Infrared Telescope in Antarctica
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REVIEW ARTICLE the NASA Spitzer Space Telescope
REVIEW OF SCIENTIFIC INSTRUMENTS 78, 011302 ͑2007͒ REVIEW ARTICLE The NASA Spitzer Space Telescope ͒ R. D. Gehrza Department of Astronomy, School of Physics and Astronomy, 116 Church Street, S.E., University of Minnesota, Minneapolis, Minnesota 55455 ͒ T. L. Roelligb NASA Ames Research Center, MS 245-6, Moffett Field, California 94035-1000 ͒ M. W. Wernerc Jet Propulsion Laboratory, California Institute of Technology, MS 264-767, 4800 Oak Grove Drive, Pasadena, California 91109 ͒ G. G. Faziod Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 ͒ J. R. Houcke Astronomy Department, Cornell University, Ithaca, New York 14853-6801 ͒ F. J. Lowf Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, Arizona 85721 ͒ G. H. Riekeg Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, Arizona 85721 ͒ ͒ B. T. Soiferh and D. A. Levinei Spitzer Science Center, MC 220-6, California Institute of Technology, 1200 East California Boulevard, Pasadena, California 91125 ͒ E. A. Romanaj Jet Propulsion Laboratory, California Institute of Technology, MS 264-767, 4800 Oak Grove Drive, Pasadena, California 91109 ͑Received 2 June 2006; accepted 17 September 2006; published online 30 January 2007͒ The National Aeronautics and Space Administration’s Spitzer Space Telescope ͑formerly the Space Infrared Telescope Facility͒ is the fourth and final facility in the Great Observatories Program, joining Hubble Space Telescope ͑1990͒, the Compton Gamma-Ray Observatory ͑1991–2000͒, and the Chandra X-Ray Observatory ͑1999͒. Spitzer, with a sensitivity that is almost three orders of magnitude greater than that of any previous ground-based and space-based infrared observatory, is expected to revolutionize our understanding of the creation of the universe, the formation and evolution of primitive galaxies, the origin of stars and planets, and the chemical evolution of the universe. -
Semiconductor Detectors and Focal Plane Arrays for Far-Infrared Imaging
OPTO−ELECTRONICS REVIEW 21(4), 406–426 DOI: 10.2478/s11772−013−0110−x Semiconductor detectors and focal plane arrays for far-infrared imaging A. ROGALSKI* Institute of Applied Physics, Military University of Technology, 2 Kaliskiego Str., 00–908 Warsaw, Poland The detection of far−infrared (far−IR) and sub−mm−wave radiation is resistant to the commonly employed techniques in the neighbouring microwave and IR frequency bands. In this wavelength detection range the use of solid state detectors has been hampered for the reasons of transit time of charge carriers being larger than the time of one oscillation period of radiation. Also the energy of radiation quanta is substantially smaller than the thermal energy at room temperature and even liquid ni− trogen temperature. The realization of terahertz (THz) emitters and receivers is a challenge because the frequencies are too high for conventional electronics and the photon energies are too small for classical optics. Development of semiconductor focal plane arrays started in seventies last century and has revolutionized imaging sys− tems in the next decades. This paper presents progress in far−IR and sub−mm−wave semiconductor detector technology of fo− cal plane arrays during the past twenty years. Special attention is given on recent progress in the detector technologies for real−time uncooled THz focal plane arrays such as Schottky barrier arrays, field−effect transistor detectors, and micro− bolometers. Also cryogenically cooled silicon and germanium extrinsic photoconductor arrays, and semiconductor bolome− ter arrays are considered. Keywords: THz detectors, focal plane arrays, Schottky barrier diodes, semiconductor hot electron bolometers, extrinsic photodetectors, performance limits. -
