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Seven gallium doped germanium (Ge:Ga) photoconductive infrared detectors were fabricated and mounted in integrating cavities. In addition, a cold preamplifier package consisting of J230 junction field effect transistors (JFETs) was produced. Tests of the system under low photon background conditions indicated that sensitivity was limited by the Johnson noise of the load resistor. The detectors were mounted in the Ames cooled grating spectrometer, and flown on the Kuiper Airborne Observatory. Good quality astronomical data were obtained during the flight of 7 July 1983.

Seven gallium doped germanium (Ge:Ga) photoconductive infrared detectors were fabricated and mounted in integrating cavities. In addition, a cold preamplifier package consisting of J230 junction field effect transistors (JFETs) was produced. Tests of the system under low photon background conditions indicated that sensitivity was limited by the Johnson noise of the load resistor. The detectors were mounted in the Ames cooled grating spectrometer, and flown on the Kuiper Airborne Observatory. Good quality astronomical data were obtained during the flight of 7 July 1983.

Seven gallium doped germanium (Ge:Ga) photoconductive infrared detectors were fabricated and mounted in integrating cavities. In addition, a cold preamplifier package consisting of J230 junction field effect transistors (JFETs) was produced. Tests of the system under low photon background conditions indicated that sensitivity was limited by the Johnson noise of the load resistor. The detectors were mounted in the Ames cooled grating spectrometer, and flown on the Kuiper Airborne Observatory. Good quality astronomical data were obtained during the flight of 7 July 1983.

Seven gallium doped germanium (Ge:Ga) photoconductive infrared detectors were fabricated and mounted in integrating cavities. In addition, a cold preamplifier package consisting of J230 junction field effect transistors (JFETs) was produced. Tests of the system under low photon background conditions indicated that sensitivity was limited by the Johnson noise of the load resistor. The detectors were mounted in the Ames cooled grating spectrometer, and flown on the Kuiper Airborne Observatory. Good quality astronomical data were obtained during the flight of 7 July 1983.

Seven gallium doped germanium (Ge:Ga) photoconductive infrared detectors were fabricated and mounted in integrating cavities. In addition, a cold preamplifier package consisting of J230 junction field effect transistors (JFETs) was produced. Tests of the system under low photon background conditions indicated that sensitivity was limited by the Johnson noise of the load resistor. The detectors were mounted in the Ames cooled grating spectrometer, and flown on the Kuiper Airborne Observatory. Good quality astronomical data were obtained during the flight of 7 July 1983.

Seven gallium doped germanium (Ge:Ga) photoconductive infrared detectors were fabricated and mounted in integrating cavities. In addition, a cold preamplifier package consisting of J230 junction field effect transistors (JFETs) was produced. Tests of the system under low photon background conditions indicated that sensitivity was limited by the Johnson noise of the load resistor. The detectors were mounted in the Ames cooled grating spectrometer, and flown on the Kuiper Airborne Observatory. Good quality astronomical data were obtained during the flight of 7 July 1983.

Seven gallium doped germanium (Ge:Ga) photoconductive infrared detectors were fabricated and mounted in integrating cavities. In addition, a cold preamplifier package consisting of J230 junction field effect transistors (JFETs) was produced. Tests of the system under low photon background conditions indicated that sensitivity was limited by the Johnson noise of the load resistor. The detectors were mounted in the Ames cooled grating spectrometer, and flown on the Kuiper Airborne Observatory. Good quality astronomical data were obtained during the flight of 7 July 1983.

