DOCSLIB.ORG

The ASTRO-H X-Ray Astronomy Satellite

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The ASTRO-H X-Ray Astronomy Satellite The ASTRO-H X-ray Astronomy Satellite Tadayuki Takahashia, Kazuhisa Mitsudaa, Richard Kelleyb, Felix Aharonianc, Hiroki Akamatsud, Fumie Akimotoe, Steve Allenf, Naohisa Anabukig, Lorella Angelinib, Keith Arnaudh, Makoto Asaif, Marc Audardi, Hisamitsu Awakij, Philipp Azzarelloi, Chris Balutaa, Aya Bambak, Nobutaka Bandoa, Marshall Bautzl, Thomas Bialasb, Roger Blandfordf, Kevin Boyceb, Laura Brennemanb, Greg Brownm, Edward Cackettn, Edgar Canavanb, Maria Chernyakovac, Meng Chiaob, Paolo Coppio, Elisa Costantinid, Jelle de Plaad, Jan-Willem den Herderd, Michael DiPirrob, Chris Donep, Tadayasu Dotania, John Dotyq, Ken Ebisawaa, Megan Eckartb, Teruaki Enotor, Yuichiro Ezoes, Andrew Fabiann, Carlo Ferrignoi, Adam Fostert, Ryuichi Fujimotou, Yasushi Fukazawav, Stefan Funkf, Akihiro Furuzawae, Massimiliano Galeazziw, Luigi Gallox, Poshak Gandhip, Kirk Gilmoref, Matteo Guainazziy, Daniel Haasd, Yoshito Habaz, Kenji Hamaguchih, Atsushi Harayamaa, Isamu Hatsukadeaa, Takayuki Hayashia, Katsuhiro Hayashia, Kiyoshi Hayashidag, Junko Hiragaab, Kazuyuki Hirosea, Ann Hornschemeierb, Akio Hoshinoac, John Hughesad, Una Hwangae, Ryo Iizukaa, Yoshiyuki Inouea, Kazunori Ishibashie, Manabu Ishidaa, Kumi Ishikawar, Kosei Ishimuraa, Yoshitaka Ishisakis, Masayuki Itoaf, Naoko Iwataa, Naoko Iyomotoag, Chris Jewellah, Jelle Kaastrad, Timothy Kallmanb, Tuneyoshi Kamaef, Jun Kataokaai, Satoru Katsudaa, Junichiro Katsutav, Madoka Kawaharadaa, Nobuyuki Kawaiaj, Taro Kawanoa, Shigeo Kawasakia, Dmitry Khangulyana, Caroline Kilbourneb, Mark Kimballb, Masashi Kimuraak, Shunji Kitamotoac, Tetsu Kitayamaal, Takayoshi Kohmuraam, Motohide Kokubuna, Saori Konamis, Tatsuro Kosakaan, Alex Koujelevao, Katsuji Koyamaap, Hans Krimmb, Aya Kubotaaq, Hideyo Kuniedae, Stephanie LaMassao, Philippe Laurentar, Fran¸cois Lebrunar, Maurice Leuteneggerb, Olivier Limousinar, Michael Loewensteinb, Knox Longas, David Lumbah, Grzegorz Madejskif, Yoshitomo Maedaa, Kazuo Makishimaab, Maxim Markevitchb, Candace Mastersb, Hironori Matsumotoe, Kyoko Matsushitaat, Dan McCammonau, Daniel Mcguinnessb, Brian McNamaraav, Joseph Mikob, Jon Milleraw, Eric Millerl, Shin Mineshigeax, Kenji Minesugia, Ikuyuki Mitsuishie, Takuya Miyazawae, Tsunefumi Mizunov, Koji Moriaa, Hideyuki Morie, Franco Morosoao, Theodore Muenchb, Koji Mukaib, Hiroshi Murakamiay, Toshio Murakamiu, Richard Mushotzkyh, Housei Naganoe, Ryo Naginog, Takao Nakagawaa, Hiroshi Nakajimag, Takeshi Nakamoriaz, Shinya Nakashimaa, Kazuhiro Nakazawaab, Yoshiharu Nambaba, Chikara Natsukaria, Yusuke Nishiokaaa, Masayoshi Nobukawaap, Hirofumi Nodar, Masaharu Nomachibb, Steve O' Dellbc, Hirokazu Odakaa, Hiroyuki Ogawaa, Mina Ogawaa, Keiji Ogij, Takaya Ohashis, Masanori Ohnov, Masayuki Ohtaa, Takashi Okajimab, Atsushi Okamotoak, Tsuyoshi Okazakia, Naomi Otabd, Masanobu Ozakia, Frits Paerelsbe, St´ephanePaltanii, Arvind Parmary, Robert Petreb, Ciro Pinton, Martin Pohli, b b b bc aw arXiv:1412.1356v1 [astro-ph.IM] 3 Dec 2014 James Pontius , F. Scott Porter , Katja Pottschmidt , Brian Ramsey , Rubens Reis , Christopher Reynoldsh, Claudio Ricciax, Helen Russelln, Samar Safi-Harbbf, Shinya Saitoa, Shin-ichiro Sakaia, Hiroaki Sameshimaa, Goro Satoai, Yoichi Satoak, Kosuke Satoat, Rie Satoa, Makoto Sawadak, Peter Serlemitsosb, Hiromi Setabg, Yasuko Shibanoa, Maki Shidaa, Takanobu Shimadaa, Keisuke Shinozakiak, Peter Shirronb, Aurora Simionescua, Cynthia Simmonsb, Randall Smitht, Gary Sneidermanb, Yang Soongb, Lukasz Stawarza, Yasuharu Sugawarabh, Hiroyuki Sugitaak, Satoshi Sugitaj, Andrew Szymkowiako, Hiroyasu