33 results on '"Stephen F. Maher"'
Search Results
2. The design and development status of the cryogenic receiver for the EXoplanet Climate Infrared TELescope (EXCITE)
- Author
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Tim Rehm, Lee Bernard, Andrea Bocchieri, Nat Butler, Quentin Changeat, Azzurra D'Alessandro, Billy Edwards, John Gamaunt, Qian Gong, John Hartley, Kyle Helson, Logan Jensen, Daniel P. Kelly, Kanchita Klangboonkrong, Annalies Kleyheeg, Nikole Lewis, Steven Li, Michael Line, Stephen F. Maher, Ryan McClelland, Laddawan R. Miko, Lorenzo Mugnai, Peter Nagler, Barth Netterfield, Vivien Parmentier, Enzo Pascale, Jennifer Patience, Javier Romualdez, Subhajit Sarkar, Paul A. Scowen, Gregory S. Tucker, Augustyn Waczynski, and Ingo Waldmann
- Published
- 2022
3. Developing Modular Adaptive Transition Edge Sensor SQUID Electronics (MATESSE)
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Stephen F. Maher, Georges Nehmetallah, Iban Ibanez Domenech, Elmer Sharp, and Dale J. Fixsen
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Pixel ,business.industry ,Computer science ,Bolometer ,Astrophysics::Instrumentation and Methods for Astrophysics ,Electrical engineering ,Large format ,Cryogenics ,Modular design ,law.invention ,SQUID ,law ,Electronics ,Transition edge sensor ,business - Abstract
Superconducting Transition Edge Sensor (TES) bolometer arrays with thousands of pixels are essential for achieving the science objectives of future cold far-infrared astronomical telescopes. The readout of such large format TES arrays represents a significant challenge for these missions in terms of power consumption and thermal loading on the coldest cryogenic stages of the instruments. The Time Domain Multiplexing (TDM) technology is mature and has been implemented on many ground-based and air-borne instruments using TES arrays. Several concept studies such as Origins Space Telescope (OST [4]) or Mid-InfraRed Exo-planet CLimate Explorer (MIRECLE [5]) consider this technology and Time Domain Multiplexing as one of the possible baseline technologies for their instruments. In order to address the aforementioned challenges we propose a novel modular solution called Modular Adaptive Transition Edge Sensor Superconducting quantum interference device Electronics (MATESSE) that will serve as the necessary step towards an adaptation of the solution to a space-proven system.
- Published
- 2020
4. COVID-19 and Transportation Infrastructure Resources from Authoritative Entities
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Nancy M. Whiting and Stephen F. Maher
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medicine.medical_specialty ,National security ,Coronavirus disease 2019 (COVID-19) ,business.industry ,Public health ,Pandemic ,medicine ,business ,Transportation infrastructure ,Environmental planning - Abstract
This paper provides information and links to resources that address the Transportation Infrastructure impacts of Covid-19.
- Published
- 2020
5. HAWC+, the Far-Infrared Camera and Polarimeter for SOFIA
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Timothy S. Rennick, Leslie W. Looney, Carolyn G. Volpert, Timothy M. Miller, Jordan A. Guerra, Mandana Amiri, Dominic J. Benford, Stephen J. Heimsath, Louise A. Hamlin, Sean Lin, Kent D. Irwin, Gene C. Hilton, Ian Gatley, Edward J. Wollack, Peter Shirron, Stuart Banks, John E. Vaillancourt, Mark Halpern, Joseph M. Michail, Matthew I. Hollister, Javad Siah, Leroy Sparr, Giles Novak, Jessie L. Dotson, R. F. Loewenstein, Marcus Runyan, Michael Amato, Carl F. Hostetter, Marc Berthoud, Dale Sandford, Brant Cook, Arlin E. Bartels, Stephen F. Maher, C. Jesse Wirth, Nicholas Chapman, Enrique Lopez-Rodriguez, Joel H. Kastner, Armen S. Toorian, Robert Spotz, Christopher J. Hansen, Rhodri Evans, Christine A. Jhabvala, David T. Chuss, Shu I. Wang, Eric Sandberg, Alfonso Hermida, Troy Ames, Sean Casey, Rebecca J. Derro, S. Harvey Moseley, Elmer Sharp, Ryan T. Hamilton, Harvey Rhody, Ernest D. Buchanan, George M. Voellmer, Shannon Towey, Attila Kovács, Rick Shafer, Robert F. Silverberg, Fabio P. Santos, Murzban D. Jhabvala, Johannes Staguhn, Robert J. Pernic, Doyal A. Harper, Robert A. Hirsch, J. G. Tuttle, C. Darren Dowell, and D. J. Fixsen
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Far infrared ,Stratospheric Observatory for Infrared Astronomy ,Instrumentation ,0103 physical sciences ,Astrophysics::Instrumentation and Methods for Astrophysics ,Environmental science ,Astronomy and Astrophysics ,Polarimeter ,010306 general physics ,010303 astronomy & astrophysics ,01 natural sciences ,Remote sensing - Abstract
High-resolution Airborne Wide-band Camera (HAWC[Formula: see text]) is the facility far-infrared imager and polarimeter for SOFIA, NASA’s Stratospheric Observatory for Infrared Astronomy. It is designed to cover the portion of the infrared spectrum that is completely inaccessible to ground-based observatories and which is essential for studies of astronomical sources with temperatures between tens and hundreds of degrees Kelvin. Its ability to make polarimetric measurements of aligned dust grains provides a unique new capability for studying interstellar magnetic fields. HAWC[Formula: see text] began commissioning flights in April 2016 and was accepted as a facility instrument in early 2018. In this paper, we describe the instrument, its operational procedures, and its performance on the observatory.
