DOCSLIB.ORG

World Space Observatory %Uf02d Ultraviolet Remains Very Relevant

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
World Space Observatory %Uf02d Ultraviolet Remains Very Relevant WORLD SPACE OBSERVATORY-ULTRAVIOLET Boris Shustov, Ana Inés Gómez de Castro, Mikhail Sachkov UV observatories aperture pointing mode , Å OAO-2 1968.12 - 1973.01 20 sp is 1000-4250 TD-1A 1972.03 - 1974.05 28 s is 1350-2800+ OAO-3 1972.08 - 1981.02 80 p s 900-3150 ANS 1974.08 - 1977.06 22 p s 1500-3300+ IUE 1978.01 - 1996.09 45 p s 1150-3200 ASTRON 1983.03 - 1989.06 80 p s 1100-3500+ EXOSAT 1983.05 - 1986. 2x30 p is 250+ ROSAT 1990.06 - 1999.02 84 sp i 60- 200+ HST 1990.04 - 240 p isp 1150-10000 EUVE 1992.06 - 2001.01 12 sp is 70- 760 ALEXIS 1993.04 - 2005.04 35 s i 130- 186 MSX 1996.04 - 2003 50 s i 1100-9000+ FUSE 1999.06 - 2007.07 39х35 (4) p s 905-1195 XMM 1999.12 - 30 p is 1700-5500 GALEX 2003.04 - 2013.06 50 sp is 1350-2800 SWIFT 2004.11 - 30 p i 1700-6500 2 ASTROSAT/UVIT UVIT - UltraViolet Imaging Telescopes (on the ISRO Astrosat observatory, launch 2015); Two 40cm telescopes: FUV and NUV, FOV 0.5 degrees, resolution ~1” Next talk by John Hutchings! 3 4 ASTRON (1983 – 1989) ASTRON is an UV space observatory with 80 cm aperture telescope equipped with a scanning spectrometer:(λλ 110-350 nm, λ ~ 2 nm) onboard. Some significant results: detection of OH (H2O) in Halley comet, UV spectroscopy of SN1987a, Pb lines in stellar spectra etc. (Photo of flight model at Lavochkin Museum).5 “Spektr” (Спектр) missions Federal Space Program (2016-2025) includes as major astrophysical projects: Spektr-R (Radioastron) – launched in 2011. Spektr-RG – scheduled for launch in 2018. Spektr-UF International name is World Space Observatory - UltraViolet (WSO-UV). Launch is scheduled for 2023. 6 WSO-UV Project WSO-UV is an international space observatory for observation in UV spectral range (115 - 350 nm). The WSO-UV includes the telescope with primary mirror of 170 cm and scientific instruments – imaging A.Boyarchuk field cameras and 3 W.Wamsteker spectrographs (resolving power ranges from 1000 to 55000). WSO-UV is still the only 2-m class UV telescope planned to be work in space during the decade after 2024. 7 WSO-UV mission partners Telescope: T-170M, 1.7 m , f/10 Russia Spectrographs: WUVS, Russia Imagers: Russia, Spain Platform: “Navigator”, Russia Orbit: geosynchronous, i=40o Launcher, launch: “Proton”, Russia Ground Segment: Russia and Spain 8 Cooperation in Russia Lavochkin Association Primary contractor for the Project: + subcontractors The T-170M Telescope, Platform, Launch, Mission control center Institute of Astronomy, RAS Primary subcontractor: (INASAN) Science Instrumentation Ground Segment (SOC) Lytkarino Optical Plant Manufacturing optics of the T-170M Physical Inst., RAS UV-spectrographs (detectors, State Optical Institute optical elements, AIV) INASAN UV-spectrographs (mechanics) “Luch” Co. Coatings of optical elements Space Research Inst., On-board Sci. Instr. Control and Data RAS (IKI) Management System, INASAN INASAN major subcontractors Fine Guidance System 9 WSO-UV S/C Field Camera Unit (FCU) 10 The “Navigator” platform Life time, yrs > 5 Spacecraft mass (wet), kg 2900 WSO-UV Payload mass, kg 1600 The power consumption 1 of P/L, KW Data transmission rate, Mbit/s 4 Stabilization and pointing 0.1 accuracy (3), arcsec The platform was successfully in-flight tested during: 1. «Electro» (remote sensing mission) 2. «Spektr-R» 11 The T-170M Telescope Optical system Ritchey – Chrètien aplanat Aperture diameter 1700 mm Telescope f-number 10.0 Field angular diameter 0.50 (300mm diameter) Wavelengths range 100 – 350 nm (+visible) Primary wavelength 200 nm Mass (payload) 1570 kg Optical quality Diffraction optics at the center of FOV 12 Structure of the T-170M Telescope 13 Optical scheme of the T-170M telescope 14 Primary mirror of the T-170M telescope Astrositall СО-115М. Mirror diameter – 1715 mm Central hole – 530 mm, Thickness at center – 110 mm edge – 25 mm Mass (glass) – 360 kg PM is being manufactured at Lytkarino Optical Plant. 