Tajimae, Hiromitsu Takahashiv, Hiroaki Takahashig, Shin-ichiro Takedaa, Yoh Takeia, Toru Tamagawar, Takayuki Tamuraa, Keisuke Tamurae, Takaaki Tanakaap, Yasuo Tanakaa, Yasuyuki Tanakav, Makoto Tashirobg, Yuzuru Tawarae, Yukikatsu Teradabg, Yuichi Terashimaj, Francesco Tombesib, Hiroshi Tomidaak, Yohko Tsuboibh, Masahiro Tsujimotoa, Hiroshi Tsunemig, Takeshi Tsuruap, Hiroyuki Uchidaap, Yasunobu Uchiyamaac, Hideki Uchiyamabi, Yoshihiro Uedaax, Shutaro Uedag, Shiro Uenoak, Shinichiro Unobj, Meg Urryo, Eugenio Ursinow, Cor de Vriesd, Atsushi Wadaa, Shin Watanabea, Tomomi Watanabeb, Norbert Wernerf, Nicholas Whiteb, Dan Wilkinsx, Takahiro Yamadaa, Shinya Yamadas, Hiroya Yamaguchib, Kazutaka Yamaokae, Noriko Yamasakia, Makoto Yamauchiaa, Shigeo Yamauchibd, Tahir Yaqoobb, Yoichi Yatsuaj, Daisuke Yonetokuu, Atsumasa Yoshidak, Takayuki Yuasar, Irina Zhuravlevaf, Abderahmen Zoghbih, John ZuHoneb, aInstitute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan; bNASA/Goddard Space Flight Center, MD 20771, USA; cAstronomy and Astrophysics Section, Dublin Institute for Advanced Studies, Dublin 2, Ireland; dSRON Netherlands Institute for Space Research, Utrecht, The Netherlands; eDepartment of Physics, Nagoya University, Aichi 338-8570, Japan; fKavli Institute for Particle Astrophysics and Cosmology, Stanford University, CA 94305, USA; g Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan; h Department of Astronomy, University of Maryland, MD 20742, USA; iUniversit´ede Gen`eve, Gen`eve 4, Switzerland; jDepartment of Physics, Ehime University, Ehime 790-8577, Japan; kDepartment of Physics and Mathematics, Aoyama Gakuin University, Kanagawa 229-8558, Japan; lKavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, MA 02139, USA; mLawrence Livermore National Laboratory, CA 94550, USA; nInstitute of Astronomy, Cambridge University, CB3 0HA, UK; oYale Center for Astronomy and Astrophysics, Yale University, CT 06520-8121, USA; pDepartment of Physics, University of Durham, DH1 3LE, UK; qNoqsi Aerospace Ltd., CO 80470, USA; rRIKEN, Saitama 351-0198, Japan; sDepartment of Physics, Tokyo Metropolitan University, Tokyo 192-0397, Japan; tHarvard-Smithsonian Center for Astrophysics, MA 02138, USA; uFaculty of Mathematics and Physics, Kanazawa University, Ishikawa 920-1192, Japan; vDepartment of Physical Science, Hiroshima University, Hiroshima 739-8526, Japan; wPhysics Department, University of Miami, FL 33124, USA; xDepartment of Astronomy and Physics, Saint Mary's University, Nova Scotia B3H 3C3, Canada; yEuropean Space Agency (ESA), European Space Astronomy Centre (ESAC), Madrid, Spain; zDepartment of Physics and Astronomy, Aichi University of Education, Aichi 448-8543, Japan; aaDepartment of Applied Physics, University of Miyazaki, Miyazaki 889-2192, Japan; abDepartment of Physics, University of Tokyo, Tokyo 113-0033, Japan; acDepartment of Physics, Rikkyo University, Tokyo 171-8501, Japan; ad Department of Physics and Astronomy, Rutgers University, NJ 08854-8019, USA; ae Department of Physics and Astronomy, Johns Hopkins University, MD 21218, USA; af Faculty of Human Development, Kobe University, Hyogo 657-8501, Japan; agKyushu University, Fukuoka 819-0395, Japan; ahEuropean Space Agency (ESA), European Space Research and Technology Centre (ESTEC), 2200 AG Noordwijk, The Netherlands; ai Research Institute for Science and Engineering, Waseda University, Tokyo 169-8555, Japan; ajDepartment of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan; ak Tsukuba Space Center (TKSC), Japan Aerospace Exploration Agency (JAXA), Ibaraki 305-8505, Japan; alDepartment of Physics, Toho University, Chiba 274-8510, Japan; am Department of