- Published
- 2018
6. Development of a robust, efficient process to produce scalable, superconducting kilopixel far-IR detector arrays
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Kent D. Irwin, Edward J. Wollack, Karwan Rostem, Ari D. Brown, Johannes Staguhn, Gene C. Hilton, Elmer Sharp, Stephen F. Maher, and Samuel H. Moseley
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Pixel ,Computer science ,Bolometer ,Detector ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Multiplexer ,Space exploration ,law.invention ,Cardinal point ,Robustness (computer science) ,law ,Scalability ,Electronic engineering - Abstract
The far-IR band is uniquely suited to study the physical conditions in the interstellar medium from nearby sources out to the highest redshifts. FIR imaging and spectroscopy instrumentation using incoherent superconducting bolometers represents a high sensitivity technology for many future suborbital and space missions, including the Origins Space Telescope. Robust, high sensitivity detector arrays with several 104 pixels, large focal plane filling factors, and low cosmic ray cross sections that operate over the entire far-IR regime are required for such missions. These arrays could consist of smaller sub-arrays, in case they are tileable. The TES based Backshort Under Grid array architecture which our group has fielded in a number of FIR cameras, is a good candidate to meet these requirements: BUGs are tileable, and with the integration of the SQUID multiplexer scaleable beyond wafer sizes; they provide high filling factors, low cosmic cross section and have been demonstrated successfully in far-infrared astronomical instrumentation. However, the production of BUGs with integrated readout multiplexers has many time and resource consuming process steps. In order to meet the requirement of robustness and efficiency on the production of future arrays, we have developed a new method to provide the superconducting connection of BUG detectors to the readout multiplexers or general readout boards behind the detectors. This approach should allow us to reach the goal to produce reliable, very large detector arrays for future FIR missions.
- Published
- 2018
7. The wide-field spatio-spectral interferometer: system overview, data synthesis and analysis
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David Leisawitz, Roser Juanola-Parramon, Alex Iacchetta, Stephen F. Maher, Stephen A. Rinehart, and Matthew R. Bolcar
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Computer science ,Testbed ,ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION ,Astrophysics::Instrumentation and Methods for Astrophysics ,Experimental data ,Hyperspectral imaging ,01 natural sciences ,law.invention ,010309 optics ,Interferometry ,symbols.namesake ,Fourier transform ,Projector ,Far infrared ,law ,0103 physical sciences ,symbols ,Angular resolution ,010303 astronomy & astrophysics ,Remote sensing - Abstract
The Wide-field Imaging Interferometry Testbed (WIIT) is a double Fourier (DF) interferometer operating at optical wavelengths, and provides data that are highly representative of those from a space-based far-infrared interferometer like SPIRIT. We have used the testbed to observe both geometrically simple and astronomically representative test scenes. Here we present an overview of the astronomical importance of high angular resolution at the far infrared, followed by the description of the optical set-up of WIIT, including the source simulator CHIP (Calibrated Hyperspectral Image Projector). We describe our synthesis algorithms used in the reconstruction of the input test scenes via a simulation of the most recent measurements. The updated algorithms, which include instruments artifacts that allow the synthesis of DF experimental data, are presented and the most recent results analyzed.
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- 2018
8. Lessons learned from the investigation of an anomalous termination of BETTII
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Jordi Vila Hernandez de Lorenzo, Elmer Sharp, Stephen A. Rinehart, A. Dhabal, Stephen F. Maher, Todd J. Veach, Maxime Rizzo, and Dale J. Fixsen
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Aeronautics ,Payload ,Launched ,Cruise ,Palestine ,Geology - Abstract
The Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII) mission launched from Palestine, Texas in June 2017. After an exciting launch and successful cruise, the BETTII gondola suffered an anomalous event at termination. BETTII separated from its parachute and free-fell 136,000 feet into the west Texas desert. This event was classified as a "close-call" and investigated as such. We present here the recovery effort required to find the payload and extract the payload from its impact site. We also present lessons learned from the event and results from the investigation, the design for the next BETTII gondola, and a path forward for return to flight.
- Published
- 2018
9. Design and Expected Performance of GISMO-2, a Two Color Millimeter Camera for the IRAM 30 m Telescope
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Gene C. Hilton, Timothy M. Miller, Johannes Staguhn, Samuel Leclercq, Stephen F. Maher, Eli Dwek, Elmer Sharp, Kent D. Irwin, Edward J. Wollack, S. Harvey Moseley, D. J. Fixsen, Christine A. Jhabvala, Dominic J. Benford, and Attila Kovács
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Physics ,Channel (digital image) ,Dynamic range ,business.industry ,Bolometer ,Condensed Matter Physics ,Atomic and Molecular Physics, and Optics ,law.invention ,Telescope ,Optics ,Full field of view ,law ,General Materials Science ,Millimeter ,Transition edge sensor ,business ,Noise-equivalent power ,Remote sensing - Abstract
We present the main design features for the GISMO-2 bolometer camera, which we build for background-limited operation at the IRAM 30 m telescope on Pico Veleta, Spain. GISMO-2 will operate simultaneously in the 1 and 2 mm atmospherical windows. The 1 mm channel uses a 32×40 TES-based backshort under grid (BUG) bolometer array, the 2 mm channel operates with a 16×16 BUG array. The camera utilizes almost the entire full field of view provided by the telescope. The optical design of GISMO-2 was strongly influenced by our experience with the GISMO 2 mm bolometer camera, which is successfully operating at the 30 m telescope. GISMO is accessible to the astronomical community through the regular IRAM call for proposals.