15 Secondary mirror unit of the T-170M Mirror diameter – 415 mm Mass (glass) – 12,9 kg Рис. 13. Модуль вторичного зеркала. 16 Mechanical tests of the T-170M All the mechanical and thermo-vacuum tests have been passed successfully. 17 Life is not easy: example of glue DP-190 The DP-190 glue is known as the best one for attachment of astrositall (zerodur) lightweight large- size space astronomical mirrors (2 m class) with elements of their frames of invar. Problem is to properly distribute the glue. 18 Coatings of T-170M mirrors Al+MgF2 coating deposition onto primary mirror in “Luch” Company (in Denton vacuum camera). Optical quality fits requirements. T-170M mirror 19 Micro-roughness 1 mm Micro-roughness of mirror surfaces fits requirements, but… rms < 0.75 nm 20 Control of scattered light . 21 22 23 φs 0.53nm To be improved up to 0.3 nm θs Standard (Black glass T-170M PM with GL10000) Al+MgF2 24 Control of contamination of optical surfaces We control contamination till launch using mirror samples (eyewitnesses). For reflectance measurements we use spectrophotometer VUVaS-1000 (McPherson Co, USA) at 115-350nm. Thanks to “red team”. 25 Telescope AIV facilities Lavochkin Sci-Tech Association 26 T170M service systems (EQMs, FMs) БУП 27 WUVS (WSO-UV Spectrograph) Three channels (spectrographs) of the WUVS (equipped with e2V CCDs): Vacuum Ultraviolet Echele Spectrograph VUVES - 115-176 nm, R 50 000 Ultraviolet Echele Spectrograph UVES - 174-310 nm, R 50 000 Long Slit Spectrograph LSS - 115-310 nm, R=1000 28 28 WUVS parameters UVES VUVES LSS Wavelength range [nm] 174-310 102-176 102-300 Spectral resolution > 50000 > 50000 >1000 (@150nm) Entrance slit dimension 80 80 82 x 6000 [µm] Detector pixel pitch [µm] 30 30 20 SNR (after 10 h) 10 10 10 (18mag) (16mag) Operation temperature 293 ± 5 293 ± 5 293 ± 5 range [K] Mass incl. 20% margin [kg] 225 kg 29 Optical schemes of WUVS channels UVES VUVES LSS 30 Spectrograph mock-ups 31 Detectors of WUVS: CCDs (e2v) STM, EM EM CCD 272 Custom design 4096 x 3112 12um pixel Back illuminated, UV coating 32 Подготовка к производству Problems with ITAR components Device delivery is forbidden by US for scientific satellite 33 WUVS efficiency (expected) 34 Field camera unit The first UV imager to be flown to a geosynchronous orbit (~ above the geocorona). 35 From ISSIS to FCU 36 Parameters of Field Camera Unit HST/ACS/S HST/WFC3/U Parameters ISSIS Far-UV Near-UV BC VIS MCP, MCP, analogue analogue of MCP, Detector CCD CCD of UVIT UVIT MAMA (Spain) (Spain) Spectral range, 174-310 (115- 115-310 115-176 115-170 200–1000 nm 1000) Effective area, 0.054 0.068 0.27 0.18 0.45 m2 Field of view, 70×75 121×121 597×451 34.59×30.8 162×162 arcsec×arcsec Angular resolution, 0.03 0.08 0.146 0.03 0.04 arcsec Detector size, 40 30 49×37 25 61×61 mm Number of 2х (5 + 2 Up to 10 Up to15 6 + 2 prism 42+5 filters neutral) 37 Field Camera Unit major features two channels: ➢ FUV channel with MCP detector, 115-176 nm o Solar blind detector o Diffraction-limited imaging in FUV o High sensitivity in photon-counting mode o High time resolution ➢ NUV channel with CCD detector, 174-310mn o Wide field of view o High dynamic range o High angular resolution o Low resolution field spectroscopy o Possibility for extended spectral range: 115-1000 nm 38 FCU preliminary layout 39 Chance for coronography? The IKI – NAOJ suggestion of the 3-rd channel is under consideration. It can be realised if funding, technical, political problems will not appear. 