The PLATO Antarctic Site Testing Observatory
PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie The PLATO Antarctic site testing observatory J. S. Lawrence, G. R. Allen, M. C. B. Ashley, C. Bonner, S. Bradley, et al. J. S. Lawrence, G. R. Allen, M. C. B. Ashley, C. Bonner, S. Bradley, X. Cui, J. R. Everett, L. Feng, X. Gong, S. Hengst, J. Hu, Z. Jiang, C. A. Kulesa, Y. Li, D. Luong-Van, A. M. Moore, C. Pennypacker, W. Qin, R. Riddle, Z. Shang, J. W. V. Storey, B. Sun, N. Suntzeff, N. F. H. Tothill, T. Travouillon, C. K. Walker, L. Wang, J. Yan, J. Yang, H. Yang, D. York, X. Yuan, X. G. Zhang, Z. Zhang, X. Zhou, Z. Zhu, "The PLATO Antarctic site testing observatory," Proc. SPIE 7012, Ground-based and Airborne Telescopes II, 701227 (10 July 2008); doi: 10.1117/12.787166 Event: SPIE Astronomical Telescopes + Instrumentation, 2008, Marseille, France Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 7/12/2018 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use The PLATO Antarctic site testing observatory J.S. Lawrence*a, G.R. Allenb, M.C.B. Ashleya, C. Bonnera, S. Bradleyc, X. Cuid, J.R. Everetta, L. Fenge, X. Gongd, S. Hengsta, J.Huf, Z. Jiangf, C.A. Kulesag, Y. Lih, D. Luong-Vana, A.M. Moorei, C. Pennypackerj, W. Qinh, R. Riddlek, Z. Shangl, J.W.V. Storeya, B. Sunh, N. Suntzeffm, N.F.H. Tothilln, T. Travouilloni, C.K. Walkerg, L. Wange/m, J. Yane/f, J. Yange, H.Yangh, D. Yorko, X. Yuand, X.G. -
The Space Infrared Telescope Facility (SIRTF)
header for SPIE use The Space Infrared Telescope Facility (SIRTF) James Fansona, Giovanni Faziob, James Houckc, Tim Kellyd, George Riekee, Domenick Tenerellif, and Milt Whittenf aJet Propulsion Laboratory, California Institute of Technology, Pasadena CA 91109 bSmithsonian Astrophysical Observatory, Cambridge, MA 02138 cCornell University, Ithaca, NY, 14853 dBall Aerospace and Technologies Corp., Boulder, CO 80301 eUniversity of Arizona, Tucson, AZ, 85721 fLockheed Martin Missiles and Space Co., Sunnyvale, CA 94089 ABSTRACT This paper describes the design of the Space Infrared Telescope Facility (SIRTF) as the project enters the detailed design phase. SIRTF is the fourth of NASA’s Great Observatories, and is scheduled for launch in December 2001. SIRTF provides background limited imaging and spectroscopy covering the spectral range from 3 to 180 mm, complementing the capabilities of the other Great Observatories – the Hubble Space Telescope (HST), the Advanced X-ray Astrophysics Facility (AXAF), and the Compton Gamma Ray Observatory (CGRO). SIRTF will be the first mission to combine the high sensitivity achievable from a cryogenic space telescope with the imaging and spectroscopic power of the new generation of infrared detector arrays. The scientific capabilities of this combination are so great that SIRTF was designated the highest priority major mission for all of US astronomy in the 1990s. Keywords: telescope, cryogenic, infrared, astronomy, astrophysics, Great Observatory 1. INTRODUCTION The SIRTF mission has experienced dramatic evolution in both architecture and mission design. Originally conceived as a low Earth orbiting observatory serviced by astronauts from the Space Shuttle, SIRTF passed through a phase in high Earth orbit using first the Titan and later the smaller Atlas launch vehicle, to the current concept of a deep-space mission orbiting the sun, and using the still smaller Delta launch vehicle. -
(IRAS) Infrared Telescope in Space How Does It Work?
