahead of a suite of instruments: two spectrometer channels covering the band 1.95 to 7.8 μm and four photometric channels (two wide and two narrow band) in the range 0.5 to 1.9 μm. The ARIEL optical design is conceived as a fore-module common afocal telescope that will feed the spectrometer and photometric channels. The telescope optical design is based on an eccentric pupil two-mirror classic Cassegrain configuration coupled to a tertiary paraboloidal mirror. The temperature of the primary mirror (M1) will be monitored and finely tuned by means of an active thermal control system based on thermistors and heaters. They will be switched on and off to maintain the M1 temperature within ±1 K thanks to a proportional-integral-derivative (PID) controller implemented within the Telescope Control Unit (TCU), a Payload electronics subsystem mainly in charge of the active thermal control of the two detectors owning to the spectrometer. TCU will collect the housekeeping data of the controlled subsystems and will forward them to the spacecraft (S/C) by means of the Instrument Control Unit (ICU), the main Payload's electronic Unit linked to the S/C On Board Computer (OBC).

  8. Optical telescope refocussing mechanism concept design on remote sensing satellite

    Science.gov (United States)

    Kuo, Jen-Chueh; Ling, Jer

    2017-09-01

    The optical telescope system in remote sensing satellite must be precisely aligned to obtain high quality images during its mission life. In practical, because the telescope mirrors could be misaligned due to launch loads, thermal distortion on supporting structures or hygroscopic distortion effect in some composite materials, the optical telescope system is often equipped with refocussing mechanism to re-align the optical elements while optical element positions are out of range during image acquisition. This paper is to introduce satellite Refocussing mechanism function model design development process and the engineering models. The design concept of the refocussing mechanism can be applied on either cassegrain type telescope or korsch type telescope, and the refocussing mechanism is located at the rear of the secondary mirror in this paper. The purpose to put the refocussing mechanism on the secondary mirror is due to its higher sensitivity on MTF degradation than other optical elements. There are two types of refocussing mechanism model to be introduced: linear type model and rotation type model. For the linear refocussing mechanism function model, the model is composed of ceramic piezoelectric linear step motor, optical rule as well as controller. The secondary mirror is designed to be precisely moved in telescope despace direction through refocussing mechanism. For the rotation refocussing mechanism function model, the model is assembled with two ceramic piezoelectric rotational motors around two orthogonal directions in order to adjust the secondary mirror attitude in tilt angle and yaw angle. From the validation test results, the linear type refocussing mechanism function model can be operated to adjust the secondary mirror position with minimum 500 nm resolution with close loop control. For the rotation type model, the attitude angle of the secondary mirror can be adjusted with the minimum 6 sec of arc resolution and 5°/sec of angle velocity.

  9. ProtoDESI: First On-Sky Technology Demonstration for the Dark Energy Spectroscopic Instrument

    Science.gov (United States)

    Fagrelius, Parker; Abareshi, Behzad; Allen, Lori; Ballester, Otger; Baltay, Charles; Besuner, Robert; Buckley-Geer, Elizabeth; Butler, Karen; Cardiel, Laia; Dey, Arjun; Duan, Yutong; Elliott, Ann; Emmet, William; Gershkovich, Irena; Honscheid, Klaus; Illa, Jose M.; Jimenez, Jorge; Joyce, Richard; Karcher, Armin; Kent, Stephen; Lambert, Andrew; Lampton, Michael; Levi, Michael; Manser, Christopher; Marshall, Robert; Martini, Paul; Paat, Anthony; Probst, Ronald; Rabinowitz, David; Reil, Kevin; Robertson, Amy; Rockosi, Connie; Schlegel, David; Schubnell, Michael; Serrano, Santiago; Silber, Joseph; Soto, Christian; Sprayberry, David; Summers, David; Tarlé, Greg; Weaver, Benjamin A.

    2018-02-01

    The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the universe using the baryon acoustic oscillations technique. The spectra of 35 million galaxies and quasars over 14,000 square degrees will be measured during a 5-year survey. A new prime focus corrector for the Mayall telescope at Kitt Peak National Observatory will deliver light to 5,000 individually targeted fiber-fed robotic positioners. The fibers in turn feed ten broadband multi-object spectrographs. We describe the ProtoDESI experiment, that was installed and commissioned on the 4-m Mayall telescope from 2016 August 14 to September 30. ProtoDESI was an on-sky technology demonstration with the goal to reduce technical risks associated with aligning optical fibers with targets using robotic fiber positioners and maintaining the stability required to operate DESI. The ProtoDESI prime focus instrument, consisting of three fiber positioners, illuminated fiducials, and a guide camera, was installed behind the existing Mosaic corrector on the Mayall telescope. A fiber view camera was mounted in the Cassegrain cage of the telescope and provided feedback metrology for positioning the fibers. ProtoDESI also provided a platform for early integration of hardware with the DESI Instrument Control System that controls the subsystems, provides communication with the Telescope Control System, and collects instrument telemetry data. Lacking a spectrograph, ProtoDESI monitored the output of the fibers using a fiber photometry camera mounted on the prime focus instrument. ProtoDESI was successful in acquiring targets with the robotically positioned fibers and demonstrated that the DESI guiding requirements can be met.

  10. Remote quantitative analysis of cerium through a shielding window by stand-off laser-induced breakdown spectroscopy

    Energy Technology Data Exchange (ETDEWEB)

    Gong, Yongdeuk [Department of Chemistry, Mokpo National University, Jeonnam 534-729 (Korea, Republic of); Choi, Daewoong [Department of Chemistry, Mokpo National University, Jeonnam 534-729 (Korea, Republic of); Korea Atomic Energy Research Institute, P.O. Box 255, Yuseong, Daejeon 305-353 (Korea, Republic of); Han, Bo-Young, E-mail: byhan@kaeri.re.kr [Korea Atomic Energy Research Institute, P.O. Box 255, Yuseong, Daejeon 305-353 (Korea, Republic of); Yoo, Jonghyun [Applied Spectra, 46665 Fremont Boulevard, Fremont, CA 94538 (United States); Han, Song-Hee [Division of Maritime Transportation System, Mokpo National Maritime University, Jeonnam 530-729 (Korea, Republic of); Lee, Yonghoon, E-mail: yhlee@mokpo.ac.kr [Department of Chemistry, Mokpo National University, Jeonnam 534-729 (Korea, Republic of)

    2014-10-15

    Highlights: • Remote LIBS analysis of cerium in the samples located behind a shielding window. • Effects of a shielding window on the remote LIBS analysis were investigated. • Multivariate analysis improves the calibration quality. - Abstract: Laser-Induced Breakdown Spectroscopy (LIBS) has been considered in many applications in nuclear industry. LIBS can be an ideal technique for analyzing the inaccessible nuclear materials typically located behind a shielding window. We report the effect of optical transmittance of the shielding window on the analytical performances of stand-off LIBS for the preliminary surrogate sample of demonstration pyrochemical process, a mixture of cerium oxide (CeO{sub 2}) and potassium chloride (KCl). A pulsed laser beam was focused on the surface of the sample located 1.45 m away from the stand-off LIBS device. The laser-induced plasma emission was collected through a Schmidt–Cassegrain telescope. LIBS spectra were obtained in an open path and through the shielding window. Univariate calibration curves were obtained using the integrated area of partially resolved Ce I and II lines. The limits of detection (LOD) for Ce were estimated to be 0.046 and 0.061 wt.% for the open-path and through-window analysis, respectively. We found that the through-window LOD is mainly influenced by the optical transmittance of the shielding window and therefore, the through-window LOD can be predicted from the open-path LOD and the optical transmittance of the shielding window. Also, multivariate calibration using partial least squares regression was successfully applied. The quality of calibration could be improved by the multivariate analysis.

  11. A Pilot Astronomy Outreach Project in Bangladesh

    Science.gov (United States)

    Bhattacharya, Dipen; Mridha, Shahjahan; Afroz, Maqsuda

    2015-08-01

    In its strategic planning for the "Astronomy for Development Project," the International Astronomical Union (IAU) has ecognized, among other important missions, the role of astronomy in understanding the far-reaching possibilities for promoting global tolerance and citizenship. Furthermore, astronomy is deemed inspirational for careers in science and technology. The "Pilot Astronomy Outreach Project in Bangladesh"--the first of its kind in the country--aspires to fulfill these missions. As Bangladesh lacks resources to promote astronomy education in universities and schools, the role of disseminating astronomy education to the greater community falls on citizen science organizations. One such group, Anushandhitshu Chokro (AChokro) Science Organization, has been carrying out a successful public outreach program since 1975. Among its documented public events, AChokro organized a total solar eclipse campaign in Bangladesh in 2009, at which 15,000 people were assembled in a single open venue for the eclipse observation. The organization has actively pursued astronomy outreach to dispel public misconceptions about astronomical phenomena and to promote science. AChokro is currently working to build an observatory and Science Outreach Center around a recently-acquired 14-inch Scmidt-Cassegrain telescope and a soon-to-be-acquired new 16-inch reflector, all funded by private donations. The telescopes will be fitted with photometers, spectrometers, and digital and CCD cameras to pursue observations that would include sun spot and solar magnetic fields, planetary surfaces, asteroid search, variable stars and supernovae. The Center will be integrated with schools, colleges, and community groups for regular observation and small-scale research. Special educational and observing sessions for adults will also be organized. Updates on the development of the Center, which is expected to be functioning by the end of 2015, will be shared and feedback invited on the fostering of

  12. Design of off-axial Gregory telescope design with freeform mirror corrector

    Science.gov (United States)

    Bazhanov, Yu.; Vlakhko, V.

    2017-08-01

    In this paper a well-known approach is used for calculation of off-axis three-mirror telescope. It includes usage of conic cross-sections properties, each of the sections forming a stigmatic image. To create a compact optical system, a flat mirror aberration corrector is introduced, which is at later stage transformed into a free-form surface in order to compensate field aberrations. Similarly, one can introduce such a corrector in finalized layout for its further optimization and getting a suitable form, including the conversion of multimirrors axial optical system into decentered one. As an example, off-axial Gregory telescope embodiment is used for infrared waveband region, due to the fact that, unlike the Cassegrain telescope, it provides a real exit pupil, and usage of the mirror corrector brings several advantages. Firstly, this feature may be used to include cold stop or adaptive mirror in the exit pupil, wherein corrector is introduced into a converging beam before the focus of the first mirror. Secondly, when placing corrector in the exit pupil of the optical system it is possible to eliminate high and low order aberrations of center point, which in turn improves optical system f-number, and minimize field aberrations. As another example, off-axial Ritchey-Chretien telescope embodiment is used as a good fit for visible region systems. Analysis and calculation results of optical systems with free-form correctors with surfaces, defined by Power polynomial series are presented in this paper. Advantages of different freeform surfaces usage depends on optical system layouts specifics.

  13. VizieR Online Data Catalog: GSC04778-00152 photometry and spectroscopy (Tuvikene+, 2008)

    Science.gov (United States)

    Tuvikene, T.; Sterken, C.; Eenmae, T.; Hinojosa-Goni, R.; Brogt, E.; Longa Pena, P.; Liimets, T.; Ahumada, M.; Troncoso, P.; Vogt, N.

    2012-04-01

    CCD photometry of GSC04778-00152 was carried out on 54 nights during 9 observing runs. In January 2006 the observations were made with the 41-cm Meade telescope at Observatorio Cerro Armazones (OCA), Chile, using an SBIG STL-6303E CCD camera (3072x2048 pixels, FOV 23.0'x15.4') and Johnson V filter. On 3 nights in December 2006 and on 2 nights in October 2007 we used the 2.4-m Hiltner telescope at the MDM Observatory, Arizona, USA, equipped with the 8kx8k Mosaic imager (FOV 23.6'x23.6'). In December 2006 and January 2007, we also used the 41-cm Meade telescope at OCA, using an SBIG ST-7XME CCD camera (FOV 5.9'x3.9') with no filter. Figure 3 shows all OCA light curves obtained with this configuration. At Tartu Observatory the observations were carried out in December 2006 and January 2007, using the 60-cm telescope with a SpectraSource Instruments HPC-1 camera (1024x1024 pixels, FOV 11.2'x11.2') and V filter. >From January to March 2007 the system was observed using the 1.0-m telescope at SAAO, Sutherland, South Africa with an STE4 CCD camera (1024x1024 pixels, FOV 5.3'x5.3') and UBVRI filters. Spectroscopic observations were carried out at the Tartu Observatory, Estonia, using the 1.5-m telescope with the Cassegrain spectrograph ASP-32 and an Andor Newton CCD camera. (3 data files).

  14. Remote quantitative analysis of cerium through a shielding window by stand-off laser-induced breakdown spectroscopy

    International Nuclear Information System (INIS)

    Gong, Yongdeuk; Choi, Daewoong; Han, Bo-Young; Yoo, Jonghyun; Han, Song-Hee; Lee, Yonghoon

    2014-01-01

    Highlights: • Remote LIBS analysis of cerium in the samples located behind a shielding window. • Effects of a shielding window on the remote LIBS analysis were investigated. • Multivariate analysis improves the calibration quality. - Abstract: Laser-Induced Breakdown Spectroscopy (LIBS) has been considered in many applications in nuclear industry. LIBS can be an ideal technique for analyzing the inaccessible nuclear materials typically located behind a shielding window. We report the effect of optical transmittance of the shielding window on the analytical performances of stand-off LIBS for the preliminary surrogate sample of demonstration pyrochemical process, a mixture of cerium oxide (CeO 2 ) and potassium chloride (KCl). A pulsed laser beam was focused on the surface of the sample located 1.45 m away from the stand-off LIBS device. The laser-induced plasma emission was collected through a Schmidt–Cassegrain telescope. LIBS spectra were obtained in an open path and through the shielding window. Univariate calibration curves were obtained using the integrated area of partially resolved Ce I and II lines. The limits of detection (LOD) for Ce were estimated to be 0.046 and 0.061 wt.% for the open-path and through-window analysis, respectively. We found that the through-window LOD is mainly influenced by the optical transmittance of the shielding window and therefore, the through-window LOD can be predicted from the open-path LOD and the optical transmittance of the shielding window. Also, multivariate calibration using partial least squares regression was successfully applied. The quality of calibration could be improved by the multivariate analysis

  15. Armenia as a Regional Centre for Astronomy for Development activities

    Science.gov (United States)

    Mickaelian, A.