Physics, Tokyo University of Science, Chiba 278-8510, Japan; anSchool of Systems Engineering, Kochi University of Technology, Kochi 782-8502, Japan; aoSpace Exploration Development Space Exploration, Canadian Space Agency John H. Chapman Space Centre, QC J3Y 8Y9, Canada; apDepartment of Physics, Kyoto University, Kyoto 606-8502, Japan; aqDepartment of Electronic Information Systems, Shibaura Institute of Technology, Saitama 337-8570, Japan; arIRFU/Service d'Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France; asSpace Telescope Science Institute, MD 21218, USA; atDepartment of Physics, Tokyo University of Science, Tokyo 162-8601, Japan; au Department of Physics, University of Wisconsin, WI 53706, USA; avUniversity of Waterloo, Ontario N2L 3G1, Canada; awDepartment of Astronomy, University of Michigan, MI 48109, USA; axDepartment of Astronomy, Kyoto University, Kyoto 606-8502, Japan; ay Department of Information Science, Faculty of Liberal Arts, Tohoku Gakuin University, Miyagi 981-3193, Japan; azDepartment of Physics, Faculty of Science, Yamagata University, Yamagata 990-8560, Japan; baDepartment of Mechanical Engineering, Chubu University, Aichi 487-8501, Japan; bbLaboratory of Nuclear Studies, Osaka University, Osaka 560-0043, Japan; bcNASA/Marshall Space Flight Center, AL 35812, USA; bd Department of Physics, Faculty of Science, Nara Women's University, Nara 630-8506, Japan; beDepartment of Astronomy, Columbia University, NY 10027, USA; bfDepartment of Physics and Astronomy, University of Manitoba, MB R3T 2N2, Canada; bgDepartment of Physics, Saitama University, Saitama 338-8570, Japan; bhDepartment of Physics, Chuo University, Tokyo 112-8551, Japan; biScience Education, Faculty of Education, Shizuoka University, Shizuoka 422-8529, Japan; bjFaculty of Social and Information Sciences, Nihon Fukushi University, Aichi 475-0012, Japan; ABSTRACT The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions de- veloped by the Institute of Space and Astronautical Science (ISAS), with a planned launch in 2015. The ASTRO-H mission is equipped with a suite of sensitive instruments with the highest energy resolution ever achieved at E > 3 keV and a wide energy range spanning four
Load more

Recommended publications
  • II Publications, Presentations
    II Publications, Presentations 1. Refereed Publications Izumi, K., Kotake, K., Nakamura, K., Nishida, E., Obuchi, Y., Ohishi, N., Okada, N., Suzuki, R., Takahashi, R., Torii, Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Y., Ueda, A., Yamazaki, T.: 2010, DECIGO and DECIGO Search for Gravitational-wave Inspiral Signals Associated with pathfinder, Class. Quantum Grav., 27, 084010. Short Gamma-ray Bursts During LIGO's Fifth and Virgo's First Aoki, K.: 2010, Broad Balmer-Line Absorption in SDSS Science Run, ApJ, 715, 1453-1461. J172341.10+555340.5, PASJ, 62, 1333. Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, All- Aoki, K., Oyabu, S., Dunn, J. P., Arav, N., Edmonds, D., Korista sky search for gravitational-wave bursts in the first joint LIGO- K. T., Matsuhara, H., Toba, Y.: 2011, Outflow in Overlooked GEO-Virgo run, Phys. Rev. D, 81, 102001. Luminous Quasar: Subaru Observations of AKARI J1757+5907, Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, PASJ, 63, S457. Search for gravitational waves from compact binary coalescence Aoki, W., Beers, T. C., Honda, S., Carollo, D.: 2010, Extreme in LIGO and Virgo data from S5 and VSR1, Phys. Rev. D, 82, Enhancements of r-process Elements in the Cool Metal-poor 102001. Main-sequence Star SDSS J2357-0052, ApJ, 723, L201-L206. Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Arai, A., et al. including Yamashita, T., Okita, K., Yanagisawa, TOPICAL REVIEW: Predictions for the rates of compact K.: 2010, Optical and Near-Infrared Photometry of Nova V2362 binary coalescences observable by ground-based gravitational- Cyg: Rebrightening Event and Dust Formation, PASJ, 62, wave detectors, Class.