INSTRUCTIONS ARE ON PAGE 7 Infrared Astronomical Satellite (IRAS) Infrared telescope in space How does it work? http://sciencing.com/infrared-telescope-work-4926827.html Infrared telescopes use the same components and follow the same principles as visible light telescopes; they use a combination of lenses and mirrors to gather and focus radiation onto special detectors and then the data is translated by computer into useful information. The detectors are usually a collection of specialized solid-state digital devices: often the material for these is the superconductor alloy HgCdTe (mercury cadmium telluride). The entire telescope has to be kept to a temperature of just a few degrees above absolute zero because otherwise the telescope itself would emit infrared radiation (heat) which would interfere with the observations. Mission/uses http://coolcosmos.ipac.caltech.edu/cosmic_classroom/cosmi c_reference/irastro_history.html IRAS was successfully launched on January 25, 1983. It revealed that some young stars have disks of minute, solid dust particles, suggesting that such stars are in the process of forming planetary systems. (It can detect the early formation of stars) It has discovered 6 new galaxies It can detect radiation thought to be from the merge of 2 galaxies. Swift satellite Gamma ray telescope based in space How does it work? https://www.reference.com/science/gamma-ray-telescope-work- bcddbfeaa873cdd2# Gamma ray telescopes operate on satellites and carry special detectors tuned to measure high-energy gamma rays at various energy levels. Astronomers aim the satellite at potential gamma ray sources and map the resulting data. Sometimes, the data is filtered to remove low-level gamma radiation and reveal significant emissions. -
Multi-Decadal Surface Temperature Trends in East
MULTI-DECADAL SURFACE TEMPERATURE TRENDS IN EAST ANTARCTICA INFERRED FROM BOREHOLE FIRN TEMPERATURE MEASUREMENTS AND GEOPHYSICAL INVERSE METHODS by Atsuhiro Muto B.Sc., Chiba University, Japan, 2003 M.Sc., Chiba University, Japan, 2005 A thesis submitted to the Faculty of the Graduate School of the University of Colorado in partial fulfillment of the requirement for the degree of Doctor of Philosophy Department of Geography 2010 This thesis entitled: Multi-decadal surface temperature trends in East Antarctica inferred from borehole firn temperature measurements and geophysical inverse methods written by Atsuhiro Muto has been approved for the Department of Geography by _____________________________________ Konrad Steffen _____________________________________ Theodore A. Scambos Date _______________ The final copy of this thesis has been examined by the signatories, and we find that both the content and the form meet acceptable presentation standards of scholarly work in the above mentioned discipline. Muto, Atsuhiro (Ph.D., Geography) Multi-decadal surface temperature trends in East Antarctica inferred from borehole firn temperature measurements and geophysical inverse methods Thesis directed by Professor Konrad Steffen Abstract The climate trend of the Antarctic interior remains unclear relative to the rest of the globe because of a lack of long-term weather records. Recent studies by other authors utilizing sparse available records, satellite data, and models have estimated a significant warming trend in the near-surface air temperature in West Antarctica and weak and poorly constrained warming trend in East Antarctica for the past 50 years. In this dissertation, firn thermal profiling was used to detect multi-decadal surface temperature trends in the interior of East Antarctica where few previous records of any kind exist. -
The Spitzer Space Telescope and the IR Astronomy Imaging Chain
Spitzer Space Telescope (A.K.A. The Space Infrared Telescope Facility) The Infrared Imaging Chain Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 1/38 The infrared imaging chain Generally similar to the optical imaging chain... 1) Source (different from optical astronomy sources) 2) Object (usually the same as the source in astronomy) 3) Collector (Spitzer Space Telescope) 4) Sensor (IR detector) 5) Processing 6) Display 7) Analysis 8) Storage ... but steps 3) and 4) are a bit more difficult! Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 2/38 The infrared imaging chain Longer wavelength – need a bigger telescope to get the same resolution or put up with lower resolution Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 3/38 Emission of IR radiation Warm objects emit lots of thermal infrared as well as reflecting it Including telescopes, people, and the Earth – so collection of IR radiation with a telescope is more complicated than an optical telescope Optical image of Spitzer Space Telescope launch: brighter regions are those which reflect more light IR image of Spitzer launch: brighter regions are those which emit more heat Infrared wavelength depends on temperature of object Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 4/38 Atmospheric absorption The atmosphere blocks most infrared radiation Need a telescope in space to view the IR properly Fundamentals of Astronomical Imaging – Spitzer Space Telescope – 8 May 2006 5/38 -