    2015-03-01

    The Byurakan Astrophysical Observatory (BAO, Armenia, http://www.bao.am) are among the candidate IAU Regional Nodes for Astronomy for Development activities. It is one of the main astronomical centers of the former Soviet Union and the Middle East region. At present there are 48 qualified researchers at BAO, including six Doctors of Science and 30 PhDs. Five important observational instruments are installed at BAO, the larger ones being 2.6m Cassegrain (ZTA-2.6) and 1m Schmidt (the one that provided the famous Markarian survey). BAO is regarded as a national scientific-educational center, where a number of activities are being organized, such as: international conferences (4 IAU symposia and 1 IAU colloquium, JENAM-2007, etc.), small workshops and discussions, international summer schools (1987, 2006, 2008 and 2010), and Olympiads. BAO collaborates with scientists from many countries. The Armenian Astronomical Society (ArAS, http://www.aras.am/) is an NGO founded in 2001; it has 93 members and it is rather active in the organization of educational, amateur, popular, promotional and other matters. The Armenian Virtual Observatory (ArVO, http://www.aras.am/Arvo/arvo.htm) is one of the 17 national VO projects forming the International Virtual Observatories Alliance (IVOA) and is the only VO project in the region serving also for educational purposes. A number of activities are planned, such as management, coordination and evaluation of the IAU programs in the area of development and education, establishment of the new IAU endowed lectureship program and organization of seminars and public lectures, coordination and initiation of fundraising activities for astronomy development, organization of regional scientific symposia, conferences and workshops, support to Galileo Teacher Training Program (GTTP), production/publication of educational and promotional materials, etc.

  16. Differential population synthesis approach to mass segregation in M92

    International Nuclear Information System (INIS)

    Tobin, W.J.

    1979-01-01

    Spectra are presented of 26 low-metal stars and of the center and one-quarter intensity positions of M92. Spectral coverage is from 390 to 870 nm with resolution better than 1 nm in the blue and 2 nm in the red. Individual pixel signal-to-noise is about 100. Dwarf features are notably absent from the M92 spectra. Numerical estimates of 36 absorption features are extracted from every spectrum, as are two continuum indices. Mathematical models are constructed describing each feature's dependence on stellar color, luminosity, and metal content and then used to estimate the metal content of 6 of the stars for which the metal content is not known. For 10 features reliably measured in M92's center and edge a mass segregation sensitivity parameter is derived from each feature's deduced luminosity dependence. The ratio of feature equivalent widths at cluster edge and center are compared to this sensitivity: no convincing evidence of mass segregation is seen. The only possible edge-to-center difference seen is in the Mg b 517.4 nm feature. Three of the 10 cluster features can be of interstellar origin, at least in part; in particular the luminosity-sensitive Na D line cannot be used as a segregation indicator. The experience gained suggests that an integrated spectrum approach to globular cluster mass segregation is very difficult. An appendix describes in detail the capabilities of the Pine Bluff Observatory .91 m telescope, Cassegrain grating spectrograph, and intensified Reticon dual diode-array detector. It is possible to determine a highly consistent wavelength calibration

  17. THE FIRST HIGH-REDSHIFT QUASAR FROM Pan-STARRS

    Energy Technology Data Exchange (ETDEWEB)

    Morganson, Eric; De Rosa, Gisella; Decarli, Roberto; Walter, Fabian; Rix, Hans-Walter [Max-Planck-Institut fuer Astronomie, Koenigstuhl 17, 69117 Heidelberg (Germany); Chambers, Ken; Burgett, William; Flewelling, Heather; Hodapp, Klaus; Kaiser, Nick; Magnier, Eugene; Sweeney, Bill; Waters, Christopher [Institute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822 (United States); McGreer, Ian; Fan, Xiaohui [Steward Observatory, University of Arizona, 933 N Cherry Ave., Tucson, AZ 85721 (United States); Greiner, Jochen [Max-Planck-Institut fuer extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching (Germany); Price, Paul, E-mail: morganson@mpia.de [Princeton University Observatory, 4 Ivy Lane, Peyton Hall, Princeton University, Princeton, NJ 08544 (United States)

    2012-06-15

    We present the discovery of the first high-redshift (z > 5.7) quasar from the Panoramic Survey Telescope and Rapid Response System 1 (Pan-STARRS1 or PS1). This quasar was initially detected as an i{sub P1} dropout in PS1, confirmed photometrically with the SAO Wide-field InfraRed Camera at Arizona's Multiple Mirror Telescope (MMT) and the Gamma-Ray Burst Optical/Near-Infrared Detector at the MPG 2.2 m telescope in La Silla. The quasar was verified spectroscopically with the MMT Spectrograph, Red Channel and the Cassegrain Twin Spectrograph at the Calar Alto 3.5 m telescope. Its near-infrared spectrum was taken at the Large Binocular Telescope Observatory (LBT) with the LBT Near-Infrared Spectroscopic Utility with Camera and Integral Field Unit for Extragalactic Research. It has a redshift of 5.73, an AB z{sub P1} magnitude of 19.4, a luminosity of 3.8 Multiplication-Sign 10{sup 47} erg s{sup -1}, and a black hole mass of 6.9 Multiplication-Sign 10{sup 9} M{sub Sun }. It is a broad absorption line quasar with a prominent Ly{beta} peak and a very blue continuum spectrum. This quasar is the first result from the PS1 high-redshift quasar search that is projected to discover more than 100 i{sub P1} dropout quasars and could potentially find more than 10 z{sub P1} dropout (z > 6.8) quasars.

  18. The opto-mechanical design for GMOX: a next-generation instrument concept for Gemini

    Science.gov (United States)

    Smee, Stephen A.; Barkhouser, Robert; Robberto, Massimo; Ninkov, Zoran; Gennaro, Mario; Heckman, Timothy M.

    2016-08-01

    We present the opto-mechanical design of GMOX, the Gemini Multi-Object eXtra-wide-band spectrograph, a potential next-generation (Gen-4 #3) facility-class instrument for Gemini. GMOX is a wide-band, multi-object, spectrograph with spectral coverage spanning 350 nm to 2.4 um with a nominal resolving power of R 5000. Through the use of Digital Micromirror Device (DMD) technology, GMOX will be able to acquire spectra from hundreds of sources simultaneously, offering unparalleled flexibility in target selection. Utilizing this technology, GMOX can rapidly adapt individual slits to either seeing-limited or diffraction-limited conditions. The optical design splits the bandpass into three arms, blue, red, and near infrared, with the near-infrared arm being split into three channels covering the Y+J band, H band, and K band. A slit viewing camera in each arm provides imaging capability for target acquisition and fast-feedback for adaptive optics control with either ALTAIR (Gemini North) or GeMS (Gemini South). Mounted at the Cassegrain focus, GMOX is a large (1.3 m x 2.8 m x 2.0 m) complex instrument, with six dichroics, three DMDs (one per arm), five science cameras, and three acquisition cameras. Roughly half of these optics, including one DMD, operate at cryogenic temperature. To maximize stiffness and simplify assembly and alignment, the opto-mechanics are divided into three main sub-assemblies, including a near-infrared cryostat, each having sub-benches to facilitate ease of alignment and testing of the optics. In this paper we present the conceptual opto-mechanical design of GMOX, with an emphasis on the mounting strategy for the optics and the thermal design details related to the near-infrared cryostat.

  19. An afocal telescope configuration for the ESA ARIEL mission

    Science.gov (United States)

    Da Deppo, Vania; Focardi, Mauro; Middleton, Kevin; Morgante, Gianluca; Pascale, Enzo; Grella, Samuele; Pace, Emanuele; Claudi, Riccardo; Amiaux, Jérôme; Colomé Ferrer, Josep; Hunt, Thomas; Rataj, Miroslaw; Sierra-Roig, Carles; Ficai Veltroni, Iacopo; Eccleston, Paul; Micela, Giuseppina; Tinetti, Giovanna

    2017-12-01

    Atmospheric Remote-Sensing Infrared Exoplanet Large Survey (ARIEL) is a candidate as an M4 ESA mission to launch in 2026. During its 3.5 years of scientific operations, ARIEL will observe spectroscopically in the infrared (IR) a large population of known transiting planets in the neighbourhood of the solar system. ARIEL aims to give a breakthrough in the observation of exoplanet atmospheres and understanding of the physics and chemistry of these far-away worlds. ARIEL is based on a 1 m class telescope feeding a collimated beam into two separate instrument modules: a spectrometer module covering the waveband between 1.95 and 7.8 μm and a combined fine guidance system/visible photometer/NIR spectrometer. The telescope configuration is a classic Cassegrain layout used with an eccentric pupil and coupled to a tertiary off-axis paraboloidal mirror. To constrain the thermo-mechanically induced optical aberrations, the primary mirror (M1) temperature will be monitored and finely tuned using an active thermal control system based on thermistors and heaters. They will be switched on and off to maintain the M1 temperature within ± 1 K by the telescope control unit (TCU). The TCU is a payload electronics subsystem also responsible for the thermal control of the spectrometer module detectors as well as the secondary mirror mechanism and IR calibration source management. The TCU, being a slave subsystem of the instrument control unit, will collect the housekeeping data from the monitored subsystems and will forward them to the master unit. The latter will run the application software, devoted to the main spectrometer management and to the scientific data on-board processing.

  20. 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.

  1. Design of a Gamma Reaction History Diagnostic for the National Ignition Facility

    International Nuclear Information System (INIS)

    Malone, R.M.; Cox, B.C.; Frogget, B.C.; Kaufman, M.I.; Tunnell, T.W.; Herrmann, H.W.; Evans, S.C.; Mack, J.M; Young, C.S.; Stoeffl, W.

    2009-01-01

    Gas Cherenkov detectors have been used to convert fusion gammas into photons to achieve gamma reaction history (GRH) measurements. These gas detectors include a converter, pressurized gas volume, relay optics, and a photon detector. A novel design for the National Ignition Facility (NIF) using 90 o Off-Axis Parabolic mirrors efficiently collects signal from fusion gammas with 8-ps time dispersion.1 Fusion gammas are converted to Compton electrons, which generate broadband Cherenkov light (our response is from 250 to 700 nm) in a pressurized gas cell. This light is relayed into a high-speed detector using three parabolic mirrors. The detector optics collect light from a 125-mm-diameter by 600-mm-long interchangeable gas (CO2 or SF6) volume. Because light is collected from source locations throughout the gas volume, the detector is positioned at the stop position rather than at an image position. The stop diameter and its position are independent of the light-generation locations along the gas cell. This design incorporates a fixed time delay that allows the detector to recover from prompt radiation. Optical ray tracings demonstrate how light can be collected from different angled trajectories of the Compton electrons as they traverse the gas volume. A Monte Carlo model of the conversion process from gammas to Cherenkov photons is used to generate photon trajectories. The collection efficiencies for different gamma energies are evaluated. At NIF, a cluster of four channels will allow for increased dynamic range, as well as different gamma energy thresholds. This GRH design is compared to a gas Cherenkov detector that utilizes a Cassegrain reflector now used at the OMEGA laser facility. 1. R. M. Malone, H. W. Herrmann, W. Stoeffl, J. M. Mack, C. S. Young, 'Gamma bang time/reaction history diagnostics for the National Ignition Facility using 90 o off-axis parabolic mirrors', Rev. Sci. Instrum. 79, 10E532 (2008)

  2. Performance of the NASA Beacon Receiver for the Alphasat Aldo Paraboni TDP5 Propagation Experiment

    Science.gov (United States)

    Nessel, James; Morse, Jacquelynne; Zemba, Michael; Riva, Carlo; Luini, Lorenzo

    2015-01-01

    NASA Glenn Research Center (GRC) and the Politecnico di Milano (POLIMI) have initiated a joint propagation campaign within the framework of the Alphasat propagation experiment to characterize rain attenuation, scintillation, and gaseous absorption effects of the atmosphere in the 40 gigahertz band. NASA GRC has developed and installed a K/Q-band (20/40 gigahertz) beacon receiver at the POLIMI campus in Milan, Italy, which receives the 20/40 gigahertz signals broadcast from the Alphasat Aldo Paraboni Technology Demonstration Payload (TDP) no. 5 beacon payload. The primary goal of these measurements is to develop a physical model to improve predictions of communications systems performance within the Q-band. Herein, we describe the design and preliminary performance of the NASA propagation terminal, which has been installed and operating in Milan since June 2014. The receiver is based upon a validated Fast Fourier Transform (FFT) I/Q digital design approach utilized in other operational NASA propagation terminals, but has been modified to employ power measurement via a frequency estimation technique and to coherently track and measure the amplitude of the 20/40 gigahertz beacon signals. The system consists of a 1.2-meter K-band and a 0.6-meter Q-band Cassegrain reflector employing synchronous open-loop tracking to track the inclined orbit of the Alphasat satellite. An 8 hertz sampling rate is implemented to characterize scintillation effects, with a 1-hertz measurement bandwidth dynamic range of 45 decibels. A weather station with an optical disdrometer is also installed to characterize rain drop size distribution for correlation with physical based models.