40 Science case for the new imager (stellar astrophysics) Study of planetary nebulae SN behavior in the UV Study of short timescale variable sources (40 ms) Asteroseismology Exoplanetary atmospheres Protostellar Jets The Galactic globular clusters and variables 41 WSO-UV Orbit Geosynchronous orbit was chosen based mainly on the following criteria: a) launcher capabilities; b) time of stay in the Earth Radiation Belts; c) Continuous visibility i=51.6o i=40o zones; d) minimum stay in the Earth shadow; e) stability of the orbit; WSO-UV geosynchronous orbit, f ) available technical equipment of the Space and Ground Segments for radio communication. 42 WSO-UV Ground Segment The GS includes : The Mission Operation Center (MOC, two fully mirror distributed parts located in Spain and Russia) with co- located control centers and ground stations are parts of the Ground Control Segment. The Science Operation Center (SOC), two fully mirror distributed parts located in Spain (UCM) and Russia (INASAN), which can be linked to various research centers. 43 First tests of the Russia-Spain WSO-UV control and data link (Jan 2010) 44 WSO-UV time sharing policy • Core Program (CP): Fundamental science to be carried by the project team • Funding Bodies Program (FBP): Guaranteed Time to the countries funding the project • Open Program (OP): Open program to the world wide scientific community Year 1-2 Year 3- ..... FBP FBP CP CP OP Others Others OP SHARING OF OBSERVATIONAL TIME 45 The WSO-UV Сore Program I.The diffuse baryonic content in the Universe and its chemical evolution: warm- hot IGM, damped Lyman-alpha systems, the role of starburts and the formation of galaxies. II.Stellar physics - activity on stars (obs. support of mass transfer theory in CB, mass loss from massive stars, physics of WD etc.). III.The early evolution of stars and role of UV in the evolution of the young planetary disks and astrochemistry in UV field.
Load more

Recommended publications
  • CASTOR: a Wide-Field, UV Space Telescope
    Astro2020 Activities and Projects White Paper CASTOR: A Wide-Field, UV Space Telescope Thematic Areas: Space Missions Ground-Based Activities and Projects Computation Astrophysics Theoretical Astrophysics Laboratory Astrophysics Principal Author: Peter L. Capak Name: Peter L. Capak Institution: Infrared Processing and Analysis Center, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA, 91125, USA Email: [email protected] Phone: (626) 395-6422 Co-authors: Michael L. Balogh (University of Waterloo), Jessie L. Christiansen (NASA Exo- planet Science Institute, Caltech), Patrick Cotˆ e´ (National Research Council of Canada), Olivier Dore´ (Caltech, JPL), Maria Drout (University of Toronto), Christopher J. Evans (UK Astronomy Technology Centre, Royal Observatory Edinburgh), Andreas L. Faisst (IPAC, Caltech), Sarah C. Gallagher (University of Western Ontario), Carl J. Grillmair (IPAC, Caltech), Paul Harrison (Magellan Aerospace), John B. Hutchings (National Research Council of Canada), JJ Kavelaars (National Research Council of Canada), J.-F. Lavigne (ABB), Janice C. Lee (IPAC, Caltech), Shouleh Nikzad (Jet Propulsion Laboratory, California Institute of Technology), Jason D. Rhodes (Jet Propulsion Laboratory, California Institute of Technology), Jason F. Rowe (Bishop’s Univer- sity), Ruben´ Sanchez-Janssen (UK Astronomy Technology Centre, Royal Observatory Edinburgh), Alan D. Scott (Honeywell Aerospace), Charles Shapiro (Jet Propulsion Laboratory, California In- stitute of Technology), Melanie Simet (University of California Riverside), Harry I. Teplitz (IPAC, Caltech), Kim A. Venn (University of Victoria), Ludovic Van Waerbeke (University of British Columbia) 1 Abstract: CASTOR (The Cosmological Advanced Survey Telescope for Optical and UV Re- search) is a proposed Canadian-led mission that would provide high-resolution imaging and spec- troscopy in the UV/optical (0.15–0.55 µm) spectral region.