    [Show full text]
  • Wide-Field Infrared Survey Explorer Launch Press
    PRess KIT/DECEMBER 2009 Wide-field Infrared Survey Explorer Launch Contents Media Services Information ................................................................................................................. 3 Quick Facts ............................................................................................................................................. 4 Mission Overview .................................................................................................................................. 5 Why Infrared? ....................................................................................................................................... 10 Science Goals and Objectives ......................................................................................................... 12 Spacecraft ............................................................................................................................................. 16 Science Instrument ............................................................................................................................. 19 Infrared Missions: Past and Present ............................................................................................... 23 NASA’s Explorer Program ................................................................................................................. 25 Program/Project Management .......................................................................................................... 27 Media Contacts J.D. Harrington
    [Show full text]
  • Building the Coolest X-Ray Satellite
    National Aeronautics and Space Administration Building the Coolest X-ray Satellite 朱雀 Suzaku A Video Guide for Teachers Grades 9-12 Probing the Structure & Evolution of the Cosmos http://suzaku-epo.gsfc.nasa.gov/ www.nasa.gov The Suzaku Learning Center Presents “Building the Coolest X-ray Satellite” Video Guide for Teachers Written by Dr. James Lochner USRA & NASA/GSFC Greenbelt, MD Ms. Sara Mitchell Mr. Patrick Keeney SP Systems & NASA/GSFC Coudersport High School Greenbelt, MD Coudersport, PA This booklet is designed to be used with the “Building the Coolest X-ray Satellite” DVD, available from the Suzaku Learning Center. http://suzaku-epo.gsfc.nasa.gov/ Table of Contents I. Introduction 1. What is Astro-E2 (Suzaku)?....................................................................................... 2 2. “Building the Coolest X-ray Satellite” ....................................................................... 2 3. How to Use This Guide.............................................................................................. 2 4. Contents of the DVD ................................................................................................. 3 5. Post-Launch Information ........................................................................................... 3 6. Pre-requisites............................................................................................................. 4 7. Standards Met by Video and Activities ...................................................................... 4 II. Video Chapter 1
    [Show full text]
  • AKARI: Astronomical IR Satellite MLHES Mission Program