  3. Preliminary Results of the NASA Beacon Receiver for Alphasat Aldo Paraboni TDP5 Propagation Experiment

    Science.gov (United States)

    Nessel, James; Morse, Jacquelynne; Zemba, Michael; Riva, Carlo; Luini, Lorenzo

    2014-01-01

    NASA Glenn Research Center (GRC) and the Politecnico di Milano (POLIMI) have initiated a joint propagation campaign within the framework of the Alphasat propagation experiment to characterize rain attenuation, scintillation, and gaseous absorption effects of the atmosphere in the 40 GHz band. NASA GRC has developed and installed a K/Q-band (20/40 GHz) beacon receiver at the POLIMI campus in Milan, Italy, which receives the 20/40 GHz signals broadcast from the Alphasat Aldo Paraboni TDP#5 beacon payload. The primary goal of these measurements is to develop a physical model to improve predictions of communications systems performance within the Q-band. Herein, we describe the design and preliminary performance of the NASA propagation terminal, which has been installed and operating in Milan since May 2014. The receiver is based upon a validated Fast Fourier Transform (FFT) I/Q digital design approach utilized in other operational NASA propagation terminals, but has been modified to employ power measurement via a frequency estimation technique and to coherently track and measure the amplitude of the 20/40 GHz beacon signals. The system consists of a 1.2-m K-band and a 0.6-m Qband Cassegrain reflector employing synchronous open-loop tracking to track the inclined orbit of the Alphasat satellite. An 8 Hz sampling rate is implemented to characterize scintillation effects, with a 1-Hz measurement bandwidth dynamic range of 45 dB. A weather station with an optical disdrometer is also installed to characterize rain drop size distribution for correlation with physical based models.

  4. 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.

  5. Emission line relative intensity variations in the symbiotic stars: CI Cygni, BF Cygni, AX Persei and V1016 Cygni

    International Nuclear Information System (INIS)

    Oliversen, N.A.

    1982-01-01

    Low resolution spectra (lambda 3800 to lambda 5900) are presented of the symbiotic stars CI Cygni, BF Cygni, AX Persei and V1016 Cygni, which were obtained with the Washburn Observatory Boller and Chivens cassegrain spectrograph and intensified Reticon. The spectra were obtained as part of a monitoring program covering 36 months since November 1978. The nebular electron temperature and density are derived from the [O III] lambda 5007 and lambda 4363 emission lines and the uv intercombination lines of lambda 1661 and lambda 1667. Relative emission line intensity variations were observed in all four stars. The relative emission line changes correlated with photometric minima for CI Cyg, AX Per and possibly BF Cyg. These changes are interpreted as due to a red giant eclipsing a nebula surrounding the exciting source. Based on the [O III] line ratio change, the nebular density of V1016 Cyg has continued to decline since 1978. The thesis also contains a discussion of the use of the emision lines of [Ne III] lambda 3869, [O III] lambda 5007, lambda 4363 and He lambda 5876 to derive nebular electron temperature and density. A decline in the intensity ratios of I(lambda 3869)/(lambda 5007) and I(lambda 5876)/I(lambda 5007) were observed during the 1980 minimum of CI Cyg. The observed I(lambda 3869)/I(lambda 5007) decline was too large to be explained by temperature or density changes. The [Ne III] and He II regions in CI Cyg are therefore closer to the hot source than the more extended (o III] emission region. Contained within the appendix is a discussion of a graphical method of solution ot the nebular temperature and density, which is based on the emission lines of [Ne III], [O III] and He I

  6. Near-infrared mapping of spiral barred galaxies

    International Nuclear Information System (INIS)

    Gallais, P.; Rouan, D.; Lacombe, F.

    1990-01-01

    The results presented were obtained with a 32 x 32 InSb charge injection device (CID) array cooled at 4K, at the f/36 cassegrain focus of the 3m60 Canada-France-Hawaii telescope with a spatial resolution of 0.5 inches per pixel. The objects presented are spiral barred galaxies mapped at J(1.25 microns), H(1.65 microns) and K(2.2 microns). The non-axisymetric potential due to the presence of a bar induces dynamical processes leading to the confinement of matter and peculiar morphologies. Infrared imaging is used to study the link between various components. Correlations with other wavelengths ranges and 2-colors diagrams ((J-H), (H-K)) lead to the identification of star forming regions, nucleus. Maps show structures connected to the central core. The question is, are they flowing away or toward the nucleus. Observations of M83 lead to several conclusions. The star forming region, detected in the visible and the infrared cannot be very compact and must extend to the edge of the matter concentration. The general shape of the near-infrared emission and the location of radio and 10 micron peaks suggest the confinement of matter between the inner Linblad resonances localized from CO measurements about 100 and 400 pc. The distribution of color indices in the arc from southern part to the star forming region suggests an increasing amount of gas and a time evolution eventually triggered by supernova explosions. Close to the direction of the bar, a bridge-like structure connects the arc to the nucleus with peculiar color indices

  7. Fluorescence/depolarization lidar for mid-range stand-off detection of biological agents

    Science.gov (United States)

    Mierczyk, Z.; Kopczyński, K.; Zygmunt, M.; Wojtanowski, J.; Młynczak, J.; Gawlikowski, A.; Młodzianko, A.; Piotrowski, W.; Gietka, A.; Knysak, P.; Drozd, T.; Muzal, M.; Kaszczuk, M.; Ostrowski, R.; Jakubaszek, M.

    2011-06-01

    LIDAR system for real-time standoff detection of bio-agents is presented and preliminary experimental results are discussed. The detection approach is based on two independent physical phenomena: (1) laser induced fluorescence (LIF), (2) depolarization resulting from elastic scattering on non-spherical particles. The device includes three laser sources, two receiving telescopes, depolarization component and spectral signature analyzing spectrograph. It was designed to provide the stand-off detection capability at ranges from 200 m up to several kilometers. The system as a whole forms a mobile platform for vehicle or building installation. Additionally, it's combined with a scanning mechanics and advanced software, which enable to conduct the semi-automatic monitoring of a specified space sector. For fluorescence excitation, 3-rd (355 nm) and 4-th (266 nm) harmonics of Nd:YAG pulsed lasers are used. They emit short (~6 ns) pulses with the repetition rate of 20 Hz. Collecting optics for fluorescence echo detection and spectral content analysis includes 25 mm diameter f/4 Newton telescope, Czerny Turner spectrograph and 32-channel PMT. Depending on the grating applied, the spectral resolution from 20 nm up to 3 nm per channel can be achieved. The system is also equipped with an eye-safe (1.5 μm) Nd:YAG OPO laser for elastic backscattering/depolarization detection. The optical echo signal is collected by Cassegrain telescope with aperture diameter of 12.5 mm. Depolarization detection component based on polarizing beam-splitter serves as the stand-off particle-shape analyzer, which is very valuable in case of non-spherical bio-aerosols sensing.

  8. Teaching of Science Through the Seedbed of Astronomy

    Science.gov (United States)

    Moreno Pedraza, L. A.; Salinas Barreto, L. F.

    2017-07-01

    This astronomy seedbed seeks for different methodologies for the development of lifelong learning; this seedbed works through three lines of field that are: rocketry (work different models to reach an advanced machinery), paper models of probes and space vehicles (looking for the representation of the mechanism and its operation), comets (the study of movement in our solar system). In light of the above this seedbed will achieve a breakthrough in science thanks to this learning based on field projects, with different methodologies of study. For this reason we took into account the design and modeling of structures for the explanation of astronomical trends. Taking into account a school curriculum with research activities in astronomy, astrophysics and aerospace science-oriented from the basic knowledge of astronomy, such as the modeling of the motion of the planets, the model of an immediately propulsion rocket and the representation of the functioning of a black hole. The advances were: in rocketry on February 18 2012, in the municipality of "Villa de Leyva", in honor of the 100th anniversary of the founder of the Dominicans of St Catherine of Siena, was launched a pilot of solid fuel rocket with a payload that reached a height of a thousand meters. The modeling on paper in 2015, in the seedbed of astronomy were different models of rockets, spacecraft and satellites. In order to be able to explain in a simple and didactic way the advances in astronomy of these technological mechanism. Since 2015 the observation camp has taken place using telescopes Smith Cassegrain type. This equipment allow investigators to get photos using color filters, which demonstrate the process of this great event.

  9. Design considerations for large detector arrays on submillimeter-wave telescopes

    Science.gov (United States)

    Stark, Antony A.

    2000-07-01

    The emerging technology of large (approximately 10,000 pixel) submillimeter-wave bolometer arrays presents a novel optical design problem -- how can such arrays be fed by diffraction- limited telescope optics where the primary mirror is less than 100,000 wavelengths in diameter? Standard Cassegrain designs for radiotelescope optics exhibit focal surface curvature so large that detectors cannot be placed more than 25 beam diameters from the central ray. The problem is worse for Ritchey-Chretien designs, because these minimize coma while increasing field curvature. Classical aberrations, including coma, are usually dominated by diffraction in submillimeter- wave single dish telescopes. The telescope designer must consider (1) diffraction, (2) aberration, (3) curvature of field, (4) cross-polarization, (5) internal reflections, (6) the effect of blockages, (7) means of beam chopping on- and off-source, (8) gravitational and thermal deformations of the primary mirror, (9) the physical mounting of large detector packages, and (10) the effect of gravity and (11) vibration on those detectors. Simultaneous optimization of these considerations in the case of large detector arrays leads to telescopes that differ considerably from standard radiotelescope designs. Offset optics provide flexibility for mounting detectors, while eliminating blockage and internal reflections. Aberrations and cross-polarization can be the same as on-axis designs having the same diameter and focal length. Trade-offs include the complication of primary mirror homology and an increase in overall cost. A dramatic increase in usable field of view can be achieved using shaped optics. Solutions having one to six mirrors will be discussed, including possible six-mirror design for the proposed South Pole 10 m telescope.

  10. New earth system model for optical performance evaluation of space instruments.

    Science.gov (United States)

    Ryu, Dongok; Kim, Sug-Whan; Breault, Robert P

    2017-03-06

    In this study, a new global earth system model is introduced for evaluating the optical performance of space instruments. Simultaneous imaging and spectroscopic results are provided using this global earth system model with fully resolved spatial, spectral, and temporal coverage of sub-models of the Earth. The sun sub-model is a Lambertian scattering sphere with a 6-h scale and 295 lines of solar spectral irradiance. The atmospheric sub-model has a 15-layer three-dimensional (3D) ellipsoid structure. The land sub-model uses spectral bidirectional reflectance distribution functions (BRDF) defined by a semi-empirical parametric kernel model. The ocean is modeled with the ocean spectral albedo after subtracting the total integrated scattering of the sun-glint scatter model. A hypothetical two-mirror Cassegrain telescope with a 300-mm-diameter aperture and 21.504 mm × 21.504-mm focal plane imaging instrument is designed. The simulated image results are compared with observational data from HRI-VIS measurements during the EPOXI mission for approximately 24 h from UTC Mar. 18, 2008. Next, the defocus mapping result and edge spread function (ESF) measuring result show that the distance between the primary and secondary mirror increases by 55.498 μm from the diffraction-limited condition. The shift of the focal plane is determined to be 5.813 mm shorter than that of the defocused focal plane, and this result is confirmed through the estimation of point spread function (PSF) measurements. This study shows that the earth system model combined with an instrument model is a powerful tool that can greatly help the development phase of instrument missions.

  11. THE ABUNDANCES OF POLYACETYLENES TOWARD CRL618

    International Nuclear Information System (INIS)

    Fonfria, J. P.; Cernicharo, J.; Richter, M. J.; Lacy, J. H.

    2011-01-01

    We present a mid-infrared high spectral resolution spectrum of CRL618 in the frequency ranges 778-784 and 1227-1249 cm -1 (8.01-8.15 and 12.75-12.85 μm) taken with the Texas Echelon-cross-Echelle Spectrograph (TEXES) and the Infrared Telescope Facility (IRTF). We have identified more than 170 rovibrational lines arising from C 2 H 2 , HCN, C 4 H 2 , and C 6 H 2 . We have found no unmistakable trace of C 8 H 2 . The line profiles display a complex structure suggesting the presence of polyacetylenes in several components of the circumstellar envelope (CSE). We derive total column densities of 2.5 x 10 17 , 3.1 x 10 17 , 2.1 x 10 17 , 9.3 x 10 16 cm -2 , and ∼ 16 cm -2 for HCN, C 2 H 2 , C 4 H 2 , C 6 H 2 , and C 8 H 2 , respectively. The observations indicate that both the rotational and vibrational temperatures in the innermost CSE depend on the molecule, varying from 100 to 350 K for the rotational temperatures and 100 to 500 K for the vibrational temperatures. Our results support a chemistry in the innermost CSE based on radical-neutral reactions triggered by the intense UV radiation field.

  12. A new visible spectroscopy diagnostic for the JET ITER-like wall main chamber

    International Nuclear Information System (INIS)

    Maggi, C. F.; Brezinsek, S.; Stamp, M. F.; Griph, S.; Heesterman, P.; Hogben, C.; Horton, A.; Meigs, A.; Studholme, W.; Zastrow, K.-D.; Morlock, C.