- Published
- 2014
10. Recent experiments conducted with the Wide-field imaging interferometry testbed (WIIT)
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James R. Fienup, Stephen F. Maher, Matthew R. Bolcar, Stephen A. Rinehart, Alexander S. Iacchetta, Roser Juanola-Parramon, and David Leisawitz
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Physics ,Wide field imaging ,Testbed ,Astrophysics::Instrumentation and Methods for Astrophysics ,Hyperspectral imaging ,02 engineering and technology ,021001 nanoscience & nanotechnology ,01 natural sciences ,010309 optics ,Interferometry ,Test scene ,Observatory ,0103 physical sciences ,0210 nano-technology ,Remote sensing - Abstract
The Wide-field Imaging Interferometry Testbed (WIIT) was developed at NASA's Goddard Space Flight Center to demonstrate and explore the practical limitations inherent in wide field-of-view double Fourier (spatio-spectral) interferometry. The testbed delivers high-quality interferometric data and is capable of observing spatially and spectrally complex hyperspectral test scenes. Although WIIT operates at visible wavelengths, by design the data are representative of those from a space-based far-infrared observatory. We used WIIT to observe a calibrated, independently characterized test scene of modest spatial and spectral complexity, and an astronomically realistic test scene of much greater spatial and spectral complexity. This paper describes the experimental setup, summarizes the performance of the testbed, and presents representative data.
- Published
- 2016
11. GISMO, a 2 mm Bolometer Camera Optimized for the Study of High Redshift Galaxies
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S. Harvey Moseley, Eli Dwek, R. G. Arendt, George M. Voellmer, Christine A. Allen, Troy Ames, David T. Chuss, A. Sievers, Catherine T. Marx, Timothy M. Miller, Attila Kovács, Edward J. Wollack, Dominic J. Benford, Johannes Staguhn, Elmer Sharp, S. Navarro, and Stephen F. Maher
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Luminous infrared galaxy ,Physics ,Active galactic nucleus ,Bolometer ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Quasar ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Condensed Matter Physics ,Atomic and Molecular Physics, and Optics ,Galaxy ,Redshift ,law.invention ,Telescope ,law ,General Materials Science ,Transition edge sensor ,Astrophysics::Galaxy Astrophysics - Abstract
The 2 mm spectral range provides a unique terrestrial window enabling ground based observations of the earliest active dusty galaxies in the universe and thereby allowing a better constraint on the star formation rate in these objects. We have built GISMO (the Goddard-IRAM Superconducting 2-Millimeter Observer), a 2 mm, 128 element superconducting Transition Edge Sensor (TES) based bolometer camera for the IRAM 30 m telescope in Spain. The camera uses an 8×16 planar array of multiplexed TES bolometers, which incorporates our recently designed Backshort Under Grid (BUG) architecture, described elsewhere. The optical design incorporates a 100 mm (4 inches) diameter silicon lens cooled to 4 K, which provides the required fast beam of 0.9 λ/D. With this spatial sampling, GISMO will be very efficient at detecting sources serendipitously in large sky surveys, while the capability for diffraction-limited observations is preserved. With the background limited performance of the detectors, the camera provides significantly greater imaging sensitivity and mapping speed at this wavelength than has previously been possible. The major scientific driver for the instrument is to provide the IRAM 30 m telescope with the capability to rapidly observe galactic and extragalactic dust emission, in particular from high-z Ultra Luminous Infrared Galaxies (ULIRGs) and quasars, even in the summer season. The instrument will fill in the SEDs of high redshift galaxies at the Rayleigh-Jeans part of the dust emission spectrum, even at the highest redshifts. Our source count models predict that GISMO will serendipitously detect one galaxy every four hours on the blank sky, and that one quarter of these galaxies will be at a redshift of z 6.5. We expect to install GISMO at the 30 m telescope in the second half of 2007.
- Published
- 2008
12. Kilopixel backshort-under-grid arrays for the Primordial Inflation Polarization Explorer
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E. Sharp, Edward Leong, J. Lazear, Kent D. Irwin, Aaron M. Datesman, Edward J. Wollack, Nick Costen, Meng-Ping Chang, Samuel H. Moseley, Christine A. Jhabvala, Dominic J. Benford, Johannes Staguhn, Timothy M. Miller, Gene C. Hilton, Stephen F. Maher, Alan J. Kogut, and Regis P. Brekosky
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Physics ,Fabrication ,Pixel ,Physics::Instrumentation and Detectors ,business.industry ,Bolometer ,Detector ,Polarization (waves) ,Multiplexer ,law.invention ,SQUID ,law ,Optoelectronics ,Transition edge sensor ,business - Abstract
We have demonstrated a kilopixel, filled, infrared bolometer array for the balloon-borne Primordial Inflation Polarization Explorer (PIPER). The array consists of three individual components assembled into a single working unit: 1) a transition-edge-sensor bolometer array with background-limited sensitivity, 2) a quarter–wavelength backshort grid, and 3) an integrated Superconducting Quantum Interference Device (SQUID) multiplexer (MUX) readout. The detector array is a filled, square–grid of suspended, one-micron thick silicon bolometers with superconducting sensors. The Backshort–Under–Grid (BUG) is a separately fabricated component serving as a backshort to each pixel in the array. The backshorts are positioned in the cavities created behind each detector by the back–etched well. The spacing of the backshort beneath the detector grid can be set from ~30-300_microns by independently adjusting process parameters during fabrication. Kilopixel arrays are directly indium–bump–bonded to a 32x40 SQUID multiplexer circuit. The array architecture is suitable for a wide range of wavelengths and applications. Detector design specific to the PIPER instrument, fabrication overview, and assembly technologies will be discussed.