James Webb Space Telescope
JAMES WEBB SPACE TELESCOPE ® Are we alone? How did we get here? The James GO BEYOND WITH BALL. Webb Space Telescope will play an important role in answering our most fundamental questions. As NASA’s next premier observatory, the Webb telescope will study emissions from objects formed when the universe was just beginning. OVERVIEW QUICK FACTS Serving as the premier observatory of the next • Webb’s primary mirror is comprised of 18 decade, NASA’s Webb telescope will revolutionize our hexagonal mirror segments, each 1.3 meters understanding of the cosmos as it studies every phase of (4.3 feet) in diameter our universe’s history, from the first luminous glows after the Big Bang to the evolution of our own solar system. • Each mirror segment weighs about 20 kg (46 lbs.) As the world’s largest infrared telescope, Webb will offer unprecedented resolution and sensitivity from long- • The primary mirror’s total diameter is 6.5 m wavelength visible light, near-infrared and mid-infrared. It (21 feet 4 in.) will detect objects up to 400 times more faint than can be • The primary mirror’s gold coating is highly observed by current ground- and space-based telescopes. reflective over all the wavelengths the Webb has four scientific goals: telescope will see, from visible to mid- • Search for the first light after the Big Bang infrared • Determine how galaxies evolved • Because Webb is an infrared telescope, • Observe the birth of stars and protoplanetary systems the mirrors and actuators must function at temperatures as low as -400⁰ F (33K) • Investigate the properties of planetary systems and the origins of life • Webb is the largest mirror ever flown in space • Webb is the first mirror to deploy in space. -
Utilisation Des Températures De Surface MODIS Et Du
Using MODIS land surface temperatures and the Crocus snow model to understand the warm bias of ERA- Interim reanalysis at the surface in Antarctica H. Fréville, E. Brun, G. Picard, N. Tatarinova, L. Arnaud, C. Lanconelli, C. Reijmer and M. van den Broeke 7th EARSeL workshop on Land Ice and Snow February 2014 • Introduction • Data and Methods • Evaluation results ▫ LST MODIS evaluation ▫ ERA-Interim and Crocus surface temperature analysis • Conclusions Introduction Use of remote-sensed surface temperature to evaluate the quality of reanalysis and snow model outputs in Antarctica. • Limited use of satellite observations for the evaluation of surface temperature simulations • Ts can be estimated from satellite observations under clear-sky conditions using the thermal emission of the surface in the infrared • Ts is more appropriate than T2m for investigating the energy budget of a snow-covered surface : • Ts : function of the surface energy budget • T2m : diagnosis from the surface temperature and the air temperature at the lowest atmospheric vertical level • Large temperature gradients near the surface Data and method OBSERVATIONS : MODIS surface temperatures Clear-sky satellite observations Hourly data; period : 2000-2011; Resolution ~1km In situ observations 7 stations : Dome C, South Pole, Syowa, Kohnen, Plateau Station B, Pole of Inaccessibility and Princess Elisabeth. MODELS : ERA-Interim surface temperatures ERA-i Ts is derived from the energy balance equation during the forecast step of IFS (Integrated Forecast Model) 3-hourly data; period: 2000-2011; Resolution : 80 km Crocus snow model simulations SURFEX/Crocus ERA-Interim forcing data : T2m, HR2m, U10m, precipitation rate, LWdown, SWdown, Ps, extracted at 0.5° resolution 3H time step. -
The History of Infrared Astronomy: the Minnesota-UCSD-Wyoming Axis