    2012-01-01

    In preparation for ITER, JET has been upgraded with a new ITER-like wall (ILW), whereby the main plasma facing components, previously of carbon, have been replaced by mainly Be in the main chamber and W in the divertor. As part of the many diagnostic enhancements, a new, survey, visible spectroscopy diagnostic has been installed for the characterization of the ILW. An array of eight lines-of-sight (LOS) view radially one of the two JET neutral beam shine through areas (W coated carbon fibre composite tiles) at the inner wall. In addition, one vertical LOS views the solid W tile at the outer divertor. The light emitted from the plasma is coupled to a series of compact overview spectrometers, with overall wavelength range of 380–960 nm and to one high resolution Echelle overview spectrometer covering the wavelength range 365–720 nm. The new survey diagnostic has been absolutely calibrated in situ by means of a radiometric light source placed inside the JET vessel in front of the whole optical path and operated by remote handling. The diagnostic is operated in every JET discharge, routinely monitoring photon fluxes from intrinsic and extrinsic impurities (e.g., Be, C, W, N, and Ne), molecules (e.g., BeD, D 2 , ND) and main chamber and divertor recycling (typically Dα, Dβ, and Dγ). The paper presents a technical description of the diagnostic and first measurements during JET discharges.

  13. EXPLORING HALO SUBSTRUCTURE WITH GIANT STARS: SUBSTRUCTURE IN THE LOCAL HALO AS SEEN IN THE GRID GIANT STAR SURVEY INCLUDING EXTENDED TIDAL DEBRIS FROM ωCENTAURI

    International Nuclear Information System (INIS)

    Majewski, Steven R.; Nidever, David L.; Damke, Guillermo J.; Patterson, Richard J.; García Pérez, Ana E.; Smith, Verne V.; Kunkel, William E.; Bizyaev, Dmitry

    2012-01-01

    We present the latitude-normalized radial velocity (v b ) distribution of 3318 subsolar metallicity, V ∼ b sequences. One sequence in the fourth Galactic quadrant lies within the l-v b space expected to contain tidal debris from the 'star cluster' ωCentauri. Not only does ωCen lie precisely in this l-v b sequence, but the positions and v b of member stars match those of N-body simulations of tidally disrupting dwarf galaxies on orbits ending with ωCen's current position and space motion. But the ultimate proof that we have very likely found extended parts of the ωCen tidal stream comes from echelle spectroscopy of a subsample of the stars that reveals a very particular chemical abundance signature known to occur only in ωCen. The newly discovered ωCen debris accounts for almost all fourth Galactic quadrant retrograde stars in the southern GGSS, which suggests ωCen is a dominant contributor of retrograde giant stars in the inner Galaxy.

  14. Chemical study of the metal-rich globular cluster NGC 5927

    Science.gov (United States)

    Mura-Guzmán, A.; Villanova, S.; Muñoz, C.; Tang, B.

    2018-03-01

    Globular clusters (GCs) are natural laboratories where stellar and chemical evolution can be studied in detail. In addition, their chemical patterns and kinematics can tell us to which Galactic structure (disc, bulge, halo or extragalactic) the cluster belongs to. NGC 5927 is one of most metal-rich GCs in the Galaxy and its kinematics links it to the thick disc. We present abundance analysis based on high-resolution spectra of seven giant stars. The data were obtained using Fibre Large Array Multi Element Spectrograph/Ultraviolet Echelle Spectrograph (UVES) spectrograph mounted on UT2 telescope of the European Southern Observatory. The principal objective of this work is to perform a wide and detailed chemical abundance analysis of the cluster and look for possible Multiple Populations (MPs). We determined stellar parameters and measured 22 elements corresponding to light (Na, Al), alpha (O, Mg, Si, Ca, Ti), iron-peak (Sc, V, Cr, Mn, Fe, Co, Ni, Cu, Zn), and heavy elements (Y, Zr, Ba, Ce, Nd, Eu). We found a mean iron content of [Fe/H] = -0.47 ± 0.02 (error on the mean). We confirm the existence of MPs in this GC with an O-Na anti-correlation, and moderate spread in Al abundances. We estimate a mean [α/Fe] = 0.25 ± 0.08. Iron-peak elements show no significant spread. The [Ba/Eu] ratios indicate a predominant contribution from SNeII for the formation of the cluster.

  15. The remarkably high excitation planetary nebula GC 6537.

    Science.gov (United States)

    Aller, L H; Hung, S; Feibelman, W A

    1999-05-11

    NGC 6537 is an unusually high excitation point symmetric planetary nebula with a rich spectrum. Its kinematical structures are of special interest. We are here primarily concerned with the high resolution spectrum as revealed by the Hamilton echelle Spectrograph at Lick Observatory (resolution approximately 0.2 A) and supplemented by UV and near-UV data. These extensive data permit a determination of interstellar extinction, plasma diagnostics, and ionic concentrations. The photoionization models that have been used successfully for many planetary nebulae are not entirely satisfactory here. The plasma electron temperature of a photoionization model cannot much exceed 20,000 K, but plasma diagnostics show that regions emitting radiation of highly ionized atoms such as [NeIV] and [NeV] are much hotter, showing that shock excitation must be important, as suggested by the remarkable kinematics of this object. Hence, instead of employing a strict photoionization model, we are guided by the nebular diagnostics, which reveal how electron temperature varies with ionization potential and accommodates density effects. The predictions of the photoionization model may be useful in estimating ionization correction factor. In effect, we have estimated the chemical composition by using both photoionization and shock considerations.

  16. 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.

  17. The RRc Stars: Chemical Abundances and Envelope Kinematics

    Energy Technology Data Exchange (ETDEWEB)

    Sneden, Christopher; Adamów, Monika [Department of Astronomy and McDonald Observatory, The University of Texas, Austin, TX 78712 (United States); Preston, George W. [Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Chadid, Merieme, E-mail: chris@verdi.as.utexas.edu, E-mail: astromysz@gmail.com, E-mail: gwp@obs.carnegiescience.edu, E-mail: chadid@unice.fr [Université Nice Sophia–Antipolis, Observatoire de la Côte dAzur, UMR 7293, Parc Valrose, F-06108, Nice Cedex 02 (France)

    2017-10-10

    We analyzed series of spectra obtained for 12 stable RRc stars observed with the echelle spectrograph of the du Pont telescope at Las Campanas Observatory and we analyzed the spectra of RRc Blazhko stars discussed by Govea et al. We derived model atmosphere parameters, [Fe/H] metallicities, and [X/Fe] abundance ratios for 12 species of 9 elements. We co-added all spectra obtained during the pulsation cycles to increase signal to noise and demonstrate that these spectra give results superior to those obtained by co-addition in small phase intervals. The RRc abundances are in good agreement with those derived for the RRab stars of Chadid et al. We used radial velocity (RV) measurements of metal lines and H α to construct variations of velocity with phase, and center-of-mass velocities. We used these to construct RV templates for use in low- to medium-resolution RV surveys of RRc stars. Additionally, we calculated primary accelerations, radius variations, and metal and H α velocity amplitudes, which we display as regressions against primary acceleration. We employ these results to compare the atmosphere structures of metal-poor RRc stars with their RRab counterparts. Finally, we use the RV data for our Blazhko stars and the Blazhko periods of Szczygieł and Fabrycky to falsify the Blazhko oblique rotator hypothesis.

  18. A FIVE-YEAR SPECTROSCOPIC AND PHOTOMETRIC CAMPAIGN ON THE PROTOTYPICAL α CYGNI VARIABLE AND A-TYPE SUPERGIANT STAR DENEB

    International Nuclear Information System (INIS)

    Richardson, N. D.; Morrison, N. D.; Kryukova, E. E.; Adelman, S. J.

    2011-01-01

    Deneb is often considered the prototypical A-type supergiant and is one of the visually most luminous stars in the Galaxy. A-type supergiants are potential extragalactic distance indicators, but the variability of these stars needs to be better characterized before this technique can be considered reliable. We analyzed 339 high-resolution echelle spectra of Deneb obtained over the five-year span of 1997 through 2001 as well as 370 Stroemgren photometric measurements obtained during the same time frame. Our spectroscopic analysis included dynamical spectra of the Hα profile, Hα equivalent widths, and radial velocities measured from Si II λλ 6347, 6371. Time-series analysis reveals no obvious cyclic behavior that proceeds through multiple observing seasons, although we found a suspected 40 day period in two, non-consecutive observing seasons. Some correlations are found between photometric and radial velocity data sets and suggest radial pulsations at two epochs. No correlation is found between the variability of the Hα profiles and that of the radial velocities or the photometry. Lucy found evidence that Deneb was a long-period single-lined spectroscopic binary star, but our data set shows no evidence for radial velocity variations caused by a binary companion.

  19. A HIGH-RESOLUTION, MULTI-EPOCH SPECTRAL ATLAS OF PECULIAR STARS INCLUDING RAVE, GAIA , AND HERMES WAVELENGTH RANGES

    International Nuclear Information System (INIS)

    Tomasella, Lina; Munari, Ulisse; Zwitter, Tomaz

    2010-01-01

    We present an Echelle+CCD, high signal-to-noise ratio, high-resolution (R = 20,000) spectroscopic atlas of 108 well-known objects representative of the most common types of peculiar and variable stars. The wavelength interval extends from 4600 to 9400 A and includes the RAVE, Gaia, and HERMES wavelength ranges. Multi-epoch spectra are provided for the majority of the observed stars. A total of 425 spectra of peculiar stars, which were collected during 56 observing nights between 1998 November and 2002 August, are presented. The spectra are given in FITS format and heliocentric wavelengths, with accurate subtraction of both the sky background and the scattered light. Auxiliary material useful for custom applications (telluric dividers, spectrophotometric stars, flat-field tracings) is also provided. The atlas aims to provide a homogeneous database of the spectral appearance of stellar peculiarities, a tool useful both for classification purposes and inter-comparison studies. It could also serve in the planning and development of automated classification algorithms designed for RAVE, Gaia, HERMES, and other large-scale spectral surveys. The spectrum of XX Oph is discussed in some detail as an example of the content of the present atlas.

  20. Laser-induced breakdown spectroscopy for space exploration applications: Influence of the ambient pressure on the calibration curves prepared from soil and clay samples

    International Nuclear Information System (INIS)

    Salle, Beatrice; Cremers, David A.; Maurice, Sylvestre; Wiens, Roger C.

    2005-01-01

    Recently, there has been an increasing interest in the laser-induced breakdown spectroscopy (LIBS) technique for stand-off detection of geological samples for use on landers and rovers to Mars, and for other space applications. For space missions, LIBS analysis capabilities must be investigated and instrumental development is required to take into account constraints such as size, weight, power and the effect of environmental atmosphere (pressure and ambient gas) on flight instrument performance. In this paper, we study the in-situ LIBS method at reduced pressure (7 Torr CO 2 to simulate the Martian atmosphere) and near vacuum (50 mTorr in air to begin to simulate the Moon or asteroids' pressure) as well as at atmospheric pressure in air (for Earth conditions and comparison). Here in-situ corresponds to distances on the order of 150 mm in contrast to stand-off analysis at distance of many meters. We show the influence of the ambient pressure on the calibration curves prepared from certified soil and clay pellets. In order to detect simultaneously all the elements commonly observed in terrestrial soils, we used an Echelle spectrograph. The results are discussed in terms of calibration curves, measurement precision, plasma light collection system efficiency and matrix effects

  1. VizieR Online Data Catalog: Photmetry and spectroscopy of PMS stars in NGC 2264 (Lim+, 2016)

    Science.gov (United States)

    Lim, B.; Sung, H.; Kim, J. S.; Bessell, M. S.; Hwang, N.; Park, B.-G.

    2018-04-01

    Queue scheduled observations were carried out on 2015 April 1 and November 24 with the multi-object high resolution echelle spectrograph Hectochelle attached to the 6.5m telescope of the MMT observatory. The resolving power of the spectrograph (R~34,000) is high enough to detect the LiI λ6708 resonance doublet with little blending from adjacent metallic lines. The multi-object capability allowed us to simultaneously obtain 240 target and sky spectra in a single observation. The OB 26 filter transmits the wavelength range 6530-6715Å, and therefore the useful spectral features Hα λ6563 and HeI λ6678 could also be observed along with the LiI λ6708 line. The spectra of a total of 134 PMS stars were taken in two sets of exposure times -8 minutes x3 for bright stars (V<13.6mag) and 30 minutes x3 for fainter stars. Offset sky spectra were also obtained to correct for the contributions of locally variable nebula emission lines to the spectra of the faint stars. Calibration frames, such as dome flat and comparison spectra, were also acquired, just before and after the target exposure. (1 data file).

  2. Fluorescence-based calculus detection using a 405-nm excitation wavelength

    Science.gov (United States)

    Brede, O.; Schelle, F.; Krueger, S.; Oehme, B.; Dehn, C.; Frentzen, M.; Braun, A.

    2011-03-01

    The aim of this study was to assess the difference of fluorescence signals of cement and calculus using a 405 nm excitation wavelength. A total number of 20 freshly extracted teeth was used. The light source used for this study was a blue LED with a wavelength of 405nm. For each tooth the spectra of calculus and cementum were measured separately. Fluorescence light was collimated into an optical fibre and spectrally analyzed using an echelle spectrometer (aryelle 200, Lasertechnik Berlin, Germany) with an additionally bandpass (fgb 67, Edmund Industrial Optics, Karlsruhe, Germany). From these 40 measurements the median values were calculated over the whole spectrum, leading to two different median spectra, one for calculus and one for cementum. For further statistical analysis we defined 8 areas of interest (AOI) in wavelength regions, showing remarkable differences in signal strength. In 7 AOIs the intensity of the calculus spectrum differed statistically significant from the intensity of the cementum spectrum (p calculus and cement between 600nm and 700nm. Thus, we can conclude that fluorescence of calculus shows a significant difference to the fluorescence of cement. A differentiation over the intensity is possible as well as over the spectrum. Using a wavelength of 405nm, it is possible to distinguish between calculus and cement. These results could be used for further devices to develop a method for feedback controlled calculus removal.