- Published
- 2014
13. The GISMO Two-millimeter Deep Field in GOODS-N
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Kent D. Irwin, Edward J. Wollack, Fabian Walter, Gene C. Hilton, Stephen F. Maher, Dale J. Fixsen, Christine A. Jhabvala, Roberto Decarli, Dominic J. Benford, Timothy M. Miller, S. Harvey Moseley, Johannes Staguhn, Alexander Karim, Eli Dwek, Samuel Leclercq, Richard G. Arendt, Attila Kovács, and Elmer Sharp
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Physics ,Hubble Deep Field ,Extraction algorithm ,Astronomy and Astrophysics ,Astrophysics ,01 natural sciences ,Redshift ,Galaxy ,Wavelength ,Space and Planetary Science ,0103 physical sciences ,Millimeter ,010306 general physics ,010303 astronomy & astrophysics - Abstract
We present deep continuum observations using the GISMO camera at a wavelength of 2 mm centered on the Hubble Deep Field (HDF) in the GOODS-N field. These are the first deep field observations ever obtained at this wavelength. The 1 sigma sensitivity in the innermost approx. 4 arcminutes of the 7 utes map is approx. 135 uJy/beam, a factor of three higher in flux/beam sensitivity than the deepest available SCUBA 850 um observations, and almost a factor of four higher in flux / beam sensitivity than the combined MAMBO/AzTEC 1.2 mm observations of this region. Our source extraction algorithm identifies 12 sources directly, and another 3 through correlation with known sources at 1.2 mm and 850 um. Five of the directly detected GISMO sources have counterparts in the MAMBO/AzTEC catalog, and four of those also have SCUBA counterparts. HDF850.1, one of the first blank-field detected submillimeter galaxies, is now detected at 2 mm. The median redshift of all sources with counterparts of known redshifts is med(z) = 2.91 +/- 0.94. Statistically, the detections are most likely real for 5 of the seven 2 mm sources without shorter wavelength counterparts, while the probability for none of them being real is negligible.
- Published
- 2014
14. Realizing 3 D visualization using crossed-beam volumetric displays
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Elizabeth Downing, Edward Bedwell, David S. Ebert, Stephen F. Maher, and Laura Smoliar
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Optics ,General Computer Science ,business.industry ,Computer science ,business ,Beam (structure) ,Visualization - Published
- 1999
15. A control system for BETTII: enabling far-infrared, balloon-borne Fourier transform spectroscopy
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David Leisawitz, Dale J. Fixsen, Robert F. Silverberg, Stephen A. Rinehart, Stephen F. Maher, Dominic J. Benford, and Maxime Rizzo
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Interferometry ,Photon ,Materials science ,Optics ,Far infrared ,business.industry ,Control system ,Phase noise ,Astrophysics::Instrumentation and Methods for Astrophysics ,Fourier transform infrared spectroscopy ,business ,Image resolution ,Fourier transform spectroscopy - Abstract
BETTII, a balloon-borne double-Fourier interferometer, requires precise control of the relative phase and angle between the beams to enable Fourier transform spectroscopy. The control system and its challenges are presented.
- Published
- 2013
16. Precision attitude control for the BETTII balloon-borne interferometer
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Maxime Rizzo, Stephen A. Rinehart, Stephen F. Maher, Richard K. Barry, Dominic J. Benford, and Dale J. Fixsen
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Physics ,business.industry ,law.invention ,Attitude control ,Telescope ,Interferometry ,Optics ,law ,Control system ,Astronomical interferometer ,Balloon-borne telescope ,Angular resolution ,business ,Image resolution ,Remote sensing - Abstract
The Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII) is an 8-meter baseline far-infrared interferometer to fly on a high altitude balloon. Operating at wavelengths of 30-90 microns, BETTII will obtain spatial and spectral information on science targets at angular resolutions down to less than half an arcsecond, a capability unmatched by other far-infrared facilities. This requires attitude control at a level ofless than a tenth of an arcsecond, a great challenge for a lightweight balloon-borne system. We have designed a precision attitude determination system to provide gondola attitude knowledge at a level of 2 milliarcseconds at rates up to 100Hz, with accurate absolute attitude determination at the half arcsecond level at rates of up to 10Hz. A mUlti-stage control system involving rigid body motion and tip-tilt-piston correction provides precision pointing stability to the level required for the far-infrared instrument to perform its spatial/spectral interferometry in an open-loop control. We present key aspects of the design of the attitude determination and control and its development status.
- Published
- 2012
17. The GISMO-2 bolometer camera
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Stephen F. Maher, Timothy M. Miller, Johannes Staguhn, Gene C. Hilton, Attila Kovács, Christine A. Jhabvala, Kent D. Irwin, Dominic J. Benford, Edward J. Wollack, Dale J. Fixsen, Samuel Leclercq, Samuel H. Moseley, and Elemer H. Sharp
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Physics ,Telescope ,Design analysis ,Optics ,Channel (digital image) ,Full field of view ,business.industry ,law ,Bolometer ,Field of view ,business ,law.invention - Abstract
We present the concept for the GISMO-2 bolometer camera) which we build for background-limited operation at the IRAM 30 m telescope on Pico Veleta, Spain. GISM0-2 will operate Simultaneously in the 1 mm and 2 mm atmospherical windows. The 1 mm channel uses a 32 x 40 TES-based Backshort Under Grid (BUG) bolometer array, the 2 mm channel operates with a 16 x 16 BUG array. The camera utilizes almost the entire full field of view provided by the telescope. The optical design of GISM0-2 was strongly influenced by our experience with the GISMO 2 mm bolometer camera which is successfully operating at the 30m telescope. GISMO is accessible to the astronomical community through the regular IRAM call for proposals.
- Published
- 2012
18. Developing wide-field spatio-spectral interferometry for far-infrared space applications
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Stephen A. Rinehart, Nargess Memarsadeghi, Stephen F. Maher, Richard G. Lyon, David Leisawitz, Evan Sinukoff, and Matthew R. Bolcar
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Physics ,COSMIC cancer database ,Infrared ,business.industry ,Testbed ,ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Systems modeling ,law.invention ,Telescope ,Interferometry ,Optics ,Far infrared ,law ,Astronomical interferometer ,Astrophysics::Solar and Stellar Astrophysics ,business ,Astrophysics::Galaxy Astrophysics ,Remote sensing - Abstract
Interferometry is an affordable way to bring the benefits of high resolution to space far-IR astrophysics. We summarize an ongoing effort to develop and learn the practical limitations of an interferometric technique that will enable the acquisition of high-resolution far-IR integral field spectroscopic data with a single instrument in a future space-based interferometer. This technique was central to the Space Infrared Interferometric Telescope (SPIRIT) and Submillimeter Probe of the Evolution of Cosmic Structure (SPECS) space mission design concepts, and it will first be used on the Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII). Our experimental approach combines data from a laboratory optical interferometer (the Wide-field Imaging Interferometry Testbed, WIIT), computational optical system modeling, and spatio-spectral synthesis algorithm development. We summarize recent experimental results and future plans.