262 pages : 28 cm

Stratospheric Observatory for Infrared Astronomy ED10-0182-03 A NASA F/A-18 mission support aircraft flies close beside NASA's Stratospheric Observatory for Infrared Astronomy 747SP during a high-altitude test flight in preparation for Early Science missions. The second series of flight envelope-expansion flight tests checked out operation of the SOFIA's telescope cavity doors and mission systems at increasingly higher altitudes and air speeds. When flight tests are completed, the SOFIA will be a fully capable observatory cleared for astronomical science missions at up to 45,000 feet altitude. July 13, 2010 (NASA photo / Jim Ross)

Includes bibliography

Includes bibliography

Includes bibliography

Montgomery College is a public, multicampus community college in Montgomery County, Maryland. Montgomery College serves nearly 60,000 students a year, through both credit and noncredit programs, in more than 100 areas of study.

Popular Astronomy 1943-08: Volume 51 , Issue 7. Digitized from IA1520728-01 . Previous issue: sim_popular-astronomy_1943-06_51_6 . Next issue: sim_popular-astronomy_1943-10_51_8 .

Digitized spark chamber detector development for satellite and balloon-borne gamma ray astronomy

Digitized spark chamber detector development for satellite and balloon-borne gamma ray astronomy

The objective is the continuation of a long-term research program designed to study the composition, structure and processes operating on the surfaces of solar system objects using the Mauna Kea Observatory with techniques and modern instrumentation. Reflectance spectroscopy and multispectral imaging in the spectral region, 0.3 to 5.0 micrometer are the major techniques used, although thermal (10 micrometer and 20 micrometer) radiometry are used in some aspects of the research. Some specific projects include: (1) systematic spectral imaging observations of the Moon; (2) systematic spectral imaging and spectral monitoring of the Martian surface; (3) thermal radiometry of asteroids as part of the IRAS follow-up and other target specific programs; (4) searches for asteroid satellites and dust belts using a stellar coronagraph; and (5) studies of circumstellar disks using a stellar coronagraph. Progress for each of the programs included is discussed. minerals; (2) completed observations of lunar multi-ringed basins and crater deposits in search of high-Ca spectral anomalies; (3) completed data reduction of an additional 5 asteroids observed by the coronagraphic technique in the search for asteroids satellites and debris clouds; and (4) completed the reduction and calibration of 350 asteroids observed at 10 micron and 20 micron using the NASA IRTF.

Backup or supporting data for the design analyses and trade studies which defined the astronomy sortie missions are presented. The subjects discussed are: (1) configuration of space shuttle orbiter, (2) electronic subsystems, (3) electric power requirements, and (4) payload requirements. Mathematical models are developed to illustrate the orbital rendezvous capabilities.

This report reviews the astronomy research carried out at The Aerospace Corporation during 1974. The report describes the activities of the San Fernando Observatory, the research in millimeter wave radio astronomy as well as the space astronomy research.

This report reviews the astronomy research carried out at The Aerospace Corporation during 1974. The report describes the activities of the San Fernando Observatory, the research in millimeter wave radio astronomy as well as the space astronomy research.

Astronomy Software for Windows These applications work with Windows XP-Win7

Astronomy Software for Windows These applications work with Windows XP-Win7

Like the Crab Nebula, the Vela Supernova Remnant has a radio pulsar at its center. In this image taken by the High Energy Astronomy Observatory (HEAO)-2/Einstein Observatory, the pulsar appears as a point source surrounded by weak and diffused emissions of x-rays. HEAO-2's computer processing system was able to record and display the total number of x-ray photons (a tiny bundle of radiant energy used as the fundamental unit of electromagnetic radiation) on a scale along the margin of the picture. The HEAO-2, the first imaging and largest x-ray telescope built to date, was capable of producing actual photographs of x-ray objects. Shortly after launch, the HEAO-2 was nicknamed the Einstein Observatory by its scientific experimenters in honor of the centernial of the birth of Albert Einstein, whose concepts of relativity and gravitation have influenced much of modern astrophysics, particularly x-ray astronomy. The HEAO-2, designed and developed by TRW, Inc. under the project management of the Marshall Space Flight Center, was launched aboard an Atlas/Centaur launch vehicle on November 13, 1978.

Innovative & fascinating astronomy lab program.