  3. Detection of calculus by laser-induced breakdown spectroscopy (LIBS) using an ultra-short pulse laser system (USPL)

    Science.gov (United States)

    Schelle, F.; Brede, O.; Krueger, S.; Oehme, B.; Dehn, C.; Frentzen, M.; Braun, A.

    2011-03-01

    The aim of this study was to assess the detection of calculus by Laser Induced Breakdown Spectroscopy (LIBS). The study was performed with an Nd:YVO4 laser, emitting pulses with a duration of 8 ps at a wavelength of 1064 nm. A repetition rate of 500 kHz at an average power of 5 W was used. Employing a focusing lense, intensities of the order of 1011 W/cm2 were reached on the tooth surface. These high intensities led to the generation of a plasma. The light emitted by the plasma was collimated into a fibre and then analyzed by an echelle spectroscope in the wavelength region from 220 nm - 900 nm. A total number of 15 freshly extracted teeth was used for this study. For each tooth the spectra of calculus and cementum were assessed separately. Comprising all single measurements median values were calculated for the whole spectrum, leading to two specific spectra, one for calculus and one for cementum. For further statistical analysis 28 areas of interest were defined as wavelength regions, in which the signal strength differed regarding the material. In 7 areas the intensity of the calculus spectrum differed statistically significant from the intensity of the cementum spectrum (p calculus. Further studies are necessary to verify that LIBS is a minimally invasive method allowing a safe application in laser-guided dentistry.

  4. Elemental analysis of cotton by laser-induced breakdown spectroscopy

    Energy Technology Data Exchange (ETDEWEB)

    Schenk, Emily R.; Almirall, Jose R.

    2010-05-01

    Laser-induced breakdown spectroscopy (LIBS) has been applied to the elemental characterization of unprocessed cotton. This research is important in forensic and fraud detection applications to establish an elemental fingerprint of U.S. cotton by region, which can be used to determine the source of the cotton. To the best of our knowledge, this is the first report of a LIBS method for the elemental analysis of cotton. The experimental setup consists of a Nd:YAG laser that operates at the fundamental wavelength as the LIBS excitation source and an echelle spectrometer equipped with an intensified CCD camera. The relative concentrations of elements Al, Ba, Ca, Cr, Cu, Fe, Mg, and Sr from both nutrients and environmental contributions were determined by LIBS. Principal component analysis was used to visualize the differences between cotton samples based on the elemental composition by region in the U.S. Linear discriminant analysis of the LIBS data resulted in the correct classification of >97% of the cotton samples by U.S. region and >81% correct classification by state of origin.

  5. Microanalysis of tool steel and glass with laser-induced breakdown spectroscopy

    Science.gov (United States)

    Loebe, Klaus; Uhl, Arnold; Lucht, Hartmut

    2003-10-01

    A laser microscope system for the microanalytical characterization of complex materials is described. The universal measuring principle of laser-induced breakdown spectroscopy (LIBS) in combination with echelle optics permits a fast simultaneous multielement analysis with a possible spatial resolution below 10 pm. The developed system features completely UV-transparent optics for the laser-microscope coupling and the emission beam path and enables parallel signal detection within the wavelength range of 200-800 nm with a spectral resolution of a few picometers. Investigations of glass defects and tool steels were performed. The characterization of a glass defect in a tumbler by a micro-LIBS line scan, with use of a 266-nm diode-pumped Nd:YAG laser for excitation, is possible by simple comparison of plasma spectra of the defect and the surrounding area. Variations in the main elemental composition as well as impurities by trace elements are detected at the same time. Through measurement of the calibration samples with the known concentration of the corresponding element, a correlation between the intensity of spectral lines and the element concentration was also achieved. The change of elemental composition at the transient stellite solder of tool steels has been determined by an area scan. The two-dimensional pictures show abrupt changes of the element distribution along the solder edge and allow fundamental researches of dynamic modifications (e.g., diffusion) in steel.

  6. Interpretation of two compact planetary nebulae, IC 4997 and NGC 6572, with aid of theoretical models.

    Science.gov (United States)

    Hyung, S; Aller, L H

    1993-01-15

    Observations of two dense compact planetary nebulae secured with the Hamilton Echelle spectrograph at Lick Observatory combined with previously published UV spectra secured with the International Ultraviolet Explorer enable us to probe the electron densities and temperatures (plasma diagnostics) and ionic concentrations in these objects. The diagnostic diagrams show that no homogenous model will work for these nebulae. NGC 6572 may consist of an inner torordal ring of density 25,000 atoms/cm3 and an outer conical shell of density 10,000 atoms/cm3. The simplest model of IC 4997 suggests a thick inner shell with a density of about 107 atoms/cm3 and an outer envelope of density 10,000 atoms/cm3. The abundances of all elements heavier than He appear to be less than the solar values in NGC 6572, whereas He, C, N, and O may be more abundant in IC 4997 than in the sun. IC 4997 presents puzzling problems.

  7. The Fourth Flight of CHESS: Analysis of Interstellar H2 on the γ Ara Sightline

    Science.gov (United States)

    Kruczek, Nick E.; France, Kevin; Nell, Nicholas; Fleming, Brian

    2018-06-01

    In this talk, we describe the scientific motivation and technical development of the Colorado High-resolution Echelle Stellar Spectrograph (CHESS) sounding rocket, focusing on the preliminary science results for the fourth launch of the payload (CHESS-4). CHESS is a far ultraviolet rocket-borne instrument designed to study the atomic-to-molecular transitions within translucent cloud regions in the interstellar medium. CHESS-4 launched on 13 April 2018 aboard NASA/CU sounding rocket mission 36.333 UG. The target for this flight was γ Ara, a B1I star that is known to display a variable and equatorially enhanced stellar wind. We present flight results of interstellar molecular hydrogen excitation, including initial measurements of the column density and temperature, on the sightline. These results are compared to previous values that were calculated using the damping wings of low-J H2 absorption features in Copernicus spectra. We also present analogous flight data for the sightline toward β Sco, finding that the derived column density of the J” = 1 rotational level differs by a factor of ~2 when compared to the previous observations. We discuss the discrepancies between the two measurements and show that the source of the difference is likely due to the opacity of higher rotational levels contributing to the J” = 1 absorption wing, increasing the inferred column density in the previous work.

  8. A young solar twin in the Rosette cluster NGC 2244 line of sight

    Science.gov (United States)

    Huber, Jeremy M.; Kielkopf, John F.; Mengel, Matthew; Carter, Bradley D.; Ferland, Gary J.; Clark, Frank O.

    2018-05-01

    Based on prior precision photometry and cluster age analysis, the bright star GSC 00154-01819 is a possible young pre-main sequence member of the Rosette cluster, NGC 2244. As part of a comprehensive study of the large-scale structure of the Rosette and its excitation by the cluster stars, we noted this star as a potential backlight for a probe of the interstellar medium and extinction along the sight line towards a distinctive nebular feature projected on to the cluster centre. New high-resolution spectra of the star were taken with the University College London Echelle Spectrograph of the AAT. They reveal that rather than being a reddened spectral type B or A star within the Mon OB2 association, it is a nearby, largely unreddened, solar twin of spectral type G2V less than 180 Myr old. It is about 219 pc from the Sun with a barycentric radial velocity of +14.35 ± 1.99 km s-1. The spectrum of the Rosette behind it and along this line of sight shows a barycentric radial velocity of +26.0 ± 2.4 km s-1 in H α, and a full width at half-maximum velocity dispersion of 61.94 ± 1.38 km s-1.

  9. Adjustment of a direct method for the determination of man body burden in Pu-239 on by X-ray detection of U-235; Mise au point d'une methode directe de determination de la charge corporelle en plutonium 239 chez l'homme par detection X de l'uranium 235

    Energy Technology Data Exchange (ETDEWEB)

    Boulay, P [Commissariat a l' Energie Atomique, Bruyeres-le-Chatel (France). Centre d' Etudes

    1968-04-01

    The use of Pu-239 on a larger scale sets a problem about the contamination measurement by aerosol at lung level. A method of direct measurement of Pu-239 lung burden is possible, thanks to the use of a large area window proportional counter. A counter of such pattern, has been especially carried out for this purpose. The adjustment of the apparatus allows an adequate sensibility to detect a contamination at the maximum permissible body burden level. Besides, a method for individual 'internal calibration', with a plutonium mock: the protactinium-233, is reported. (author) [French] L'utilisation a une echelle de plus en plus large du plutonium-239 pose un probleme de la mesure de la contamination par aerosol au niveau du poumon. Une methode de mesure directe de la charge pulmonaire en plutonium-239 est possible grace a l'utilisation d'un compteur proportionnel a fenetre de grande surface. Un compteur de ce type a specialement ete realise dans ce but. La mise au point de l'appareillage permet une sensibilite suffisante pour deceler une contamination au niveau de la Q.M.A (quantite maximale admissible). D'autre part, une methode 'd'etalonnage interne' de l'individu a l'aide d'un simulateur de plutonium, le protactinium-233, est decrite. (auteur)

  10. KECK NIRSPEC RADIAL VELOCITY OBSERVATIONS OF LATE-M DWARFS

    Energy Technology Data Exchange (ETDEWEB)

    Tanner, Angelle; White, Russel [Department of Astronomy, Georgia State University, One Park Place, Atlanta, GA 30303 (United States); Bailey, John [Department of Astronomy, University of Michigan, 830 Dennison Building, 500 Church Street, Ann Arbor, MI 48109-1042 (United States); Blake, Cullen [Department of Astrophysical Sciences, Princeton University, Peyton Hall, Ivy Lane, Princeton, NJ 08544 (United States); Blake, Geoffrey [Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States); Cruz, Kelle [Department of Physics and Astronomy, Hunter College, 695 Park Avenue, New York, NY 10065 (United States); Burgasser, Adam J. [Center for Astrophysics and Space Science, University of California San Diego, La Jolla, CA 92093 (United States); Kraus, Adam [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)

    2012-11-15

    We present the results of an infrared spectroscopic survey of 23 late-M dwarfs with the NIRSPEC echelle spectrometer on the Keck II telescope. Using telluric lines for wavelength calibration, we are able to achieve measurement precisions of down to 45 m s{sup -1} for our late-M dwarfs over a one- to four-year long baseline. Our sample contains two stars with radial velocity (RV) variations of >1000 m s{sup -1}. While we require more measurements to determine whether these RV variations are due to unseen planetary or stellar companions or are the result of starspots known to plague the surface of M dwarfs, we can place upper limits of <40 M{sub J} sin i on the masses of any companions around those two M dwarfs with RV variations of <160 m s{sup -1} at orbital periods of 10-100 days. We have also measured the rotational velocities for all the stars in our late-M dwarf sample and offer our multi-order, high-resolution spectra over 2.0-2.4 {mu}m to the atmospheric modeling community to better understand the atmospheres of late-M dwarfs.

  11. Comparison of a long-pulse Nd:YAG laser and a combined 585/1,064-nm laser for the treatment of acne scars: a randomized split-face clinical study.

    Science.gov (United States)

    Min, Seong U K; Choi, Yu Sung; Lee, Dong Hun; Yoon, Mi Young; Suh, Dae Hun

    2009-11-01

    Nonablative laser is gaining popularity because of the low risk of complications, especially in patients with darker skin. To compare the efficacy and safety of a long-pulse neodymium-doped yttrium aluminium garnet (Nd:YAG) laser and a combined 585/1,064-nm laser for the treatment of acne scars. Nineteen patients with mild to moderate atrophic acne scars received four long-pulse Nd:YAG laser or combined 585/1,064-nm laser treatment sessions at fortnightly intervals. Treatments were administered randomly in a split-face manner. Acne scars showed mild to moderate improvement, with significant Echelle d'évaluation clinique des cicatrices d'acné (ECCA) score reductions, after both treatments. Although intermodality differences were not significant, combined 585/1,064-nm laser was more effective for deep boxcar scars. In patients with combined 585/1,064-nm laser-treated sides that improved more than long-pulse Nd:YAG laser-treated sides, ECCA scores were significantly lower for combined 585/1,064-nm laser treatment. Histologic evaluations revealed significantly greater collagen deposition, although there was no significant difference between the two modalities. Patient satisfaction scores concurred with physicians' evaluations. Both lasers ameliorated acne scarring with minimal downtime. In light of this finding, optimal outcomes might be achieved when laser treatment types are chosen after considering individual scar type and response.

  12. The Variability of Atmospheric Deuterium Brightness at Mars: Evidence for Seasonal Dependence

    Science.gov (United States)

    Mayyasi, Majd; Clarke, John; Bhattacharyya, Dolon; Deighan, Justin; Jain, Sonal; Chaffin, Michael; Thiemann, Edward; Schneider, Nick; Jakosky, Bruce

    2017-10-01

    The enhanced ratio of deuterium to hydrogen on Mars has been widely interpreted as indicating the loss of a large column of water into space, and the hydrogen content of the upper atmosphere is now known to be highly variable. The variation in the properties of both deuterium and hydrogen in the upper atmosphere of Mars is indicative of the dynamical processes that produce these species and propagate them to altitudes where they can escape the planet. Understanding the seasonal variability of D is key to understanding the variability of the escape rate of water from Mars. Data from a 15 month observing campaign, made by the Mars Atmosphere and Volatile Evolution Imaging Ultraviolet Spectrograph high-resolution echelle channel, are used to determine the brightness of deuterium as observed at the limb of Mars. The D emission is highly variable, with a peak in brightness just after southern summer solstice. The trends of D brightness are examined against extrinsic as well as intrinsic sources. It is found that the fluctuations in deuterium brightness in the upper atmosphere of Mars (up to 400 km), corrected for periodic solar variations, vary on timescales that are similar to those of water vapor fluctuations lower in the atmosphere (20-80 km). The observed variability in deuterium may be attributed to seasonal factors such as regional dust storm activity and subsequent circulation lower in the atmosphere.