- Published
- 2012
19. Demonstration of the wide-field imaging interferometer testbed using a calibrated hyperspectral image projector
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Matthew R. Bolcar, Stephen A. Rinehart, Stephen F. Maher, and David Leisawitz
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Physics ,Pixel ,Spectrometer ,business.industry ,ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION ,Astrophysics::Instrumentation and Methods for Astrophysics ,Hyperspectral imaging ,law.invention ,Interferometry ,Optics ,Projector ,law ,Computer Science::Computer Vision and Pattern Recognition ,Astronomical interferometer ,Digital Light Processing ,business ,Image resolution ,Remote sensing - Abstract
The Wide-field Imaging Interferometer testbed (WIIT) at NASA's Goddard Space Flight Center uses a dual-Michelson interferometric technique. The WIIT combines stellar interferometry with Fourier-transform interferometry to produce high-resolution spatial-spectral data over a large field-of-view. This combined technique could be employed on future NASA missions such as the Space Infrared Interferometric Telescope (SPIRIT) and the Sub-millimeter Probe of the Evolution of Cosmic Structure (SPECS). While both SPIRIT and SPECS would operate at far-infrared wavelengths, the WIIT demonstrates the dual-interferometry technique at visible wavelengths. The WIIT will produce hyperspectral image data, so a true hyperspectral object is necessary. A calibrated hyperspectral image projector (CHIP) has been constructed to provide such an object. The CHIP uses Digital Light Processing (DLP) technology to produce customized, spectrally-diverse scenes. CHIP scenes will have approximately 1.6-micron spatial resolution and the capability of . producing arbitrary spectra in the band between 380 nm and 1.6 microns, with approximately 5-nm spectral resolution. Each pixel in the scene can take on a unique spectrum. Spectral calibration is achieved with an onboard fiber-coupled spectrometer. In this paper we describe the operation of the CHIP. Results from the WIIT observations of CHIP scenes will also be presented.
- Published
- 2012
20. Star and Dust Formation Activities in AzTEC-3, a Starburst Galaxy at z = 5.3
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Dale J. Fixsen, Alexander Karim, Samuel Leclercq, Stephen F. Maher, Richard G. Arendt, Peter Capak, Samuel H. Moseley, Attila Kovács, Johannes Staguhn, Elmer Sharp, Eva Schinnerer, Dominic J. Benford, and Eli Dwek
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar mass ,010308 nuclear & particles physics ,Infrared ,Star formation ,Molecular cloud ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Galaxy ,Luminosity ,Stars ,Space and Planetary Science ,0103 physical sciences ,Spectral energy distribution ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Analyses of high-redshift ultraluminous infrared (IR) galaxies traditionally use the observed optical to submillimeter spectral energy distribution (SED) and estimates of the dynamical mass as observational constraints to derive the star formation rate (SFR), the stellar mass, and age of these objects. An important observational constraint neglected in the analysis is the mass of dust giving rise to the IR emission. In this paper we add this constraint to the analysis of AzTEC-3. Adopting an upper limit to the mass of stars and a bolometric luminosity for this object, we construct stellar and chemical evolutionary scenarios, constrained to produce the inferred dust mass and observed luminosity before the associated stellar mass exceeds the observational limit. We find that the model with a Top Heavy IMF provided the most plausible scenario consistent with the observational constraints. In this scenario the dust formed over a period of ~200 Myr, with a SFR of ~500 Msun/yr. These values for the age and SFR in AzTEC-3 are significantly higher and lower, respectively, from those derived without the dust mass constraint. However, this scenario is not unique, and others cannot be completely ruled out because of the prevailing uncertainties in the age of the galaxy, its bolometric luminosity, and its stellar and dust masses. A robust result of our models is that all scenarios require most of the radiating dust mass to have been accreted in molecular clouds. Our new procedure highlights the importance of a multiwavelength approach, and of the use of dust evolution models in constraining the age and the star formation activity and history in galaxies., Accepted for publication in the ApJ. 12 pages with 11 embedded figures
- Published
- 2011
21. The GISMO 2 Millimeter Camera
- Author
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Johannes G. Staguhn, Dominic J. Benford, Richard Arendt, David T. Chuss, Dale Fixsen, Jithin George, Christine A. Jhabvala, Stephen F. Maher, Timothy M. Miller, S. Harvey Moseley, Elmer H. Sharp, Hans Ungerechts, Edward J. Wollack, Betty Young, Blas Cabrera, and Aaron Miller
- Subjects
Red shift ,Telescope ,Physics ,Optics ,business.industry ,law ,Bolometer ,Millimeter ,business ,Remote sensing ,law.invention - Abstract
In October 2008, for the second time we demonstrated a monolithic Backshort Under Grid (BUG) 8×16 TES array in the field using our 2 mm wavelength imager GISMO (Goddard IRAM Superconducting 2 Millimeter Observer) at the IRAM 30 m telescope in Spain. We present astronomical results from this observing run together with a discussion of the instrument performance.