    [Show full text]
  • Pushing the Limits of the Coronagraphic Occulters on Hubble Space Telescope/Space Telescope Imaging Spectrograph
    Pushing the limits of the coronagraphic occulters on Hubble Space Telescope/Space Telescope Imaging Spectrograph John H. Debes Bin Ren Glenn Schneider John H. Debes, Bin Ren, Glenn Schneider, “Pushing the limits of the coronagraphic occulters on Hubble Space Telescope/Space Telescope Imaging Spectrograph,” J. Astron. Telesc. Instrum. Syst. 5(3), 035003 (2019), doi: 10.1117/1.JATIS.5.3.035003. Downloaded From: https://www.spiedigitallibrary.org/journals/Journal-of-Astronomical-Telescopes,-Instruments,-and-Systems on 02 Jul 2019 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use Journal of Astronomical Telescopes, Instruments, and Systems 5(3), 035003 (Jul–Sep 2019) Pushing the limits of the coronagraphic occulters on Hubble Space Telescope/Space Telescope Imaging Spectrograph John H. Debes,a,* Bin Ren,b,c and Glenn Schneiderd aSpace Telescope Science Institute, AURA for ESA, Baltimore, Maryland, United States bJohns Hopkins University, Department of Physics and Astronomy, Baltimore, Maryland, United States cJohns Hopkins University, Department of Applied Mathematics and Statistics, Baltimore, Maryland, United States dUniversity of Arizona, Steward Observatory and the Department of Astronomy, Tucson Arizona, United States Abstract. The Hubble Space Telescope (HST)/Space Telescope Imaging Spectrograph (STIS) contains the only currently operating coronagraph in space that is not trained on the Sun. In an era of extreme-adaptive- optics-fed coronagraphs, and with the possibility of future space-based coronagraphs, we re-evaluate the con- trast performance of the STIS CCD camera. The 50CORON aperture consists of a series of occulting wedges and bars, including the recently commissioned BAR5 occulter. We discuss the latest procedures in obtaining high-contrast imaging of circumstellar disks and faint point sources with STIS.