  13. Carbon Chemistry in IRC+10216: Infrared Detection of Diacetylene

    Science.gov (United States)

    Fonfría, J. P.; Agúndez, M.; Cernicharo, J.; Richter, M. J.; Lacy, J. H.

    2018-01-01

    We present the detection of C4H2 for first time in the envelope of the C-rich AGB star IRC+10216, based on high spectral resolution mid-infrared observations carried out with the Texas Echelon-cross-Echelle Spectrograph mounted on the Infrared Telescope Facility. The obtained spectrum contains 24 narrow absorption features above the detection limit, identified as lines of the ro-vibrational C4H2 band {ν }6+{ν }8({σ }u+). The analysis of these lines through a ro-vibrational diagram indicates that the column density of C4H2 is (2.4 ± 1.5) × 1016 cm‑2. Diacetylene is distributed in two excitation populations accounting for 20% and 80% of the total column density and with rotational temperatures of 47 ± 7 and 420 ± 120 K, respectively. This two-folded rotational temperature suggests that the absorbing gas is located beyond ≃0.″4 ≃ 20 R ⋆ from the star, with a noticeable cold contribution outwards from ≃10″ ≃ 500 R ⋆. This outer shell matches up with the place where cyanoacetylenes and carbon chains are known to form due to the action of the Galactic dissociating radiation field on the neutral gas coming from the inner layers of the envelope.

  14. Validation of nine years of MOPITT V5 NIR using MOZAIC/IAGOS measurements: biases and long-term stability

    Directory of Open Access Journals (Sweden)

    A. T. J. de Laat

    2014-11-01

    Full Text Available Validation results from a comparison between Measurement Of Pollution In The Troposphere (MOPITT V5 Near InfraRed (NIR carbon monoxide (CO total column measurements and Measurement of Ozone and Water Vapour on Airbus in-service Aircraft (MOZAIC/In-Service Aircraft for a Global Observing System (IAGOS aircraft measurements are presented. A good agreement is found between MOPITT and MOZAIC/IAGOS measurements, consistent with results from earlier studies using different validation data and despite large variability in MOPITT CO total columns along the spatial footprint of the MOZAIC/IAGOS measurements. Validation results improve when taking the large spatial footprint of the MOZAIC/IAGOS data into account. No statistically significant drift was detected in the validation results over the period 2002–2010 at global, continental and local (airport scales. Furthermore, for those situations where MOZAIC/IAGOS measurements differed from the MOPITT a priori, the MOPITT measurements clearly outperformed the MOPITT a priori data, indicating that MOPITT NIR retrievals add value to the MOPITT a priori. Results from a high spatial resolution simulation of the chemistry-transport model MOCAGE (MOdèle de Chimie Atmosphérique à Grande Echelle showed that the most likely explanation for the large MOPITT variability along the MOZAIC-IAGOS profile flight path is related to spatio-temporal CO variability, which should be kept in mind when using MOZAIC/IAGOS profile measurements for validating satellite nadir observations.

  15. Study of the Matrix Effect on the Plasma Characterization of Heavy Elements in Soil Sediments

    Directory of Open Access Journals (Sweden)

    Tawfik W.

    2007-01-01

    Full Text Available Laser-induced breakdown spectroscopy (LIBS has been applied to perform a study of the matrix effect on the plasma characterization of soil sediment targets. The plasma is generated by focusing a pulsed Nd: YAG laser on the target in air at atmospheric pressure. The plasma emission spectrum was detected using a portable Echelle spectrometer (Mechelle 7500 — Multichannel Instruments, Stockholm, Sweden with intensified CCD camera. Spectroscopic analysis of plasma evolution of laser produced plasmas has been characterized in terms of their spectra, and electron temperature. Four heavy elements V, Pb, Mn and Co were determined in the obtained spectra. The LTE and optically thin plasma conditions were verified for the produced plasma. The electron temperature and density were determined using the emission intensity and stark broadening, respectively, of the spectral lines of the heavy elements in the soil sediments. The electron temperature does not change with concentration. For environmental applications, the obtained results showed the capability of the proposed LIBS setup with the portable Mechelle 7500 spectrometer to be applied in-situ for real-time measurements of the variation of the matrix elemental composition of soil sediments by following up only a single element as a marker for the composition of the soil sediment without need of analysis of the other elements.

  16. THE NATURE OF THE HYPER-RUNAWAY CANDIDATE HIP 60350

    International Nuclear Information System (INIS)

    Irrgang, Andreas; Przybilla, Norbert; Heber, Ulrich; Fernanda Nieva, M.; Schuh, Sonja

    2010-01-01

    Young, massive stars in the Galactic halo are widely supposed to be the result of an ejection event from the Galactic disk forcing some stars to leave their place of birth as so-called runaway stars. Here, we present a detailed spectroscopic and kinematic analysis of the runaway B star HIP 60350 to determine which runaway scenario-a supernova explosion disrupting a binary system or dynamical interaction in star clusters-may be responsible for HIP 60350's peculiar orbit. Based on a non-local thermodynamic equilibrium approach, a high-resolution optical echelle spectrum was examined to revise spectroscopic quantities and for the first time to perform a differential chemical abundance analysis with respect to the B-type star 18 Peg. The results together with proper motions from the Hipparcos Catalog further allowed the three-dimensional kinematics of the star to be studied numerically. The abundances derived for HIP 60350 are consistent with a slightly supersolar metallicity agreeing with the kinematically predicted place of birth ∼6 kpc away from the Galactic center. However, they do not exclude the possibility of an α-enhanced abundance pattern expected in the case of the supernova scenario. Its outstanding high Galactic rest-frame velocity of 530 ± 35 km s -1 is a consequence of ejection in the direction of Galactic rotation and slightly exceeds the local Galactic escape velocity in a standard Galactic potential. Hence, HIP 60350 may be unbound to the Galaxy.

  17. A SEARCH FOR THE TRANSIT OF HD 168443b: IMPROVED ORBITAL PARAMETERS AND PHOTOMETRY

    Energy Technology Data Exchange (ETDEWEB)

    Pilyavsky, Genady; Mahadevan, Suvrath; Wright, Jason T.; Wang, Xuesong X. [Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 (United States); Kane, Stephen R.; Ciardi, David R.; Dragomir, Diana; Von Braun, Kaspar [NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125 (United States); Howard, Andrew W. [Department of Astronomy, University of California, Berkeley, CA 94720 (United States); De Pree, Chris; Marlowe, Hannah [Department of Physics and Astronomy, Agnes Scott College, 141 East College Avenue, Decatur, GA 30030 (United States); Fischer, Debra [Department of Astronomy, Yale University, New Haven, CT 06511 (United States); Henry, Gregory W. [Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209 (United States); Jensen, Eric L. N. [Department of Physics and Astronomy, Swarthmore College, Swarthmore, PA 19081 (United States); Laughlin, Gregory [UCO/Lick Observatory, University of California, Santa Cruz, CA 95064 (United States); Rabus, Markus, E-mail: gcp5017@psu.edu, E-mail: suvrath@astro.psu.edu [Departamento de Astonomia y Astrofisica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22 (Chile)

    2011-12-20

    The discovery of transiting planets around bright stars holds the potential to greatly enhance our understanding of planetary atmospheres. In this work we present the search for transits of HD 168443b, a massive planet orbiting the bright star HD 168443 (V = 6.92) with a period of 58.11 days. The high eccentricity of the planetary orbit (e = 0.53) significantly enhances the a priori transit probability beyond that expected for a circular orbit, making HD 168443 a candidate for our ongoing Transit Ephemeris Refinement and Monitoring Survey. Using additional radial velocities from Keck High Resolution Echelle Spectrometer, we refined the orbital parameters of this multi-planet system and derived a new transit ephemeris for HD 168443b. The reduced uncertainties in the transit window make a photometric transit search practicable. Photometric observations acquired during predicted transit windows were obtained on three nights. Cerro Tololo Inter-American Observatory 1.0 m photometry acquired on 2010 September 7 had the required precision to detect a transit but fell just outside of our final transit window. Nightly photometry from the T8 0.8 m automated photometric telescope at Fairborn Observatory, acquired over a span of 109 nights, demonstrates that HD 168443 is constant on a timescale of weeks. Higher-cadence photometry on 2011 April 28 and June 25 shows no evidence of a transit. We are able to rule out a non-grazing transit of HD 168443b.

  18. A Search for the Transit of HD 168443b: Improved Orbital Parameters and Photometry

    Science.gov (United States)

    Pilyavsky, Genady; Mahadevan, Suvrath; Kane, Stephen R.; Howard, Andrew W.; Ciardi, David R.; de Pree, Chris; Dragomir, Diana; Fischer, Debra; Henry, Gregory W.; Jensen, Eric L. N.; Laughlin, Gregory; Marlowe, Hannah; Rabus, Markus; von Braun, Kaspar; Wright, Jason T.; Wang, Xuesong X.

    2011-12-01

    The discovery of transiting planets around bright stars holds the potential to greatly enhance our understanding of planetary atmospheres. In this work we present the search for transits of HD 168443b, a massive planet orbiting the bright star HD 168443 (V = 6.92) with a period of 58.11 days. The high eccentricity of the planetary orbit (e = 0.53) significantly enhances the a priori transit probability beyond that expected for a circular orbit, making HD 168443 a candidate for our ongoing Transit Ephemeris Refinement and Monitoring Survey. Using additional radial velocities from Keck High Resolution Echelle Spectrometer, we refined the orbital parameters of this multi-planet system and derived a new transit ephemeris for HD 168443b. The reduced uncertainties in the transit window make a photometric transit search practicable. Photometric observations acquired during predicted transit windows were obtained on three nights. Cerro Tololo Inter-American Observatory 1.0 m photometry acquired on 2010 September 7 had the required precision to detect a transit but fell just outside of our final transit window. Nightly photometry from the T8 0.8 m automated photometric telescope at Fairborn Observatory, acquired over a span of 109 nights, demonstrates that HD 168443 is constant on a timescale of weeks. Higher-cadence photometry on 2011 April 28 and June 25 shows no evidence of a transit. We are able to rule out a non-grazing transit of HD 168443b.

  19. CHEMICAL COMPOSITIONS OF THIN-DISK, HIGH-METALLICITY RED HORIZONTAL-BRANCH FIELD STARS

    International Nuclear Information System (INIS)

    Afşar, M.; Sneden, C.; For, B.-Q.

    2012-01-01

    We present a detailed abundance analysis and atmospheric parameters of 76 stars from a survey to identify field Galactic red horizontal-branch (RHB) stars. High-resolution echelle spectra (R ≅ 60,000, S/N ≥ 100) were obtained with the 2.7 m Harlan J. Smith Telescope at McDonald Observatory. The target stars were selected only by color and parallax information. Overall metallicities and relative abundances of proton-capture elements (C, N, O, Li), α-elements (Ca and Si), and neutron-capture elements (Eu and La) were determined by either equivalent width or synthetic spectrum analyses. We used CN features at the λλ7995-8040 region in order to determine the 12 C/ 13 C ratios of our targets. Investigation of the evolutionary stages, using spectroscopic T eff and log g values along with derived 12 C/ 13 C ratios, revealed the presence of 18 probable RHB stars in our sample. We also derived kinematics of the stars with available distance information. Taking into account both the kinematics and probable evolutionary stages, we conclude that our sample contains 5 thick-disk and 13 thin-disk RHB stars. Up until now, RHB stars have been considered as members of the thick disk, and were expected to have large space velocities and sub-solar metallicities. However, our sample is dominated by low-velocity solar-metallicity RHB stars; their existence cannot be easily explained with standard stellar evolution.

  20. VizieR Online Data Catalog: Solar-type stars from SDSS-III MARVELS. VI. HD 87646 (Ma+, 2016)

    Science.gov (United States)

    Ma, B.; Ge, J.; Wolszczan, A.; Muterspaugh, M. W.; Lee, B.; Henry, G. W.; Schneider, D. P.; Martin, E. L.; Niedzielski, A.; Xie, J.; Fleming, S. W.; Thomas, N.; Williamson, M.; Zhu, Z.; Agol, E.; Bizyaev, D.; da Costa, L. N.; Jiang, P.; Fiorenzano, A. F. M.; Hernandez, J. I. G.; Guo, P.; Grieves, N.; Li, R.; Liu, J.; Mahadevan, S.; Mazeh, T.; Nguyen, D. C.; Paegert, M.; Sithajan, S.; Stassun, K.; Thirupathi, S.; van Eyken, J. C.; Wan, X.; Wang, J.; Wisniewski, J. P.; Zhao, B.; Zucker, S.