- Published
- 2009
22. Design of the Millimeter-Wavelength Superconducting Bolometer Camera GISMO
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Dominic J. Benford, Johannes G. Staguhn, Christine A. Jhabvala, Catherine T. Marx, Elmer H. Sharp, Stephen F. Maher, Betty Young, Blas Cabrera, and Aaron Miller
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Luminous infrared galaxy ,Physics ,business.industry ,Planar array ,Detector ,Bolometer ,Astrophysics::Instrumentation and Methods for Astrophysics ,Quasar ,Astrophysics::Cosmology and Extragalactic Astrophysics ,law.invention ,Telescope ,Optics ,law ,Millimeter ,Transition edge sensor ,business ,Astrophysics::Galaxy Astrophysics - Abstract
We have built and operated the GISMO (the Goddard‐IRAM Superconducting 2‐ Millimeter Observer) at the IRAM 30 m telescope in Spain. GISMO is a 128 element superconducting Transition Edge Sensor (TES) based bolometer camera for the two millimeter (150 GHz) band. The camera uses an 8×16 planar array of multiplexed TES bolometers, which incorporates our Backshort Under Grid (BUG) bolometer array architecture. The major scientific driver for the instrument is to provide the capability to observe galactic and extragalactic dust emission rapidly, in particular from high—z Ultra Luminous Infrared Galaxies (ULIRGs) and quasars. With the background‐limited performance of the detectors, the camera provides significantly greater imaging sensitivity and mapping speed at this wavelength than has previously been possible. We discuss the overall instrument design, including our second‐generation cryogenic optical and detector subsystem.
- Published
- 2009
23. Instrument performance of GISMO, a 2 millimeter TES bolometer camera used at the IRAM 30 m Telescope
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Dominic J. Benford, Johannes Staguhn, Timothy M. Miller, Christine A. Allen, Edward J. Wollack, R. G. Arendt, A. Sievers, David T. Chuss, Troy Ames, Elmer Sharp, D. J. Fixsen, S. Harvey Moseley, Stephen F. Maher, S. Navarro, and E. Dwek
- Subjects
Physics ,Galactic astronomy ,business.industry ,Bolometer ,Astronomy ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Large format ,Redshift ,law.invention ,Telescope ,Optics ,Observational astronomy ,law ,Spectral energy distribution ,Millimeter ,business ,Astrophysics::Galaxy Astrophysics - Abstract
In November of 2007 we demonstrated a monolithic Backshort-Under-Grid (BUG) 8x16 array in the field using our 2 mm wavelength imager GISMO (Goddard IRAM Superconducting 2 Millimeter Observer) at the IRAM 30 m telescope in Spain for astronomical observations. The 2 mm spectral range provides a unique terrestrial window enabling ground-based observations of the earliest active dusty galaxies in the universe and thereby allowing a better constraint on the star formation rate in these objects. The optical design incorporates a 100 mm diameter silicon lens cooled to 4 K, which provides the required fast beam yielding 0.9 lambda/D pixels. With this spatial sampling, GISMO will be very efficient at detecting sources serendipitously in large sky surveys, while the capability for diffraction limited imaging is preserved. The camera provides significantly greater detection sensitivity and mapping speed at this wavelength than has previously been possible. The instrument will fill in the spectral energy distribution of high redshift galaxies at the Rayleigh-Jeans part of the dust emission spectrum, even at the highest redshifts. Here1 will we present early results from our observing run with the first fielded BUG bolometer array. We have developed key technologies to enable highly versatile, kilopixel, infrared through millimeter wavelength bolometer arrays. The Backshort-Under-Grid (BUG) array consists of three components: 1) a transition-edge-sensor (TES) based bolometer array with background-limited sensitivity and high filling factor, 2) a quarter-wave reflective backshort grid providing high optical efficiency, and 3) a superconducting bump-bonded large format Superconducting Quantum Interference Device (SQUID) multiplexer readout. The array is described in more detail elsewhere (Allen et al., this conference). In November of 2007 we demonstrated a monolithic 8x 16 array with 2 mm-pitch detectors in the field using our 2 mm wavelength imager GISMO (Goddard IRAM Superconducting 2 Millimeter Observer) at the IRAM 30 m telescope in Spain for astronomical observations. The 2 mm spectral range provides a unique terrestrial window enabling ground-based observations of the earliest active dusty galaxies in the universe and thereby allowing a better constraint on the star formation rate in these objects. The optical design incorporates a 100 mm diameter silicon lens cooled to 4 K, which provides the required fast beam yielding 0.9 lambda1D pixels. With this spatial sampling, GISMO will be very efficient at detecting sources serendipitously in large sky surveys, while the capability for diffraction limited imaging is preserved. The camera provides significantly greater detection sensitivity and mapping speed at this wavelength than has previously been possible. The instrument will fill in the spectral energy distribution of high redshift galaxies at the Rayleigh-Jeans part of the dust emission spectrum, even at the highest redshifts. Here I will we present early results from our observing run with the first fielded BUG bolometer array.
- Published
- 2008
24. MUSTANG: 90 GHz science with the Green Bank Telescope
- Author
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Dominic J. Benford, Troy Ames, Kent D. Irwin, Brian Mason, Peter A. R. Ade, James A. Chervenak, D. J. Tally, Simon Dicker, Stephen F. Maher, Samuel H. Moseley, Carole Tucker, S. White, W. D. Cotton, James E. Aguirre, Mark J. Devlin, Phillip Korngut, Enectali Figueroa-Feliciano, T. C. Chen, and M. Mello
- Subjects
Physics ,Bolometer ,Green Bank Telescope ,FOS: Physical sciences ,High resolution ,01 natural sciences ,Focal Plane Arrays ,law.invention ,010309 optics ,Telescope ,Radio telescope ,law ,0103 physical sciences ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,Transition edge ,Remote sensing - Abstract
MUSTANG is a 90 GHz bolometer camera built for use as a facility instrument on the 100 m Robert C. Byrd Green Bank radio telescope (GBT). MUSTANG has an 8 by 8 focal plane array of transition edge sensor bolometers read out using time-domain multiplexed SQUID electronics. As a continuum instrument on a large single dish MUSTANG has a combination of high resolution (8") and good sensitivity to extended emission which make it very competitive for a wide range of galactic and extragalactic science. Commissioning finished in January 2008 and some of the first science data have been collected., 9 Pages, 5 figures, Presented at the SPIE conference on astronomical instrumentation in 2008
- Published
- 2008
25. Design and performance of a high-throughput cryogenic detector system
- Author
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Elmer Sharp, Dale J. Fixsen, Catherine T. Marx, Stephen F. Maher, Dominic J. Benford, Edward J. Wollack, and Johannes Staguhn
- Subjects
Physics ,Stray light ,business.industry ,Bolometer ,Detector ,Particle detector ,law.invention ,Lens (optics) ,Telescope ,Optics ,Band-pass filter ,law ,Optoelectronics ,Millimeter ,business - Abstract
Keywords: GISMO, Optical Design, High-throughput, Detector System, IRAMThe Goddard IRAM Superconducting Millimeter Observer (GISMO) is a new superconducting bolometer array camerafor the IRAM 30 Meter Telescope on Pico Veleta, Spain. GISMO uses a 3He/4He cooler mounted to a liquid He/LN2cryostat to cool the bolometer array and SQUID electronics to an operating temperature of 260mK. The bolometer arrayis based on the backshort-under-grid architecture and features 128 2mm square absorbing pixels. A 101mm diameteranti-reflection coated silicon lens is used to define the beam. A single cold pupil stop prevents warm radiation fromreaching the array, but no other stops are used. In the beam, filters and a cold baffling and stray light suppression systemwere used to define the bandpass and prevent out-of-band radiation to a very high level, including out-of-band radiationleaking through the metal-mesh filters from extreme angles. We present a detailed description of this optical design andits performance. A comprehensive report of the electronics and cryogenic integration are also included.