    [Show full text]
  • Precollimator for X-Ray Telescope (Stray-Light Baffle) Mindrum Precision, Inc Kurt Ponsor Mirror Tech/SBIR Workshop Wednesday, Nov 2017
    Mindrum.com Precollimator for X-Ray Telescope (stray-light baffle) Mindrum Precision, Inc Kurt Ponsor Mirror Tech/SBIR Workshop Wednesday, Nov 2017 1 Overview Mindrum.com Precollimator •Past •Present •Future 2 Past Mindrum.com • Space X-Ray Telescopes (XRT) • Basic Structure • Effectiveness • Past Construction 3 Space X-Ray Telescopes Mindrum.com • XMM-Newton 1999 • Chandra 1999 • HETE-2 2000-07 • INTEGRAL 2002 4 ESA/NASA Space X-Ray Telescopes Mindrum.com • Swift 2004 • Suzaku 2005-2015 • AGILE 2007 • NuSTAR 2012 5 NASA/JPL/ASI/JAXA Space X-Ray Telescopes Mindrum.com • Astrosat 2015 • Hitomi (ASTRO-H) 2016-2016 • NICER (ISS) 2017 • HXMT/Insight 慧眼 2017 6 NASA/JPL/CNSA Space X-Ray Telescopes Mindrum.com NASA/JPL-Caltech Harrison, F.A. et al. (2013; ApJ, 770, 103) 7 doi:10.1088/0004-637X/770/2/103 Basic Structure XRT Mindrum.com Grazing Incidence 8 NASA/JPL-Caltech Basic Structure: NuSTAR Mirrors Mindrum.com 9 NASA/JPL-Caltech Basic Structure XRT Mindrum.com • XMM Newton XRT 10 ESA Basic Structure XRT Mindrum.com • XMM-Newton mirrors D. de Chambure, XMM Project (ESTEC)/ESA 11 Basic Structure XRT Mindrum.com • Thermal Precollimator on ROSAT 12 http://www.xray.mpe.mpg.de/ Basic Structure XRT Mindrum.com • AGILE Precollimator 13 http://agile.asdc.asi.it Basic Structure Mindrum.com • Spektr-RG 2018 14 MPE Basic Structure: Stray X-Rays Mindrum.com 15 NASA/JPL-Caltech Basic Structure: Grazing Mindrum.com 16 NASA X-Ray Effectiveness: Straylight Mindrum.com • Correct Reflection • Secondary Only • Backside Reflection • Primary Only 17 X-Ray Effectiveness Mindrum.com • The Crab Nebula by: ROSAT (1990) Chandra 18 S.
    [Show full text]
  • Detection of Large-Scale X-Ray Bubbles in the Milky Way Halo
    Detection of large-scale X-ray bubbles in the Milky Way halo P. Predehl1†, R. A. Sunyaev2,3†, W. Becker1,4, H. Brunner1, R. Burenin2, A. Bykov5, A. Cherepashchuk6, N. Chugai7, E. Churazov2,3†, V. Doroshenko8, N. Eismont2, M. Freyberg1, M. Gilfanov2,3†, F. Haberl1, I. Khabibullin2,3, R. Krivonos2, C. Maitra1, P. Medvedev2, A. Merloni1†, K. Nandra1†, V. Nazarov2, M. Pavlinsky2, G. Ponti1,9, J. S. Sanders1, M. Sasaki10, S. Sazonov2, A. W. Strong1 & J. Wilms10 1Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany. 2Space Research Institute of the Russian Academy of Sciences, Moscow, Russia. 3Max-Planck-Institut für Astrophysik, Garching, Germany. 4Max-Planck-Institut für Radioastronomie, Bonn, Germany. 5Ioffe Institute, St Petersburg, Russia. 6M. V. Lomonosov Moscow State University, P. K. Sternberg Astronomical Institute, Moscow, Russia. 7Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia. 8Institut für Astronomie und Astrophysik, Tübingen, Germany. 9INAF-Osservatorio Astronomico di Brera, Merate, Italy. 10Dr. Karl-Remeis-Sternwarte Bamberg and ECAP, Universität Erlangen-Nürnberg, Bamberg, Germany. †e-mail: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]; [email protected] The halo of the Milky Way provides a laboratory to study the properties of the shocked hot gas that is predicted by models of galaxy formation. There is observational evidence of energy injection into the halo from past activity in the nucleus of the Milky Way1–4; however, the origin of this energy (star formation or supermassive-black-hole activity) is uncertain, and the causal connection between nuclear structures and large-scale features has not been established unequivocally.