    Probing Ancient Mass Loss with AKARI’s Extended Dust Emission Objects Rachael Tomasino1, Dr. Toshiya Ueta1,2, Dr. Yamamura Issei2, Dr. Hideyuki Izumiura3 1University of Denver, USA; 2Institute of Space and Astronomical Science, Japan Aerospace Exploration Agency (ISAS/JAXA), Japan, 3Okayama Astrophysical Observatory, Japan AKARI: Astronomical IR Satellite FIS-AKARI Slow-scan Tools! Extended Emission Calibration! AKARI (formerly ASTRO-F), is the second Japanese satellite FAST is a program that allows for interactive Original calibration of the FIS detector was done using diffuse galactic cirrus emission dedicated to infrared (IR) astronomy, from the Institute of assessment of the data quality and on-the-fly with low photon counts. On the other hand, bright point sources can cause the slow Space and Astronautical Science (ISAS) of the Japanese corrections to the time-series data on a pixel-by- transient response effect because of high photon counts. Marginally extended sources Aerospace Exploration Agency (JAXA). Its main objective is pixel basis in order to manually correct glitches consist of regions of high and low photon counts, and therefore, only parts of them suffer to perform an all-sky survey with better spatial resolution and that would have been missed in the pipeline from the slow transient response effect. Hence, we needed to devise a specific method to wider wavelength coverage than IRAS (first US, UK, Dutch process. These corrections include: (1) eliminate address the detector response as a whole. This method uses a contour aperture to include infrared satellite launched in 1983), mapping the entire sky in bad on-sky calibration sequences, (2) flag out both the faint and bright emission by setting a threshold of background + 3#.! six infrared bands.
    [Show full text]
  • ASTRO-F Observer's Manual
    ASTRO-F Observer’s Manual Version 3.2 — for Open Time Observation Planning — ASTRO-F User Support Team in Institute of Space and Astronautical Science / JAXA contact: iris [email protected] European Space Astronomy Centre / ESA contact: http://astro-f.esac.esa.int/esupport/ November 29, 2005 Version 3.2 (November 29, 2005) i Revision Record 2005 Nov. 29: Version 3.2 released. Updated description of IRC FoV and slit (Section 5.1.4 and 5.1.5). Updated IRC04 detection and saturation limits. Also improve the description (Section 5.5.9). Section 5.4.2 revised to clarify the point. Units for Ho given value in p.113. 2005 Nov. 8: Version 3.1 released. Updated Visibility Map for Open Time Users (Figure 3.4.3) Information for the handling of Solar System Object observations (Section 3.4) Updated saturation limits for FTS (FIS03) mode (Table 4.4.16) IRC04 detection limits for NG+Np added (Table 5.5.25,5.5.26) Updated worked examples using the latest versions of the Tools (Section B) ESAC web pages URL and Helpdesk contact address updated Numerous errors and typos corrected 2005 Sep.20: Version 3.0 released. Contents 1 Introduction 1 1.1Purposeofthisdocument............................... 1 1.2RelevantInformation.................................. 3 2 Mission Overview 5 2.1TheASTRO-FMission................................ 5 2.2 Satellite . ........................................ 6 2.2.1 TheBusModule................................ 6 2.2.2 AttitudeDeterminationandControlSystem................. 7 2.2.3 Cryogenics................................... 8 2.3Telescope........................................ 9 2.3.1 Specification.................................. 9 2.3.2 Pre-flightperformance............................. 10 2.4Focal-PlaneInstruments................................ 11 2.4.1 SpecificationOverview............................. 11 2.4.2 Focal-PlaneLayout..............................