- Published
- 2008
26. The wide-field imaging interferometry testbed: enabling techniques for high angular resolution astronomy
- Author
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Stephen A. Rinehart, Stephen F. Maher, John Jung, Thomas A. Pauls, David Leisawitz, Thomas Armstrong, Bradley J. Frey, Douglas B. Leviton, Anthony J. Martino, Jeff Kirk, and Richard G. Lyon
- Subjects
Physics ,business.industry ,Real-time computing ,Testbed ,Field of view ,Iterative reconstruction ,Automation ,Interferometry ,Data acquisition ,Data quality ,Computer vision ,Artificial intelligence ,business ,Image restoration - Abstract
The Wide-Field Imaging Interferometry Testbed (WIIT) was designed to develop techniques for wide-field of view imaging interferometry, using "double-Fourier" methods. These techniques will be important for a wide range of future space-based interferometry missions. We have provided simple demonstrations of the methodology already, and continuing development of the testbed will lead to higher data rates, improved data quality, and refined algorithms for image reconstruction. At present, the testbed effort includes five lines of development; automation of the testbed, operation in an improved environment, acquisition of large high-quality datasets, development of image reconstruction algorithms, and analytical modeling of the testbed. We discuss the progress made towards the first four of these goals; the analytical modeling is discussed in a separate paper within this conference.
- Published
- 2007
27. MUSTANG. First light and current status
- Author
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Phillip Korngut, Enectali Figueroa-Feliciano, Mark J. Devlin, Brian Mason, S. White, Dominic J. Benford, Samuel H. Moseley, B. A. Werner, Stephen F. Maher, Troy Ames, J. Aguirre, Roger D. Norrod, D. J. Tally, John Abrahams, T. C. Chen, Simon Dicker, Kent D. Irwin, W. D. Cotton, Peter A. R. Ade, Carole Tucker, Johannes G. Staguhn, Jay Chervenak, and M. Mello
- Subjects
Physics ,business.industry ,media_common.quotation_subject ,Bolometer ,Astronomy ,First light ,law.invention ,Radio telescope ,Telescope ,Optics ,Cardinal point ,Sky ,law ,Transition edge sensor ,business ,Noise (radio) ,media_common - Abstract
MUSTANG is a 90 GHz bolometer camera built for use as a facility instrument on the 100 m Green Bank radio telescope (GBT). MUSTANG has an 8 by 8 focal plane array of transition edge sensor bolometers read out using time-multiplexed SQUID electronics. On the GBT each pixel has an 8" beam size. In one hour we expect to be able to map a 15' square of sky to 0.2 mjy/beam RMS making MUSTANG on the GBT a very competitive instrument capable of a wide range of galactic and extragalactic science. In September 2006 MUSTANG had first light and became the first instrument to use the GBT at 90 GHz. During two months of subsequent testing we showed that MUSTANG behaved as well on the telescope as it did in the lab. Observations were made of many astronomical sources including Saturn and the star forming region W3. We were able to confirm our beam shape and different observing strategies were tested. Procedures were put in place for pointing and focusing and a data analysis pipeline was set up. Several problems were identified during commissioning and are currently being addressed. One of these, excessive 1/f noise, has already been solved and we plan to take our first science observations in late 2007.
- Published
- 2007
28. First astronomical images with a multiplexed superconducting bolometer array
- Author
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Christine A. Allen, Troy Ames, Johannes G. Staguhn, James A. Chervenak, Dominic J. Benford, Stephen F. Maher, C. Rioux, George M. Voellmer, Richard A. Shafer, Sebastien Lefranc, Catherine R. Kennedy, François Pajot, and S. Harvey Moseley
- Subjects
Physics ,Spectrometer ,Physics::Instrumentation and Detectors ,business.industry ,Bolometer ,Detector ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,law.invention ,SQUID ,Caltech Submillimeter Observatory ,Interferometry ,Optics ,law ,Optoelectronics ,Transition edge sensor ,Spectral resolution ,business ,Astrophysics::Galaxy Astrophysics - Abstract
We present images taken with the first deployed astronomical instrument to use multiplexed superconducting bolometers. The Fabry-Perot Interferometer Bolometer Research Experiment (FIBRE), a broadband submillimeter spectrometer, took these images as a detector investigation at the Caltech Submillimeter Observatory (CSO). FIBRE's detectors are superconducting bilayer transition edge sensor (TES) bolometers read out by a SQUID multiplexer. An order-sorted Fabry-Perot provides illumination of a 16-element linear bolometer array, resulting in five orders at a spectral resolution of around 1200 covering the 350 micron atmospheric band. We present multiwavelength images of Jupiter, Venus and the high-mass star-forming region G34.3+0.2 taken with this instrument at several wavelengths in the 350 micron band, separated by approximately 8 microns. These images have validated the use of multiplexed superconducting bolometers in an astronomical application and have helped inform the design of our future instruments.
