Presentation from Mission PI Takao Nakagawa
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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. -
Cryogenics in Space
— 37 — Cryogenics in space Nicola RandoI Abstract Cryogenics plays a key role on board space-science missions, with a range of applications, mainly in the domain of astrophysics. Indeed a tremendous progress has been achieved over the last 20 years in cryogenics, with enhanced reliability and simpler operations, thus matching the needs of advanced focal-plane detectors and complex science instrumentation. In this article we provide an overview of recent applications of cryogenics in space, with specific emphasis on science missions. The overview includes an analysis of the impact of cryogenics on the spacecraft system design and of the main technical solutions presently adopted. Critical technology developments and programmatic aspects are also addressed, including specific needs of future science missions and lessons learnt from recent programmes. Introduction H. Kamerlingh-Onnes liquefied 4He for the first time in 1908 and discovered superconductivity in 1911. About 100 years after such achievements (Pobell 1996), cryogenics plays a key role on board space-science missions, providing the environ- ment required to perform highly sensitive measurements by suppressing the thermal background radiation and allowing advantage to be taken of the performance of cryogenic detectors. In the last 20 years several spacecraft have been equipped with cryogenic in- strumentation. Among such missions we should mention IRAS (launched in 1983), ESA’s ISO (launched in 1995) (Kessler et al 1996) and, more recently, NASA’s Spitzer (formerly SIRTF, launched in 2006) (Werner 2005) and the Japanese mis- sion Akari (IR astronomy mission launched in 2006) (Shibai 2007). New missions involving cryogenics are the ESA missions Planck (dedicated to the mapping of the cosmic background radiation) and Herschel (far infrared and sub-millimetre observatory), carrying instruments operating at temperatures of 0.1 K and 0.3 K, respectively (Crone et al 2006). -
NASA HQ Update on IXO
NASA HQ Update on IXO IXO Facility Science Team Meeting GSFC, 20 August 2008 Michael Salamon Astrophysics Division, NASA HQ Recent History of IXO • Stern and Southwood at NASA/ESA bilateral informally agree that Con-X and XEUS must find a path forward to a single, merged mission (Paris, Sept 2007). • Southwood letter to Stern (Jan 2008) invites NASA to participate in XEUS study as a starting point leading to possible interagency partnership. • Morse/Favata letter (May 2008): • Con-X is highest priority large-class mission following JWST (2000 Decadal), to be revisited in 2010 Decadal. • XEUS selected as one of three CV L-class competing missions (Outer Planets, XEUS, LISA) with downselection in 2009 and 2011. • Limited resources in both agencies and considerable overlap in science goals argue for finding a joint mission approach. • Agreement for a joint mission study (not the mission itself). • Formation of coordination group (CG) composed of ESA, NASA, and JAXA representatives. • First task of CG is to determine the existence of possible joint mission scenarios. • Once found, study the joint mission scenario to the level required by the selection process milestones of the agencies involved. • No consideration to be given by the CG of which agency might lead the merged mission. IXO Coordination Group • IXO-CG initially charged to find a joint mission scenario for further joint study by the agencies (ESA, NASA, JAXA). • IXO-CG now charged with definition of science requirements for the IXO concept, scientific supervision of study activities, reporting to Agencies. • IXO-CG jointly chaired by the ESA and NASA study scientists. -
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. -
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.............................. -
Messenger-No117.Pdf
ESO WELCOMES FINLANDINLAND AS ELEVENTH MEMBER STAATE CATHERINE CESARSKY, ESO DIRECTOR GENERAL n early July, Finland joined ESO as Education and Science, and exchanged which started in June 2002, and were con- the eleventh member state, following preliminary information. I was then invit- ducted satisfactorily through 2003, mak- II the completion of the formal acces- ed to Helsinki and, with Massimo ing possible a visit to Garching on 9 sion procedure. Before this event, howev- Tarenghi, we presented ESO and its scien- February 2004 by the Finnish Minister of er, Finland and ESO had been in contact tific and technological programmes and Education and Science, Ms. Tuula for a long time. Under an agreement with had a meeting with Finnish authorities, Haatainen, to sign the membership agree- Sweden, Finnish astronomers had for setting up the process towards formal ment together with myself. quite a while enjoyed access to the SEST membership. In March 2000, an interna- Before that, in early November 2003, at La Silla. Finland had also been a very tional evaluation panel, established by the ESO participated in the Helsinki Space active participant in ESO’s educational Academy of Finland, recommended Exhibition at the Kaapelitehdas Cultural activities since they began in 1993. It Finland to join ESO “anticipating further Centre with approx. 24,000 visitors. became clear, that science and technology, increase in the world-standing of ESO warmly welcomes the new mem- as well as education, were priority areas Astronomy in Finland”. In February 2002, ber country and its scientific community for the Finnish government. we were invited to hold an information that is renowned for its expertise in many Meanwhile, the optical astronomers in seminar on ESO in Helsinki as a prelude frontline areas. -
The XEUS Mission
1 THE XEUS MISSION Johan Bleeker1 and Mariano M´endez1 SRON, National Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands Abstract 1. Introduction XEUS, the X-ray Evolving Universe Spectroscopy mis- At the end of the 20th century, the promise of high spa- sion, constitutes at present an ESA-ISAS initiative for the tial and spectral resolution in X-rays has become a reality. study of the evolution of the hot Universe in the post- The two major X-ray observatories nowadays operational, Chandra/XMM-Newton era. The key science objectives NASA’s Chandra and ESA’s XMM Newton, are provid- of XEUS can be formulated as the: ing a new, clear-focused, vision of the X-ray Universe, in a – Search for the origin, and subsequent study of growth, way that had not been possible in the first 40 years of X- of the first massive black holes in the early Universe. ray astronomy. These two missions complement each other – Assessment of the formation of the first gravitationally very well: Chandra has a ∼<0.5 arcsec angular resolution bound dark matter dominated systems, i.e. small groups and the capability of high spectral resolution on a variety of galaxies, and their evolution. of point sources with the High- and Low-Energy Trans- – Study of the evolution of metal synthesis up till the mission Grating Spectrometers, while XMM-Newton has present epoch. Characterization of the true intergalactic a larger spectroscopic area and bandwidth (up to ∼15 medium. keV), and the capability of high-resolution spectroscopic To reach these ambitious science goals the two salient observations on spatially extended sources. -
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. -
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. -
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. -
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. -
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$