    [Show full text]
  • The AKARI FU-HYU Galaxy Evolution Program: First Results from The
    A&A 514, A9 (2010) Astronomy DOI: 10.1051/0004-6361/200913383 & c ESO 2010 Astrophysics Science with AKARI Special feature The AKARI FU-HYU galaxy evolution program: first results from the GOODS-N field C. P. Pearson1,2,3, S. Serjeant3, M. Negrello3,T.Takagi4, W.-S. Jeong5, H. Matsuhara4,T.Wada4,S.Oyabu4, H. M. Lee6,andM.S.Im6 1 Space Science and Technology Department, CCLRC Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK e-mail: [email protected] 2 Department of Physics, University of Lethbridge, 4401 University Drive, Lethbridge, Alberta T1J 1B1, Canada 3 Astrophysics Group, Department of Physics, The Open University, Milton Keynes MK7 6AA, UK 4 Institute of Space and Astronautical Science, Yoshinodai 3-1-1, Sagamihara, Kanagawa 229 8510, Japan 5 KASI, 61-1, Whaam-dong, Yuseong-gu, Deajeon 305-348, South Korea 6 Department of Physics and Astronomy, Seoul National University, Shillim-Dong, Kwanak-Gu, Seoul 151-742, Korea Received 30 September 2009 / Accepted 9 February 2010 ABSTRACT The AKARI FU-HYU mission program carried out mid-infrared imaging of several well studied Spitzer fields preferentially selecting fields already rich in multi-wavelength data from radio to X-ray wavelengths filling in the wavelength desert between the Spitzer IRAC and MIPS bands. We present the initial results for the FU-HYU survey in the GOODS-N field. We utilize the supreme multiwavelength coverage in the GOODS-N field to produce a multiwavelength catalogue from infrared to ultraviolet wavelengths, containing more than 4393 sources, including photometric redshifts. Using the FU-HYU catalogue we present colour-colour diagrams that map the passage of PAH features through our observation bands.
    [Show full text]
  • Special Spitzer Telescope Edition No
    INFRARED SCIENCE INTEREST GROUP Special Spitzer Telescope Edition No. 4 | August 2020 Contents From the IR SIG Leadership Council In the time since our last newsletter in January, the world has changed. 1 From the SIG Leadership Travel restrictions and quarantine have necessitated online-conferences, web-based meetings, and working from home. Upturned semesters, constantly shifting deadlines and schedules, and the evolving challenge of Science Highlights keeping our families and communities safe have all taken their toll. We hope this newsletter offers a moment of respite and a reminder that our community 2 Mysteries of Exoplanet continues its work even in the face of great uncertainty and upheaval. Atmospheres In January we said goodbye to the Spitzer Space Telescope, which 4 Relevance of Spitzer in the completed its mission after sixteen years in space. In celebration of Spitzer, Era of Roman, Euclid, and in recognition of the work of so many members of our community, this Rubin & SPHEREx newsletter edition specifically highlights cutting edge science based on and inspired by Spitzer. In the words of Dr. Paul Hertz, Director of Astrophysics 6 Spitzer: The Star-Formation at NASA: Legacy Lives On "Spitzer taught us how important infrared light is to our 8 AKARI Spitzer Survey understanding of our universe, both in our own cosmic 10 Science Impact of SOFIA- neighborhood and as far away as the most distant galaxies. HIRMES Termination The advances we make across many areas in astrophysics in the future will be because of Spitzer's extraordinary legacy." Technical Highlights Though Spitzer is gone, our community remains optimistic and looks forward to the advances that the next generation of IR telescopes will bring.