- Published
- 2006
29. GISMO: a 2-millimeter bolometer camera for the IRAM 30 m telescope
- Author
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Edward J. Wollack, S. Navarro, Christine A. Allen, Walter Brunswig, Eli Dwek, David T. Chuss, Troy Ames, Stephen F. Maher, Timothy M. Miller, Elmer Sharp, Catherine T. Marx, S. Harvey Moseley, Johannes G. Staguhn, and Dominic J. Benford
- Subjects
Physics ,Galactic astronomy ,Star formation ,Bolometer ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Quasar ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Redshift ,Galaxy ,law.invention ,Telescope ,law ,Infrared window ,Astrophysics::Galaxy Astrophysics - Abstract
We are building a bolometer camera (the Goddard-Iram Superconducting 2-Millimeter Observer, GISMO) for operation in the 2 mm atmospheric window to be used at the IRAM 30 m telescope. The instrument uses a 8x16 planar array of multiplexed TES bolometers which incorporates our newly designed Backshort Under Grid (BUG) architecture. Due to the size and sensitivity of the detector array (the NEP of the detectors is 4×10-17 W/√Hz), this instrument will be unique in that it will be capable of providing significantly greater imaging sensitivity and mapping speed at this wavelength than has previously been possible. The major scientific driver for this instrument is to provide the IRAM 30 m telescope with the capability to rapidly observe galactic and extragalactic dust emission, in particular from high-z ULIRGs and quasars, even in the summer season. The 2 mm spectral range provides a unique window to observe the earliest active dusty galaxies in the universe and is well suited to better confine the star formation rate in these objects. The instrument will fill in the SEDs of high redshift galaxies at the Rayleigh-Jeans part of the dust emission spectrum, even at the highest redshifts. The observational efficiency of a 2 mm camera with respect to bolometer cameras operating at shorter wavelengths increases for objects at redshifts beyond z ~ 1 and is most efficient at the highest redshifts, at the time when the first stars were re-ionizing the universe. Our models predict that at this wavelength one out of four serendipitously detected galaxies will be at a redshift of z > 6.5.
- Published
- 2006
30. Language through gesture in a VRML world
- Author
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Sarah Geitz, Diane Brentari, Stephen F. Maher, and Chai-hi Park
- Subjects
Computer science ,Computer graphics (images) ,VRML ,computer.file_format ,computer ,Gesture - Published
- 1998
31. Computer generated 3-dimensional models of manual alphabet handshapes for the World Wide Web
- Author
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Timothy Hanson, Stephen F. Maher, and Sarah Geitz
- Subjects
American Sign Language ,Computer science ,computer.file_format ,Virtual reality ,language.human_language ,Conjunction (grammar) ,World Wide Web ,Teaching tool ,Computer graphics (images) ,VRML ,ComputingMethodologies_DOCUMENTANDTEXTPROCESSING ,language ,Alphabet ,computer ,ComputingMethodologies_COMPUTERGRAPHICS - Abstract
A teaching tool consisting of a collection of three dimensional computer graphic models representing American Sign Language manual alphabet hand shapes in various locations and orientations has been established. These computer graphic models have been recorded in the "Virtual Reality Modeling Language (VRML) [1] for display with World Wide Web browsers such as Netscape or Mosaic, in conjunction with VRML browsers such as WebSpace or WorldView".
- Published
- 1996
32. THE RADIO-2 mm SPECTRAL INDEX OF THE CRAB NEBULA MEASURED WITH GISMO
- Author
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Brian Mason, S. Navarro, Christine A. Jhabvala, Dale J. Fixsen, R. G. Arendt, Timothy M. Miller, Kent D. Irwin, Edward J. Wollack, Samuel H. Moseley, J. V. George, Stephen F. Maher, Johannes Staguhn, Elmer Sharp, Mark J. Devlin, Jonathan Sievers, A. Sievers, Dominic J. Benford, Simon Dicker, Attila Kovács, and Phillip Korngut
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,law.invention ,Telescope ,law ,0103 physical sciences ,010306 general physics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,Spectral index ,Nebula ,Bolometer ,Astrophysics::Instrumentation and Methods for Astrophysics ,Green Bank Telescope ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Synchrotron ,Crab Nebula ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Millimeter ,Astrophysics::Earth and Planetary Astrophysics - Abstract
We present results of 2 mm observations of the Crab Nebula, obtained using the Goddard-IRAM Superconducting 2 Millimeter Observer (GISMO) bolometer camera on the IRAM 30 m telescope. Additional 3.3 mm observations with the MUSTANG bolometer array on the Green Bank Telescope are also presented. The integrated 2 mm flux density of the Crab Nebula provides no evidence for the emergence of a second synchrotron component that has been proposed. It is consistent with the radio power law spectrum, extrapolated up to a break frequency of log(nu_{b} [GHz]) = 2.84 +/- 0.29 or nu_{b} = 695^{+651}_{-336} GHz. The Crab Nebula is well-resolved by the ~16.7" beam (FWHM) of GISMO. Comparison to radio data at comparable spatial resolution enables us to confirm significant spatial variation of the spectral index between 21 cm and 2 mm. The main effect is a spectral flattening in the inner region of the Crab Nebula, correlated with the toroidal structure at the center of the nebula that is prominent in the near-IR through X-ray regime., Comment: Accepted for publication in the ApJ
- Published
- 2011
33. Virtual reality at NASA/Goddard Space Flight Center
- Author
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Stephen F. Maher and Jarrett Cohen
- Subjects
General Computer Science ,Computer science ,Computer graphics (images) ,Center (algebra and category theory) ,Virtual reality ,Space (commercial competition) ,Computer Graphics and Computer-Aided Design - Published
- 1996
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