    2016-11-01

    obtained at KPNO in 2008 January, February, and May. The integration time was 35-40 minutes in 2007 November and 20 minutes in 2008 January, February, and May. A total of 40 data points were obtained from 2007 November to 2008 May and are also listed in Table1. Follow-up observations of HD87646 were conducted with the fiber-fed High Resolution Spectrograph (HRS) of the Hobby Eberley telescope (HET). The observations were executed in queue scheduled mode and used a 2 arcsec fiber, with the HRS slit set, to yield a spectral resolution of R~60000. A total of 29 data points were obtained between 2007 December and 2008 March. The HRS spectra consisted of 46 echelle orders recorded on the blue CCD (407-592nm) and 24 orders on the red one (602-784nm). The spectral data used for RV measurements were extracted from the 17 orders (505-592nm) in which the I2 cell superimposed strong absorption lines. The radial velocities obtained are also provided in Table1. HD87646 was selected as an radial velocity survey target by the Multi-object APO RV Exoplanet Large-area Survey (MARVELS) preselection criterion. The star has been monitored at 23 epochs using the MARVELS instrument mounted on the SDSS 2.5m Telescope at APO between 2009 May and 2011 December. The MARVELS instrument is a fiber-fed dispersed fixed-delay interferometer instrument capable of observing 60 objects simultaneously and covers a wavelength range of 5000-5700Å with a resolution of R~12000. The final differential radial velocity products are included in the SDSS Data Release 12 (Alam et al. 2015ApJS..219...12A) and are presented in Table1. We have obtained additional observations of HD87646 with a fiber-fed echelle spectrograph situated at the 2m Automatic Spectroscopic Telescope (AST) in the Fairborn Observatory. Through 2011 June, the detector was a 2048*4096 SITe ST-002A CCD with 15μm pixels. The AST echelle spectrograph has 21 orders that cover the wavelength range of 4920-7100Å, and has an average resolution of 0

  1. Experimental similitude determination of the influence of perturbations in the thickness of a heating channel on the isolated wall temperatures (1960); Determination experimentale en similitude de l'influence de perturbations dans l'epaisseur d'un canal chauffant sur les temperatures de la paroi isolee (1960)

    Energy Technology Data Exchange (ETDEWEB)

    Vernier, Ph [Commissariat a l' Energie Atomique, Grenoble (France).Centre d' Etudes Nucleaires; Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    A study is made of the local heating phenomena produced on the isolated wall of a channel heated by the Joule effect by a sudden fluctuation in the conducting thickness. By the use of an experimental scale model it has been possible to measure the differences in the isolated wall temperature along the abscissa of the perturbation. The tests carried out show that the temperature differences are contained within a range of {+-} 4 per cent with respect to the temperature differences between the isolated and the isolated walls. (author) [French] On analyse le phenomene thermique local cree sur la paroi isolee d'un canal chauffe par effet Joule, par une perturbation brusque de l'epaisseur conductrice. Un modele experimental a l'echelle a permis de mesurer les ecarts de temperature de la paroi isolee a l'abscisse de la perturbation. Les essais realises ont montre que les ecarts de temperature se situaient dans une bande de {+-} 4 pour cent par rapport a l'ecart de temperature moyen entre paroi isolee et paroi refroidie. (auteur)

  2. Detection of interstellar (C-13)N toward Zeta Ophiuchi

    International Nuclear Information System (INIS)

    Crane, P.; Hegyi, D.J.

    1988-01-01

    Observations of a diffuse interstellar cloud toward Zeta Oph, obtained with resolution 100,000-150,000 near the 3874.608-A R(0) line of (C-12)N using a coude echelle spectrograph on the 1.4-m telescope at ESO during 1984 and 1985, are reported. Data from 54 20-min runs were fitted to Gaussian line shapes using the line center, depth, and width of the R(0) and R(1) lines of (C-12)N and the line center and depth of the R(0) line of (C-13)N as fitting parameters. The (C-13)N R(0) line, with equivalent width 0.190 + or - 0.020 mA, was detected 173.7 + or - 0.8 mA to the red of (C-12)N R(0); the corresponding isotope abundance ratio, (C-12)N/(C-13)N = 47.3 + 5.5 or -4.4, is shown to be in good agreement with previous measurements for CH(+) (Hawkins et al., 1985). 13 references

  3. Retrieval of Optical Parameters From Seawifs Observations Over The Pomme Area (north-est Atlantic): Biogeochemical Applications

    Science.gov (United States)

    Loisel, H.; Nicolas, J.-M.; Merien, D.; Claustre, H.; Sciandra, A.; Becu, G.; Deschamps, P.-Y.

    Since the success of the first ocean color instrument, the Coastal Zone Color Sen- sor (CZCS), the interpretation of ocean color in terms of phytoplankton pigment (the chlorophyll, Chl) is now well recognized. The chlorophyll data, as detected from space, are now currently used to constraint oceanic biological models. New gener- ation of biological models now integrate explicitly 2 or more species of plankton, as well as dissolved organic and particulate matter, DOC and POC, respectively. The as- sessment of such information from the Sea-viewing Wide Field-of-view Sensor and inverse modeling will be discussed. In the frame of the POMME (Programme Océan Multidisciplinaire Méso-Echelle) project we will present the seasonal variability of the absorption, a, the backscattering, bb, and the scattering, b, coefficients as retrieved from SeaWiFS observations over the POMME area. These optical parameters will be compared with in situ measurements made during winter, spring and summer 2001, and biological information derived from these optical properties retrieved at different wavelengths will be presented.

  4. A contribution to the theory of nuclear matter at low density; Contribution a la theorie de la matiere nucleaire a basse densite

    Energy Technology Data Exchange (ETDEWEB)

    Madan, L M [Commissariat a l' Energie Atomique, Saclay (France). Centre d' Etudes Nucleaires

    1961-07-01

    A combination of the variational method using special momentum conserving canonical transformations and the method of resummation of the infinite series of dominating terms in the low density limit is used to study a strongly interacting N particle system. Under the hypothesis that the excitation energy E{sub k} is convex and everywhere positive after the special canonical transformation minimising the average value of the energy has been performed, we have shown that the t-matrix obtained by the summation of the ascending ladders is free from all singularities. Some particular examples are studied in detail. (author) [French] Une combinaison de la methode variationnelle utilisant des transformations canoniques speciales conservant l'impulsion, et de la methode de resommation infinie des termes dominants a basse densite est utilisee pour etudier l'etat fondamental d'un systeme a N particules en interaction forte. Sous reserve de l'hypotnese que l'energie d'excitation E{sub k} est convexe et partout positive, nous avons demontre la regularite de la matrice t obtenue en resommant des echelles montantes une fois effectuee la transformation canonique speciale qui minimise la valeur moyenne de l'energie. Quelques exemples particuliers sont etudies en detail. (auteur)

  5. VizieR Online Data Catalog: Discovery of 2 hot Jupiters KELT-14b & KELT-15b (Rodriguez+, 2016)

    Science.gov (United States)

    Rodriguez, J. E.; Colon, K. D.; Stassun, K. G.; Wright, D.; Cargile, P. A.; Bayliss, D.; Pepper, J.; Collins, K. A.; Kuhn, R. B.; Lund, M. B.; Siverd, R. J.; Zhou, G.; Gaudi, B. S.; Tinney, C. G.; Penev, K.; Tan, T. G.; Stockdale, C.; Curtis, I. A.; James, D.; Udry, S.; Segransan, D.; Bieryla, A.; Latham, D. W.; Beatty, T. G.; Eastman, J. D.; Myers, G.; Bartz, J.; Bento, J.; Jensen, E. L. N.; Oberst, T. E.; Stevens, D. J.

    2018-04-01

    Spectroscopic observations of KELT-14 and KELT-15 were carried out using the CYCLOPS2 fiber feed with the UCLES spectrograph instrument on the Anglo-Australian Telescope (AAT) over two observing runs: UT 2015 February 02-UT 2015 March 01 and UT 2015 May 6-UT 2015 May 13. The instrumental set-up and observing strategy for these observations closely follow that described in earlier CYCLOPS RV papers (Addison et al. 2013ApJ...774L...9A, 2014ApJ...792..112A). CORALIE is a fiber-fed echelle spectrograph (Queloz et al. 2001Msngr.105....1Q) attached to the Swiss 1.2 m Leonard Euler telescope at the ESO La Silla Observatory in Chile. It has a spectral resolution of R~60000, a wavelength range of 3900-6800 Å, and is able to measure radial velocities of bright stars to a precision of 3 m/s or better (Pepe et al. 2002, J/A+A/388/632). We obtained spectra at five epochs of KELT-15 from UT 2015 September 02 to UT 2015 September 14. (3 data files).

  6. High performance modeling of atmospheric re-entry vehicles

    International Nuclear Information System (INIS)

    Martin, Alexandre; Scalabrin, Leonardo C; Boyd, Iain D

    2012-01-01

    Re-entry vehicles designed for space exploration are usually equipped with thermal protection systems made of ablative material. In order to properly model and predict the aerothermal environment of the vehicle, it is imperative to account for the gases produced by ablation processes. In the case of charring ablators, where an inner resin is pyrolyzed at a relatively low temperature, the composition of the gas expelled into the boundary layer is complex and may lead to thermal chemical reactions that cannot be captured with simple flow chemistry models. In order to obtain better predictions, an appropriate gas flow chemistry model needs to be included in the CFD calculations. Using a recently developed chemistry model for ablating carbon-phenolic-in-air species, a CFD calculation of the Stardust re-entry at 71 km is presented. The code used for that purpose has been designed to take advantage of the nature of the problem and therefore remains very efficient when a high number of chemical species are involved. The CFD result demonstrates the need for such chemistry model when modeling the flow field around an ablative material. Modeling of the nonequilibrium radiation spectra is also presented, and compared to the experimental data obtained during Stardust re-entry by the Echelle instrument. The predicted emission from the CN lines compares quite well with the experimental results, demonstrating the validity of the current approach.

  7. The discovery of Ni V in the photospheres of the hot DA white dwarfs RE 2214-492 and G191-B2B

    Science.gov (United States)

    Holberg, J. B.; Hubeny, I.; Barstow, M. A.; Lanz, T.; Sion, E. M.; Tweedy, R. W.

    1994-01-01

    We have co-added six recently obtained International Ultraviolet Explorer (IUE) echelle spectra of the hot DA white dwarf RE 2214-492 and 10 existing archive spectra of the well-known hot DA, G191-B2B. We find that both stars contain numerous weak features due to Ni V. Nickel is thus the second iron-group element to be found in the spectra of the very hottest DA white dwarfs. In addition to Ni V, we also observe Al III in both stars and present evidence for the possible presence of Ni IV and Fe IV in RE 2214-492. The presence of Ni and Al, together with previously reported elements, will contribute significantly to both the EUV opacity and to the apparent complexity of the UV spectra of these stars. Using Non-Local Thermodynamic Equilibrium (NLTE) model atmospheres we estimate the Ni abundances in RE 2214-492 the G191-B2B to be log(Ni/H) = -5.5 +/- 0.3 and -6.0 +/- 0.3, respectively.

  8. Second COS FUV Lifetime Position: Verification of FUV Bright Object Aperture (BOA) Operations (FCAL4)

    Science.gov (United States)

    Debes, John H.

    2013-05-01

    As part of the calibration of the second lifetime position on the Cosmic Origins Spectrograph (COS) far-ultraviolet (FUV) detectors, observations of the external target, G191-B2B, were obtained with the G130M, G160M, and G140L gratings in combi- nation with the Bright Object Aperture. The observations were designed to verify the performance of these spectroscopic modes by reproducing similar observations taken during the SM4 Servicing Mission Observatory Verification (SMOV) of COS. These observations allowed for a detailed determination of the spatial location and profile of the spectra from the three gratings, as well as a determination of the spectral resolution of the G130M grating prior to and after the lifetime move. In general, the negligi- ble differences which exist between the two lifetime positions can be attributed to slight differences in the optical path. In particular, the spectral resolution appears to be slightly improved. The stability of the absolute and relative flux calibration was investigated for G130M as well using STIS echelle data of G191-B2B. We determine that the COS ab- solute flux calibration with the BOA is accurate to 10%, and flux calibrated data are reproducible at the 1-2% level since SMOV.

  9. Classification of uraniferous vein deposits (1960); Essai d'une classification des gites uraniferes filiniens (1960)

    Energy Technology Data Exchange (ETDEWEB)

    Geffroy, J; Sarcia, J A [Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    On the basis of a study of French uraniferous seams and of information found in the literature from all parts of the world, especially since the first Geneva Conference (1955), the authors class these deposits according to two broad categories: - the first type, bound up with the differentiation of an acid rock, fall naturally into the conventional hydrothermal category; - the others come right outside it and seem to be connected to some age modifications, originally of tectonic origin, of the uranium dispersed amongst the rocks on a regional scale. (author) [French] Se basant sur l'etude des filons uraniferes francais, et sur ce qu'apporte la litterature mondiale surtout depuis la premiere conference de Geneve (1955), les auteurs distinguent deux grandes categories de gites: - les uns, lies a la differenciation d'une roche acide, se placent tout naturellement dans les cadres hydrothermalistes classiques; - les autres y echappent totalement, et apparaissent comme lies a des remaniements d'age quelconque, d'origine tectonique au depart, de l'uranium disperse dans les roches a l'echelle regionale. (auteur)

  10. New red giant star in the Kepler open cluster NGC 6819

    Science.gov (United States)

    Komucyeya, E.; Abedigamba, O. P.; Jurua, E.; Anguma, S. K.

    2018-05-01

    A recent study indicated that 39 red giant stars showing solar-like oscillations were discovered in the field of Kepleropen cluster NGC 6819. The study was based on photometric distance estimates of 27 stars out of the 39. Using photometric method alone may not be adequate to confirm the membership of these stars. The stars were not previously known in literature to belong to the open cluster NGC 6819. In this study, Kepler data was used to study the membership of the 27 stars. A plot of apparent magnitude as a function of the large frequency separation, supplemented with the proper motion and radial velocity values from literature revealed KIC 5112840 to lie on the same plane with the well known members of the cluster. Echelle diagram was constructed, and the median gravity-mode period spacings (ΔP) calculated for KIC 5112840. A value of ΔP = 66.3 s was obtained, thus placing the red giant star KIC 5112840 on the Red Giant Branch stage of evolution. Our evolutionary status result using the approach in this paper is in agreement with what is in the available literature.