The History of Infrared Astronomy: the Minnesota-UCSD-Wyoming Axis By Robert D. Gehrz Department of Astronomy, School of Physics and Astronomy, 116 Church Street, S. E., University of Minnesota, Minneapolis, MN 55455, [email protected] 1. Ed Ney, Fred Gillett, Wayne Stein, and Nick Woolf A complex set of circumstances converged to propel the University of Minnesota (UM), the University of California at San Diego (UCSD), and the University of Wyoming (UW) into a collaboration that played a leading role in the first four decades of infrared (IR) astronomy. The cornerstone was laid in 1962 when Neville J. ANick@ Woolf was a postdoctoral student at Lick Observatory. Martin Schwartzschild of Princeton University, then the boss of Project Stratoscope II (SS2), attended a conference at Lick and met Nick. Their mutual interest in problems in stellar evolution led Schwarzschild to offer Nick a position at Princeton working on SS2. Carl Sagan had suggested to Schwartzschild that a major objective of the project should be to search for water on Mars. Nick realized that the detection of water emission bands in the infrared could be a key to this search. Bob Danielson, an SS2 collaborator and former student of Ed Ney=s at UM, had recently read Frank J. Low=s paper on the development of the GaGe bolometer (Low 1961) and decided it was the detector of choice. Bob piqued Nick=s interest in this prospect, and Nick became the SS2 IR detector guru. Nick visited Frank Low at Texas Instruments, Inc. to learn about his detector and its operation and brought a technology collaboration back to Princeton for SS2. -
Waba Directory 2003
DIAMOND DX CLUB www.ddxc.net WABA DIRECTORY 2003 1 January 2003 DIAMOND DX CLUB WABA DIRECTORY 2003 ARGENTINA LU-01 Alférez de Navió José María Sobral Base (Army)1 Filchner Ice Shelf 81°04 S 40°31 W AN-016 LU-02 Almirante Brown Station (IAA)2 Coughtrey Peninsula, Paradise Harbour, 64°53 S 62°53 W AN-016 Danco Coast, Graham Land (West), Antarctic Peninsula LU-19 Byers Camp (IAA) Byers Peninsula, Livingston Island, South 62°39 S 61°00 W AN-010 Shetland Islands LU-04 Decepción Detachment (Navy)3 Primero de Mayo Bay, Port Foster, 62°59 S 60°43 W AN-010 Deception Island, South Shetland Islands LU-07 Ellsworth Station4 Filchner Ice Shelf 77°38 S 41°08 W AN-016 LU-06 Esperanza Base (Army)5 Seal Point, Hope Bay, Trinity Peninsula 63°24 S 56°59 W AN-016 (Antarctic Peninsula) LU- Francisco de Gurruchaga Refuge (Navy)6 Harmony Cove, Nelson Island, South 62°18 S 59°13 W AN-010 Shetland Islands LU-10 General Manuel Belgrano Base (Army)7 Filchner Ice Shelf 77°46 S 38°11 W AN-016 LU-08 General Manuel Belgrano II Base (Army)8 Bertrab Nunatak, Vahsel Bay, Luitpold 77°52 S 34°37 W AN-016 Coast, Coats Land LU-09 General Manuel Belgrano III Base (Army)9 Berkner Island, Filchner-Ronne Ice 77°34 S 45°59 W AN-014 Shelves LU-11 General San Martín Base (Army)10 Barry Island in Marguerite Bay, along 68°07 S 67°06 W AN-016 Fallières Coast of Graham Land (West), Antarctic Peninsula LU-21 Groussac Refuge (Navy)11 Petermann Island, off Graham Coast of 65°11 S 64°10 W AN-006 Graham Land (West); Antarctic Peninsula LU-05 Melchior Detachment (Navy)12 Isla Observatorio -
Astronomy 113 Laboratory Manual
UNIVERSITY OF WISCONSIN - MADISON Department of Astronomy Astronomy 113 Laboratory Manual Fall 2011 Professor: Snezana Stanimirovic 4514 Sterling Hall [email protected] TA: Natalie Gosnell 6283B Chamberlin Hall [email protected] 1 2 Contents Introduction 1 Celestial Rhythms: An Introduction to the Sky 2 The Moons of Jupiter 3 Telescopes 4 The Distances to the Stars 5 The Sun 6 Spectral Classification 7 The Universe circa 1900 8 The Expansion of the Universe 3 ASTRONOMY 113 Laboratory Introduction Astronomy 113 is a hands-on tour of the visible universe through computer simulated and experimental exploration. During the 14 lab sessions, we will encounter objects located in our own solar system, stars filling the Milky Way, and objects located much further away in the far reaches of space. Astronomy is an observational science, as opposed to most of the rest of physics, which is experimental in nature. Astronomers cannot create a star in the lab and study it, walk around it, change it, or explode it. Astronomers can only observe the sky as it is, and from their observations deduce models of the universe and its contents. They cannot ever repeat the same experiment twice with exactly the same parameters and conditions. Remember this as the universe is laid out before you in Astronomy 113 – the story always begins with only points of light in the sky. From this perspective, our understanding of the universe is truly one of the greatest intellectual challenges and achievements of mankind. The exploration of the universe is also a lot of fun, an experience that is largely missed sitting in a lecture hall or doing homework.