    [Show full text]
  • Observations of Comet IRAS-Araki-Alcock (1983D) at La Silla T
    - 12 the visual by 1.3 mag). Like for the other SOor variables we M explain this particular finding by the very high mass loss (M = Bol 5 6.10- M0 yr-') during outburst. The variations in the visual are caused by bolometric flux redistribution in the envelope whilst -10 the bolometric luminosity remains practically constant. The location of R127 in the Hertzsprung-Russell diagram together with the other two known SOor variables of the LMC -B are shown in fig. 8. We note that Walborn classified R127 as an Of or alterna­ tively as a late WN-type star. This indicates that the star is a late Of star evolving right now towards a WN star. Since we have -6 detected an SOor-type outburst of this star we conclude that this transition is not a smooth one but is instead accompanied '.8 '.6 4.0 3.6 by the occasional ejection of dense envelopes. Fig. 8: Location of the newly discovered S Dar variable R 127 in the References Hertzsprung-Russell diagram in comparison with the other two estab­ lished SOor variables of the LMG. Also included in the figure is the Conti, P. S.: 1976, Mem. Soc. Roy. Sei. Liege 9,193. upper envelope of known stellar absolute bolometric magnitudes as Dunean, J. C.: 1922, Publ. Astron. Soc. Pacific 34, 290. derived byHumphreys andDavidson (1979). The approximateposition Hubble, E., Sandage, A.: 1953, Astrophys. J. 118, 353. o( the late WN-type stars is also given. Humphreys, R. M., Davidson, K.: 1979, Astrophys. J. 232,409. Lamers, H.
    [Show full text]
  • Highlights in Space 2010
    International Astronautical Federation Committee on Space Research International Institute of Space Law 94 bis, Avenue de Suffren c/o CNES 94 bis, Avenue de Suffren UNITED NATIONS 75015 Paris, France 2 place Maurice Quentin 75015 Paris, France Tel: +33 1 45 67 42 60 Fax: +33 1 42 73 21 20 Tel. + 33 1 44 76 75 10 E-mail: : [email protected] E-mail: [email protected] Fax. + 33 1 44 76 74 37 URL: www.iislweb.com OFFICE FOR OUTER SPACE AFFAIRS URL: www.iafastro.com E-mail: [email protected] URL : http://cosparhq.cnes.fr Highlights in Space 2010 Prepared in cooperation with the International Astronautical Federation, the Committee on Space Research and the International Institute of Space Law The United Nations Office for Outer Space Affairs is responsible for promoting international cooperation in the peaceful uses of outer space and assisting developing countries in using space science and technology. United Nations Office for Outer Space Affairs P. O. Box 500, 1400 Vienna, Austria Tel: (+43-1) 26060-4950 Fax: (+43-1) 26060-5830 E-mail: [email protected] URL: www.unoosa.org United Nations publication Printed in Austria USD 15 Sales No. E.11.I.3 ISBN 978-92-1-101236-1 ST/SPACE/57 *1180239* V.11-80239—January 2011—775 UNITED NATIONS OFFICE FOR OUTER SPACE AFFAIRS UNITED NATIONS OFFICE AT VIENNA Highlights in Space 2010 Prepared in cooperation with the International Astronautical Federation, the Committee on Space Research and the International Institute of Space Law Progress in space science, technology and applications, international cooperation and space law UNITED NATIONS New York, 2011 UniTEd NationS PUblication Sales no.
    [Show full text]
  • Annexe: Summary of Soviet and Russian Space Science Missions
    Contents Introduction by the authors ..................................... ix Acknowledgments ............................................ xi Glossary .................................................. xiii Terminological and translation notes ..............................xv Reference notes .............................................xvii List of tables ............................................... xix List of illustrations ......................................... xxiii List of figures .............................................xxvii 1 Early space science ........................................... 1 Space science by balloon....................................... 3 Scientific flights into the atmosphere: the Akademik series..............14 Scientific test flights with animals ................................20 The idea of a scientific Earth satellite .............................23 Scientific objectives of the first Earth satellites . ....................25 Key people .................................................25 Instead, Prosteishy Sputnik .....................................27 PS2......................................................29 Object D: the first large scientific satellite in orbit....................33 Early space science: what was learned? ............................37 References .................................................39 2 Deepening our understanding ....................................43 Following Sputnik: the MS series ................................43 Cosmos 5 and Starfish: introducing Yuri Galperin