Innovative & fascinating astronomy lab program.

Gamma-ray Bursts (GRBs) are relativistic cosmological beacons of transient high energy radiation whose afterglows span the electromagnetic spectrum. Theoretical expectations of correlated neutrino and/or gravitational wave (GW) emission position GRBs at an astrophysical nexus for a metamorphosis in our understanding of the Cosmos. This new dawn in the era of experimental (particle) astrophysics and cosmology is afforded by current and planned facilities enabling the novel astronomies of high energy neutrinos and gravitational waves, in concert with unprecedented electromagnetic coverage. In this white paper, we motivate GRBs as a compelling scientific theme and highlight key technical advances that may facilitate fundamental breakthroughs in the context of Swift, Fermi, IceCube and LIGO (Laser Interferometer Gravitational Wave Observatory), whose capabilities would be augmented with JANUS (Joint Astrophysics Nascent Universe Satellite), EXIST (Energetic X-ray Imaging Survey Telescope) and LISA (Laser Interferometer Space Antenna). Scientific synergy will be achieved by leveraging the combined sensitivity of contemporaneous ground-based and satellite observatories, thus optimizing their collective discovery potential for: (i) revealing the origin(s) and acceleration mechanism(s) of cosmic rays, (ii) exposing GRB progenitor(s) and (iii) exploring the high-z Cosmos. Hence, the advent of GRB multi-messenger astronomy may cement an explicit connection to fundamental physics, via nascent cosmic windows, throughout the next decade and beyond.

Despite their paucity, massive hot stars are real cosmic engines of fundamental importance in shaping our Universe, from its very early stages up to its current appearance. Understanding the physics of massive stars is then a key issue for many relevant astrophysical phenomena. Probing the massive stellar population of nearby galaxies by means of quantitative spectroscopy allows us to unveil a wealth of information that will aid our current understanding of stellar and galaxy evolution. In addition, blue luminous stars can be used as standard candles for extragalactic distances up to 10 Mpc. In this contribution, we present a brief overview of recent steps we have undertaken in this exciting research field.

SOFIA presents a number of interesting challenges for the development of a data reduction environment which, at its initial phase, will have to incorporate pipelines from seven different instruments. Therefore, the SOFIA data reduction software must run code which has been developed in a variety of dissimilar environments which will only increase in future generations of instrumentation. We investigated three distinctly different situations for performing pipelined data reduction in SOFIA: automated data reduction after data archival at the end of a mission, re-pipelining of science data with updated calibrations or optimum parameters, and the interactive user-driven local execution and analysis of data reduction by an investigator. These different modes would traditionally result in very different software implementations of algorithms used by each instrument team, in effect tripling the amount of data reduction software that would need to be maintained by SOFIA. We present here a unique approach for enfolding all the instrument-specific data reduction software in the observatory framework and verifies the needs for all three reduction scenarios as well as the standard visualization tools. The SOFIA data reduction structure would host the different algorithms and techniques that the instrument teams develop in their own environment. Ideally, duplication of software is minimized across the system because instrument teams can draw on software solutions and techniques previously delivered to SOFIA by other instruments. With this approach, we minimize the effort for analyzing and developing new software reduction pipelines for future generation instruments. We also explore the potential benefits of this approach in the portability of the software to an ever-broadening science audience, as well as its ability to ease the use of distributed processing for data reduction pipelines.