  11. Calibration-free quantitative elemental analysis of meteor plasma using reference laser-induced breakdown spectroscopy of meteorite samples

    Science.gov (United States)

    Ferus, Martin; Koukal, Jakub; Lenža, Libor; Srba, Jiří; Kubelík, Petr; Laitl, Vojtěch; Zanozina, Ekaterina M.; Váňa, Pavel; Kaiserová, Tereza; Knížek, Antonín; Rimmer, Paul; Chatzitheodoridis, Elias; Civiš, Svatopluk

    2018-03-01

    Aims: We aim to analyse real-time Perseid and Leonid meteor spectra using a novel calibration-free (CF) method, which is usually applied in the laboratory for laser-induced breakdown spectroscopic (LIBS) chemical analysis. Methods: Reference laser ablation spectra of specimens of chondritic meteorites were measured in situ simultaneously with a high-resolution laboratory echelle spectrograph and a spectral camera for meteor observation. Laboratory data were subsequently evaluated via the CF method and compared with real meteor emission spectra. Additionally, spectral features related to airglow plasma were compared with the spectra of laser-induced breakdown and electric discharge in the air. Results: We show that this method can be applied in the evaluation of meteor spectral data observed in real time. Specifically, CF analysis can be used to determine the chemical composition of meteor plasma, which, in the case of the Perseid and Leonid meteors analysed in this study, corresponds to that of the C-group of chondrites.

  12. Oxygen and iron abundances in two metal-poor dwarfs

    Science.gov (United States)

    Spiesman, William J.; Wallerstein, George

    1991-11-01

    Oxygen abundances from the O I line at 6300 A in two metal-poor K dwarfs, HD 25329 and HD 134440, are derived. The spectra were obtained with the KPNO 4-m echelle spectrograph and long camera, yielding a resolution of 32,000 and an S/N of about 125. Model atmospheres with Te of 4770 were appropriate to both stars, whose metallicities were found to be -1.74 and -1.43 for HD 25329 and HD 134440, respectively. These oxygen abundances are 0.3 and 0.4 for the two stars. From the resolution an S/N a 3(sigma) upper limit of 0.8 is derived for each star, which may be combined into an upper limit of O/Fe of 0.6 for a generic K dwarf with Fe/H of 1.6. These values are more in line with O/Fe as seen in similarly metal-poor red giant than those reported in metal-poor subdwarfs by Abia and Rebolo (1989).

  13. Control apparatus for radioactive contamination of the filtering device adapted on the protection apparatus of the respiratory tracts (1961); Appareil de controle de la contamination radioactive des dispositifs filtrants adaptes sur les appareils de protection des voies respiratoires (1961)

    Energy Technology Data Exchange (ETDEWEB)

    Dujancourt, S; Roche, J [Commissariat a l' Energie Atomique, Centre de Production de Plutonium, Marcoule (France). Centre d' Etudes Nucleaires

    1961-07-01

    That apparatus allows to detect and localize the radioactive contamination of the mask cartridge, for alpha, beta and gamma radiations, concerning external contamination, and for beta and gamma radiations, concerning internal contamination. It consists of lead coffin, in which the cartridge is inserted for control. Halogen counters are in contact with it. Operation conditions (Geiger or proportional) and their position on regard to the cartridge are controlled from outside. A sealer counts the pulses, given by the different counters. (authors) [French] Cet appareil permet de detecter et de localiser la contamination radioactive de cartouches filtrantes de masques, en {alpha}, {beta} et {gamma}, en ce qui concerne la contamination exterieure, et en {beta} et {gamma} en ce qui concerne la contamination interieure. Il est constitue par un coffre en plomb dans lequel est introduite la cartouche a controler. Des compteurs halogenes sont au contact de celle-ci. Leur regime de fonctionnement (Geiger ou proportionnel) et leur position par rapport a la cartouche sont commandes de l'exterieur. Une echelle de comptage compte les impulsions donnees par les differents compteurs. (auteurs)

  14. Evaluation of pressure in a plasma produced by laser ablation of steel

    Science.gov (United States)

    Hermann, Jörg; Axente, Emanuel; Craciun, Valentin; Taleb, Aya; Pelascini, Frédéric

    2018-05-01

    We investigated the time evolution of pressure in the plume generated by laser ablation with ultraviolet nanosecond laser pulses in a near-atmospheric argon atmosphere. These conditions were previously identified to produce a plasma of properties that facilitate accurate spectroscopic diagnostics. Using steel as sample material, the present investigations benefit from the large number of reliable spectroscopic data available for iron. Recording time-resolved emission spectra with an echelle spectrometer, we were able to perform accurate measurements of electron density and temperature over a time interval from 200 ns to 12 μs. Assuming local thermodynamic equilibrium, we computed the plasma composition within the ablated vapor material and the corresponding kinetic pressure. The time evolution of plume pressure is shown to reach a minimum value below the pressure of the background gas. This indicates that the process of vapor-gas interdiffusion has a negligible influence on the plume expansion dynamics in the considered timescale. Moreover, the results promote the plasma pressure as a control parameter in calibration-free laser-induced breakdown spectroscopy.

  15. Extraction apparatus used in the treatment of irradiated fuels; Les appareils d'extraction utilises dans le traitement des combustibles irradies

    Energy Technology Data Exchange (ETDEWEB)

    Faugeras, P; Talmont, X [Commissariat a l' Energie Atomique, Saclay (France).Centre d' Etudes Nucleaires

    1960-07-01

    The two qualities necessary in an extractor in the case of solvent extraction of radioactive materials are that they should occupy little space and require little maintenance. In this paper various types of apparatus designed to this effect are examined: firstly mixer-decanter types with mechanical shaking and with shaking and decantation ultrasonically accelerated; then pulsed columns; finally hydro-cyclones. The chemical engineering studies peculiar to the running, supply and control of each of these extractors are described in detail. In certain cases some results obtained on radioactive solutions on a pilot scale are given. (author) [French] Faible encombrement, peu d'entretien, telles sont les deux qualites qu'un extracteur doit posseder dans le cas d'extraction par solvant de matieres radioactives. Dans ce texte seront examines differents types d'appareils concus dans cet esprit: d'abord les appareils typez melangeurs-decanteurs a agitation mecanique, a agitation et decantation accelerees aux ultra-sons; puis les colonnes pulsees; enfin les hydrocyclones. Pour chacun de ces extracteurs seront detaillees les etudes de genie chimique propres a son fonctionnement, a son alimentation, a son controle. Pour certains seront notes quelques resultats obtenus sur des solutions radioactives a l'echelle pilote. (auteur)

  16. The height variation of supergranular velocity fields determined from simultaneous OSO 8 satellite and ground-based observations

    Science.gov (United States)

    November, L. J.; Toomre, J.; Gebbie, K. B.; Simon, G. W.

    1979-01-01

    Results are reported for simultaneous satellite and ground-based observations of supergranular velocities in the sun, which were made using a UV spectrometer aboard OSO 8 and a diode-array instrument operating at the exit slit of an echelle spectrograph attached to a vacuum tower telescope. Observations of the steady Doppler velocities seen toward the limb in the middle chromosphere and the photosphere are compared; the observed spectral lines of Si II at 1817 A and Fe I at 5576 A are found to differ in height of formation by about 1400 km. The results show that supergranular motions are able to penetrate at least 11 density scale heights into the middle chromosphere, that the patterns of motion correlate well with the cellular structure seen in the photosphere, and that the motion increases from about 800 m/s in the photosphere to at least 3000 m/s in the middle chromosphere. These observations imply that supergranular velocities should be evident in the transition region and that strong horizontal shear layers in supergranulation should produce turbulence and internal gravity waves.

  17. The Kinematics of the Permitted C ii λ 6578 Line in a Large Sample of Planetary Nebulae

    Energy Technology Data Exchange (ETDEWEB)

    Richer, Michael G.; Suárez, Genaro; López, José Alberto; García Díaz, María Teresa, E-mail: richer@astrosen.unam.mx, E-mail: gsuarez@astro.unam.mx, E-mail: jal@astrosen.unam.mx, E-mail: tere@astro.unam.mx [Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, Baja California (Mexico)

    2017-03-01

    We present spectroscopic observations of the C ii λ 6578 permitted line for 83 lines of sight in 76 planetary nebulae at high spectral resolution, most of them obtained with the Manchester Echelle Spectrograph on the 2.1 m telescope at the Observatorio Astronómico Nacional on the Sierra San Pedro Mártir. We study the kinematics of the C ii λ 6578 permitted line with respect to other permitted and collisionally excited lines. Statistically, we find that the kinematics of the C ii λ 6578 line are not those expected if this line arises from the recombination of C{sup 2+} ions or the fluorescence of C{sup +} ions in ionization equilibrium in a chemically homogeneous nebular plasma, but instead its kinematics are those appropriate for a volume more internal than expected. The planetary nebulae in this sample have well-defined morphology and are restricted to a limited range in H α line widths (no large values) compared to their counterparts in the Milky Way bulge; both these features could be interpreted as the result of young nebular shells, an inference that is also supported by nebular modeling. Concerning the long-standing discrepancy between chemical abundances inferred from permitted and collisionally excited emission lines in photoionized nebulae, our results imply that multiple plasma components occur commonly in planetary nebulae.

  18. THE KINEMATICS OF THE NEBULAR SHELLS AROUND LOW MASS PROGENITORS OF PNe WITH LOW METALLICITY

    Energy Technology Data Exchange (ETDEWEB)

    Pereyra, Margarita; López, José Alberto; Richer, Michael G., E-mail: mally@astrosen.unam.mx, E-mail: jal@astrosen.unam.mx, E-mail: richer@astrosen.unam.mx [Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 106, C.P. 22800 Ensenada, BC, México (Mexico)

    2016-03-15

    We analyze the internal kinematics of 26 planetary nebulae (PNe) with low metallicity that appear to derive from progenitor stars of the lowest masses, including the halo PN population. Based upon spatially resolved, long-slit, echelle spectroscopy drawn from the San Pedro Mártir Kinematic Catalog of PNe, we characterize the kinematics of these PNe measuring their global expansion velocities based upon the largest sample used to date for this purpose. We find kinematics that follow the trends observed and predicted in other studies, but also find that most of the PNe studied here tend to have expansion velocities less than 20 km s{sup −1} in all of the emission lines considered. The low expansion velocities that we observe in this sample of low metallicity PNe with low mass progenitors are most likely a consequence of a weak central star (CS) wind driving the kinematics of the nebular shell. This study complements previous results that link the expansion velocities of the PN shells with the characteristics of the CS.

  19. Algeria facing the challenges of Europe natural gas supply and the respect of the environment.; L'Algerie face aux defis de l'approvisionnement de l'Europe en gaz naturel et le respect de l'environnement

    Energy Technology Data Exchange (ETDEWEB)

    Ali, Nadia Nait

    2010-09-15

    Taking into account the expectations, for the next decades, of a strong increase in the demand for gas in Europe, Algeria has committed to large structuring projects, adding to the two gas pipeline linking Algeria to Spain via Morocco and Algeria to Italy via Tunisia. Two more undertakings are added linking Algeria directly to two European partners. Sonatrach will play an important role in global environment protection, natural gas being less polluting than oil and coal and emitting less co2. Substitution of coal by natural gas will generate socio economical advantages and will preserve the environment. [French] Compte tenu des attentes, pour les decennies prochaines, d'une forte croissance de la demande de gaz en Europe, l'Algerie s'est engagee dans de grands projet structurants s'ajoutant aux deux gazoducs reliant l'Algerie a l'Espagne via le Maroc et l'Algerie a l'Italie via la Tunisie, viennent s'ajouter deux autres ouvrages reliant directement l'Algerie a deux partenaires europeens. Sonatrach Jouera un role important dans la protection de l'environnement a l'echelle mondiale, le gaz naturel est moins polluants que le petrole, le charbon et emet moins de co2. La substitution du charbon par le gaz naturel generera des avantages socio-economiques, preservation de l'environnement.

  20. SWIFTS: on-chip very high spectral resolution spectrometer

    Science.gov (United States)

    le Coarer, E.; Venancio, L. G.; Kern, P.; Ferrand, J.; Puget, P.; Ayraud, M.; Bonneville, C.; Demonte, B.; Morand, A.; Boussey, J.; Barbier, D.; Blaize, S.; Gonthiez, T.

    2017-11-01

    The size and the weight of state of the art spectrometers is a serious issue regarding space applications. SWIFTS (Stationary Wave Integrated Fourier Transform Spectrometer) is a new FTS family without any moving part. This very promising technology is an original way to fully sample the Fourier interferogram obtained in a waveguide by either a reflection (SWIFTS Lippmann) or counter-propagative (SWIFTS Gabor) interference phenomenon. The sampling is simultaneously performed the optical path thanks to "nano-detectors" located in the evanescent field of the waveguide. For instance a 1.7cm long waveguide properly associated to the detector achieves directly a resolution of 0.13cm-1 on a few centimetre long instruments. Here, firstly we present the development status of this new kind of spectrometers and the first results obtained with on going development of spectrometer covering simultaneously the visible domain from 400 to 1000 nm like an Echelle spectrometer. Valuable technologies allows one to extend the concept to various wavelength domains. Secondly, we present the results obtained in the frame of an activity funded by the European Space Agency where several potential applications in space missions have been identified and studied.