    [Show full text]
  • JAXA's X-Ray Astronomy Mission ASTRO-H: Launch and First
    46th International Conference on Environmental Systems ICES-2016-157 10-14 July 2016, Vienna, Austria JAXA’s X-ray Astronomy Mission ASTRO-H: Launch and First Month’s In-Orbit Thermal Performance Naoko IWATA1 Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, 252-5210 Tel: +81-50-3362-3592, Fax: +81-42-759-8068 E-mail: [email protected] Takashi USUI2, Akihiko MIKI3, Mizuho IKEDA4 NEC Corporation and Yoh TAKEI5, Atsushi OKAMOTO6, Hiroyuki OGAWA7, Tadayuki TAKAHASHI8 Japan Aerospace Exploration Agency In this study, the thermal performance evaluation results of JAXA’s X-ray astronomy mission ASTRO-H are presented. ASTRO-H was successfully launched on February 17, 2016 from Tanegashima Space Center using an H2A rocket. ASTRO-H houses four telescopes and six detectors. Each detector has its own radiator and heat pipes for heat dissipation. The most major mission will feature a soft X-ray spectrometer having four loop heat pipes (LHPs) for heat transport from two cryocoolers. Six fans have been mounted close to each cryocooler for ground cooling in the fairing just before the launch. Hard X-ray imagers (HXIs) are mounted on an HXI plate; this plate is expanded by 6.4 m via an extensible optical bench (EOB) in orbit to achieve the necessary focal length. The EOB was successfully expanded 11 days after the launch. Heat pipes appropriately functioned in orbit. The two LHPs for the compressors have been operated properly for more than one month Measured inflight temperatures agree well with predicted ones for an attitude condition. Nomenclature
    [Show full text]
  • IAU Commission 8 Astrometry Transactions Report 2012-2015
    Transactions IAU, Volume XXIXA Proc. XXVIII IAU General Assembly, August 2012 c 2015 International Astronomical Union Thierry Montmerle, ed. DOI: 00.0000/X000000000000000X DIVISION I COMMISSION 8 ASTROMETRY (ASTROMETRY) PRESIDENT Norbert Zacharias VICE-PRESIDENT Anthony Brown PAST PRESIDENT Dafydd Evans ORGANIZING COMMITTEE Li Chen, Naoteru Gouda, Valeri Makarov, Aleksandr Shulga, Jean Souchay, Rama Teixeira, Stephen Unwin 1. Introduction Commission 8 has regularly published triennial reports in the past and the current OC therefore voted to adopt a traditional format also for this special Legacy issue of the IAU Transactions. The outgoing President is grateful for the support of many Commission members who contributed to this report. Our contribution consists of 3 parts: 1) this introduction, providing a general overview and highlights of recent research in astrometry, 2) a summary of the astrometry business & science meeting at the 2015 IAU General Assembly, and 3) the activity report of our Commisson covering the mid-2012 to mid-2015 period. Astrometry is about to be revolutionized by the European Space Agency (ESA) Gaia mission. Regular survey operations began mid-2014. The first data release is expected by mid-2016 and the final catalog by about 2020, depending on the lifetime of the mission, currently expected to be over 5 years. Gaia will provide an optical reference frame with positions, proper motions and parallaxes in the 10 to 300 micro-arcsecond (µas) range (depending on brightness) down to almost 21st magnitude, which will soon make most current optical reference star catalogs obsolete. Radio astrometry continues to provide the defining celestial reference frame by VLBI observations of compact, extragalactic sources.