SOFIA presents a number of interesting challenges for the development of a data reduction environment which, at its initial phase, will have to incorporate pipelines from seven different instruments. Therefore, the SOFIA data reduction software must run code which has been developed in a variety of dissimilar environments which will only increase in future generations of instrumentation. We investigated three distinctly different situations for performing pipelined data reduction in SOFIA: automated data reduction after data archival at the end of a mission, re-pipelining of science data with updated calibrations or optimum parameters, and the interactive user-driven local execution and analysis of data reduction by an investigator. These different modes would traditionally result in very different software implementations of algorithms used by each instrument team, in effect tripling the amount of data reduction software that would need to be maintained by SOFIA. We present here a unique approach for enfolding all the instrument-specific data reduction software in the observatory framework and verifies the needs for all three reduction scenarios as well as the standard visualization tools. The SOFIA data reduction structure would host the different algorithms and techniques that the instrument teams develop in their own environment. Ideally, duplication of software is minimized across the system because instrument teams can draw on software solutions and techniques previously delivered to SOFIA by other instruments. With this approach, we minimize the effort for analyzing and developing new software reduction pipelines for future generation instruments. We also explore the potential benefits of this approach in the portability of the software to an ever-broadening science audience, as well as its ability to ease the use of distributed processing for data reduction pipelines.

SOFIA presents a number of interesting challenges for the development of a data reduction environment which, at its initial phase, will have to incorporate pipelines from seven different instruments. Therefore, the SOFIA data reduction software must run code which has been developed in a variety of dissimilar environments which will only increase in future generations of instrumentation. We investigated three distinctly different situations for performing pipelined data reduction in SOFIA: automated data reduction after data archival at the end of a mission, re-pipelining of science data with updated calibrations or optimum parameters, and the interactive user-driven local execution and analysis of data reduction by an investigator. These different modes would traditionally result in very different software implementations of algorithms used by each instrument team, in effect tripling the amount of data reduction software that would need to be maintained by SOFIA. We present here a unique approach for enfolding all the instrument-specific data reduction software in the observatory framework and verifies the needs for all three reduction scenarios as well as the standard visualization tools. The SOFIA data reduction structure would host the different algorithms and techniques that the instrument teams develop in their own environment. Ideally, duplication of software is minimized across the system because instrument teams can draw on software solutions and techniques previously delivered to SOFIA by other instruments. With this approach, we minimize the effort for analyzing and developing new software reduction pipelines for future generation instruments. We also explore the potential benefits of this approach in the portability of the software to an ever-broadening science audience, as well as its ability to ease the use of distributed processing for data reduction pipelines.

SOFIA presents a number of interesting challenges for the development of a data reduction environment which, at its initial phase, will have to incorporate pipelines from seven different instruments. Therefore, the SOFIA data reduction software must run code which has been developed in a variety of dissimilar environments which will only increase in future generations of instrumentation. We investigated three distinctly different situations for performing pipelined data reduction in SOFIA: automated data reduction after data archival at the end of a mission, re-pipelining of science data with updated calibrations or optimum parameters, and the interactive user-driven local execution and analysis of data reduction by an investigator. These different modes would traditionally result in very different software implementations of algorithms used by each instrument team, in effect tripling the amount of data reduction software that would need to be maintained by SOFIA. We present here a unique approach for enfolding all the instrument-specific data reduction software in the observatory framework and verifies the needs for all three reduction scenarios as well as the standard visualization tools. The SOFIA data reduction structure would host the different algorithms and techniques that the instrument teams develop in their own environment. Ideally, duplication of software is minimized across the system because instrument teams can draw on software solutions and techniques previously delivered to SOFIA by other instruments. With this approach, we minimize the effort for analyzing and developing new software reduction pipelines for future generation instruments. We also explore the potential benefits of this approach in the portability of the software to an ever-broadening science audience, as well as its ability to ease the use of distributed processing for data reduction pipelines.

SOFIA presents a number of interesting challenges for the development of a data reduction environment which, at its initial phase, will have to incorporate pipelines from seven different instruments. Therefore, the SOFIA data reduction software must run code which has been developed in a variety of dissimilar environments which will only increase in future generations of instrumentation. We investigated three distinctly different situations for performing pipelined data reduction in SOFIA: automated data reduction after data archival at the end of a mission, re-pipelining of science data with updated calibrations or optimum parameters, and the interactive user-driven local execution and analysis of data reduction by an investigator. These different modes would traditionally result in very different software implementations of algorithms used by each instrument team, in effect tripling the amount of data reduction software that would need to be maintained by SOFIA. We present here a unique approach for enfolding all the instrument-specific data reduction software in the observatory framework and verifies the needs for all three reduction scenarios as well as the standard visualization tools. The SOFIA data reduction structure would host the different algorithms and techniques that the instrument teams develop in their own environment. Ideally, duplication of software is minimized across the system because instrument teams can draw on software solutions and techniques previously delivered to SOFIA by other instruments. With this approach, we minimize the effort for analyzing and developing new software reduction pipelines for future generation instruments. We also explore the potential benefits of this approach in the portability of the software to an ever-broadening science audience, as well as its ability to ease the use of distributed processing for data reduction pipelines.

SOFIA presents a number of interesting challenges for the development of a data reduction environment which, at its initial phase, will have to incorporate pipelines from seven different instruments. Therefore, the SOFIA data reduction software must run code which has been developed in a variety of dissimilar environments which will only increase in future generations of instrumentation. We investigated three distinctly different situations for performing pipelined data reduction in SOFIA: automated data reduction after data archival at the end of a mission, re-pipelining of science data with updated calibrations or optimum parameters, and the interactive user-driven local execution and analysis of data reduction by an investigator. These different modes would traditionally result in very different software implementations of algorithms used by each instrument team, in effect tripling the amount of data reduction software that would need to be maintained by SOFIA. We present here a unique approach for enfolding all the instrument-specific data reduction software in the observatory framework and verifies the needs for all three reduction scenarios as well as the standard visualization tools. The SOFIA data reduction structure would host the different algorithms and techniques that the instrument teams develop in their own environment. Ideally, duplication of software is minimized across the system because instrument teams can draw on software solutions and techniques previously delivered to SOFIA by other instruments. With this approach, we minimize the effort for analyzing and developing new software reduction pipelines for future generation instruments. We also explore the potential benefits of this approach in the portability of the software to an ever-broadening science audience, as well as its ability to ease the use of distributed processing for data reduction pipelines.

PCN PACTV Community News Backyard Astronomy Dux Library New Telescope The Duxbury Free Library has caught on to a trend that is sweeping across libraries all over Massachusetts: Loaning out a telescope the way you would take out a book. The program started in New Hampshire by the New Hampshire Society in 2008. The Aldrich Astronomical Society out of Paxton, MA took it upon themselves to initiate the program here in the Bay State a little over three years ago and it’s continued to blossom ever since

PCN PACTV Community News Backyard Astronomy Dux Library New Telescope The Duxbury Free Library has caught on to a trend that is sweeping across libraries all over Massachusetts: Loaning out a telescope the way you would take out a book. The program started in New Hampshire by the New Hampshire Society in 2008. The Aldrich Astronomical Society out of Paxton, MA took it upon themselves to initiate the program here in the Bay State a little over three years ago and it’s continued to blossom ever since

PCN PACTV Community News Backyard Astronomy Dux Library New Telescope The Duxbury Free Library has caught on to a trend that is sweeping across libraries all over Massachusetts: Loaning out a telescope the way you would take out a book. The program started in New Hampshire by the New Hampshire Society in 2008. The Aldrich Astronomical Society out of Paxton, MA took it upon themselves to initiate the program here in the Bay State a little over three years ago and it’s continued to blossom ever since

Star Gazer Astronomy (Disk 1)

GAAC Meeting, Friday, November 12, 2021, with Guest Speaker Kelly Beatty, science writer and Senior Editor at Sky & Telescope magazine, and his compelling story of the discovery of Pluto, its eventual demotion, and the New Horizons mission to the dwarf planet. ---------------------------------------------------------- 1623 Studios is a #nonprofit organization dedicated to producing community programming for #CapeAnn—Gloucester, Rockport, Manchester-by-the-Sea, and Essex—and to providing a forum for the free exchange of information and ideas. We also provide a full spectrum of creative services to support our mission. Learn more at https://1623studios.org