    [Show full text]
  • Science Vision Draft
    A Science Vision for European Astronomy ASTRONET SVWG DRAFT December 19, 2006 ii Contents 1 Introduction 1 1.1 The role of science in society . ............................. 1 1.2 Astronomy . ........................................ 3 1.3 Predicting the future .................................... 5 1.4 This document ........................................ 6 2 Do we understand the extremes of the Universe? 7 2.1 How did the Universe begin? . ............................. 8 2.1.1 Background . .................................... 8 2.1.2 Key observables . ............................. 9 2.1.3 Future experiments . ............................. 9 2.2 What is dark matter and dark energy? . ......................... 10 2.2.1 Current status .................................... 10 2.2.2 Experimental signatures . ............................. 11 2.2.3 Future strategy . ............................. 12 2.3 Can we observe strong gravity in action? . ..................... 13 2.3.1 Background . .................................... 13 2.3.2 Experiments . .................................... 15 2.4 How do supernovae and gamma-ray bursts work? . ................. 17 2.4.1 Current status .................................... 17 2.4.2 Key questions .................................... 18 2.4.3 Future experiments . ............................. 19 2.5 How do black hole accretion, jets and outflows operate? . .......... 20 2.5.1 Background . .................................... 20 2.5.2 Experiments . .................................... 21 2.6 What do we learn
    [Show full text]
  • NEC Space Business
    Japan Space industry Workshop in ILA Berlin Airshow 2014 NEC Space Business May 22nd, 2014 NEC Corporation Kentaro (Kent) Sakagami (Mr.) General Manager Satellite Systems and Equipment, Global Business Unit E-mail: [email protected] NEC Corporate Profile Company Name: NEC Corporation Established: July 17, 1899 Kaoru Yano Nobuhiro Endo Chairman of the Board: Kaoru Yano President: Nobuhiro Endo Capital: ¥ 397.2 billion (As of Mar. 31, 2013) Consolidated Net Sales: ¥ 3,071.6 billion (FY ended Mar. 31, 2013) Employees: 102,375 (As of Mar. 31, 2013) Consolidated Subsidiaries: 270 (As of Mar. 31, 2013) Financial results are based on accounting principles generally accepted in Japan Page 2 © NEC Corporation 2014 NEC Worldwide: “One NEC” formation in 5 regions Marketing & Service affiliates 77 in 32 countries Manufacturing affiliates 8 in 5 countries Liaison Offices 7 in 7 countries Branch Offices 7 in 7 countries Laboratories 4 in 3 countries North America Greater China NECJ EMEA APAC Latin America (As of Apr. 1, 2014) Page 3 © NEC Corporation 2014 NEC in EMEA 1 NEC in Germany NEC Deutschland GmbH NEC Display Solutions Europe NEC Laboratories Europe (Internal division of NEC Europe Ltd.) NEC Tokin Europe NEC Scandinavia AB in Espoo, 2 NEC in Netherlands Finland NEC Logistics Europe NEC Nederland B.V. NEC Neva Communications Systems NEC Scandinavia AB in Oslo, Norway NEC in the U.K. 3 NEC Scandinavia AB NEC Europe Ltd. NEC Capital (UK) plc NEC in the UK NEC Technologies (UK) NEC in Netherlands NEC Telecom MODUS Limited 3 2 NEC (UK) Ltd.
    [Show full text]
  • Possibilities and Future Vision of Micro/Nano/Pico-Satellites - from Japanese Experiences
    CanSat & Rocket Experiment(‘99～） Hodoyoshiハイブリッド-1 ‘14 ロケット Possibilities and Future Vision of Micro/nano/pico-satellites - From Japanese Experiences Shinichi Nakasuka University of Tokyo PRISM ‘09 CubeSat 03,05 Nano-JASMINE ‘15 Contents • Features of Micro/nano/pico-satellites • Japanese History and Lessons Learned – CanSat to CubeSat “First CubeSat on orbit” – From education to practical applications – Important tips for development • Visions on Various Applications of Micro/nano/pico-satellites • University Space Engineering Consortium (UNISEC) and International Collaborations Micro/nano/pico-satellite “Lean Satellite” Micro-satellite: 20-100kg Nano-satellite: 2-20kg Pico-satellite: 0.5-2kg Japanese Governmental Satellites ALOS-1: 4 ton ASNARO: 500 kg Kaguya: 3 ton Hayabusa: 510 kg Motivation of Smaller Satellites Current Problem of Mid-large Satellites ALOS 4.0 (4t) Trend towards 3.5 larger satellites Weight SELENE ・Enormous cost >100M$ 3.0 (3t) ・Development period >5-10 years 2.5 ・Conservative design （ton 2.0 ・Almost governmental use ・No new users and utilization ideas ） ・Low speed of innovation 1.5 10-50M$ Micro 1.0 Small-sat /Nano /Pico 0.5 Sat 0 1975 1980 1985 1990 1995 2000 2005 <50kg Introduce more variedGEO new players intoOTHERS space. 1-5M$ Innovation by Micro/nano/pico satellites (<100kg) 超小型衛星革命 Education Remote sensing Telescope Weather Bio-engineering Re-entry Rendezvous/ Communication Space Science Atmosphere Exploration High Resolution. docking Universty/venture companies’ innovative idea and development process <10M$
    [Show full text]