GAAC Meeting, Friday, November 12, 2021, with Guest Speaker Kelly Beatty, science writer and Senior Editor at Sky & Telescope magazine, and his compelling story of the discovery of Pluto, its eventual demotion, and the New Horizons mission to the dwarf planet. ---------------------------------------------------------- 1623 Studios is a #nonprofit organization dedicated to producing community programming for #CapeAnn—Gloucester, Rockport, Manchester-by-the-Sea, and Essex—and to providing a forum for the free exchange of information and ideas. We also provide a full spectrum of creative services to support our mission. Learn more at https://1623studios.org

SOFIA is a 2.5 meter airborne infrared telescope, mounted in a Boeing 747SP aircraft. Due to the large size of the telescope, only a few degrees of azimuth are available at the telescope bearing. This means the heading of the aircraft is fundamentally associated with the telescope's observation targets, and the ground track necessary to enable a given mission is highly complex and dependent on the coordinates, duration, and order of observations to be performed. We have designed and implemented a Flight Management Infrastructure (FMI) product in order to plan and execute such missions in the presence of a large number of external constraints (e.g. restricted airspace, international boundaries, elevation limits of the telescope, aircraft performance, winds at altitude, and ambient temperatures). We present an overview of the FMI, including the process, constraints and basic algorithms used to plan and execute SOFIA missions.

Modern Terrestrial Cerenkov Telescopes and Array Scintillators facing the Horizons may soon reveal far Cosmic Rays or nearer PeVs-EeVs Neutrino Showers Astronomy. Indeed UHE neutrino interactions in air, leading to Horizontal Showers, may take place through several channels: the main Glashow resonant one, the charged nuclear interactions and the neutral current events. Analogous events occur also for the neutrino-nucleon events. These interactions are producing hadronic or electromagnetic showers at the far horizons and their correlated secondaries Cerenkov flashes. Comparable interactions are producing, inside the Earth, the Horizontal, but Up-going ultra-relativistic tau, whose decay in flight is source of tau Air Showers (Uptaus and HorTaus); Horizontal Tau Air-Showers are rarely (one-two order of magnitude) enhanced by highest mountain chains at horizons, as in AUGER experimental site; their hadronic or electromagnetic traces are preferentially at PeV-EeV energies; their tracks are amplified by their muon-gamma bundles whose signals are above the random noises and better disentangled by Cerenkov flashes in time coincidence. More exotic UHE SUSY interactions at tens PeVs-EeV energy may blaze at Horizons. Anyway common High Energy Cosmic rays at PeVs-EeVs energy must traces their presence in Magic-like Cerenkov Telescopes at horizons. Present Magic Telescopes facing the Horizons are, at equal given time, almost comparable with the Amanda underground neutrino detector.

The new 1-m f/4 fast-slew Zadko Telescope was installed in June 2008 about 70 km north of Perth, Western Australia. It is the only metre-class optical facility at this southern latitude between the east coast of Australia and South Africa, and can rapidly image optical transients at a longitude not monitored by other similar facilities. We report on first imaging tests of a pilot program of minor planet searches, and Target of Opportunity observations triggered by the Swift satellite. In 12 months, 6 gamma-ray burst afterglows were detected, with estimated magnitudes; two of them, GRB 090205 (z = 4.65) and GRB 090516 (z = 4.11), are among the most distant optical transients imaged by an Australian telescope. Many asteroids were observed in a systematic 3-month search. In September 2009, an automatic telescope control system was installed, which will be used to link the facility to a global robotic telescope network; future targets will include fast optical transients triggered by highenergy satellites, radio transient detections, and LIGO gravitational wave candidate events. We also outline the importance of the facility as a potential tool for education, training, and public outreach.