    [Show full text]
  • The World Space Observatory: Ultraviolet Mission: Science Program and Status Report
    PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie The World Space Observatory: ultraviolet mission: science program and status report Sachkov, M., Gómez de Castro, A. I., Shustov, B. M. Sachkov, A. I. Gómez de Castro, B. Shustov, "The World Space Observatory: ultraviolet mission: science program and status report," Proc. SPIE 11444, Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, 1144473 (13 December 2020); doi: 10.1117/12.2562929 Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online Only Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 19 Jan 2021 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use The World Space Observatory - Ultraviolet mission: science program and status report M. Sachkov*a , A.I. Gómez de Castrob, B. Shustova aInstitute of Astronomy of Russian Academy of Sciences, Pyatnitskaya str., 48, Moscow, 119017, Russia; bAEGORA Research Group, Fac. CC. Matematicas, Universidad Complutense, Plaza de Ciencias 3, 28040, Madrid, Spain ABSTRACT A general description of the international space mission "Spectr-UF" (World Space Observatory-Ultraviolet) is given. The project is aimed to create a large space telescope to work in the UV wavelength domain (115 - 310 nm). In the Federal Space Program of Russia for 2016-2025 the launch of the project is scheduled for 2025. We implement several important improvements: updated scientific program of the project; a new design of the Field Camera Unit instrument; corrected orbit; developed a system of collecting applications etc. This paper briefly describes the current status of the mission. Keywords: ultraviolet, spectroscopy, imaging, exoplanet, UV space telescope, WSO-UV 1. INTRODUCTION The Earth's atmosphere blocks observations of celestial objects in the ultraviolet (UV) part of the electromagnetic spectrum.
    [Show full text]
  • INDIA JANUARY 2018 – June 2020
    SPACE RESEARCH IN INDIA JANUARY 2018 – June 2020 Presented to 43rd COSPAR Scientific Assembly, Sydney, Australia | Jan 28–Feb 4, 2021 SPACE RESEARCH IN INDIA January 2018 – June 2020 A Report of the Indian National Committee for Space Research (INCOSPAR) Indian National Science Academy (INSA) Indian Space Research Organization (ISRO) For the 43rd COSPAR Scientific Assembly 28 January – 4 Febuary 2021 Sydney, Australia INDIAN SPACE RESEARCH ORGANISATION BENGALURU 2 Compiled and Edited by Mohammad Hasan Space Science Program Office ISRO HQ, Bengalure Enquiries to: Space Science Programme Office ISRO Headquarters Antariksh Bhavan, New BEL Road Bengaluru 560 231. Karnataka, India E-mail: [email protected] Cover Page Images: Upper: Colour composite picture of face-on spiral galaxy M 74 - from UVIT onboard AstroSat. Here blue colour represent image in far ultraviolet and green colour represent image in near ultraviolet.The spiral arms show the young stars that are copious emitters of ultraviolet light. Lower: Sarabhai crater as imaged by Terrain Mapping Camera-2 (TMC-2)onboard Chandrayaan-2 Orbiter.TMC-2 provides images (0.4μm to 0.85μm) at 5m spatial resolution 3 INDEX 4 FOREWORD PREFACE With great pleasure I introduce the report on Space Research in India, prepared for the 43rd COSPAR Scientific Assembly, 28 January – 4 February 2021, Sydney, Australia, by the Indian National Committee for Space Research (INCOSPAR), Indian National Science Academy (INSA), and Indian Space Research Organization (ISRO). The report gives an overview of the important accomplishments, achievements and research activities conducted in India in several areas of near- Earth space, Sun, Planetary science, and Astrophysics for the duration of two and half years (Jan 2018 – June 2020).
    [Show full text]
  • The Status of the Hubble Space Telescope
    al insights into the atmospheric struc- ture of hot stars. It is essential, although time consum- ing, to disentangle effects due to binari- ty from effects reflecting the kinematics of the stellar group (11). Especially the lack of recognition of wider binaries with an RV amplitude of the order of 10 kmls might significantly influence the conclu- sions. Hence, repetition of RV observa- tions is necessary and will in turn in- crease our knowledge on binarity in the selected young stellar groups. The spectra will in addition allow a study of stellar rotation in these star groups (12). In many respects, this project forms an extension towards the earliest spec- tral types of the key programmes of Mayor et al. and Gerbaldi et al. (de- scribed in the Messenger 56), even when the primary scientific motivation is somewhat different. In addition to the common interest in radial velocities, the stars in Sco-Cen are also observed by the Hipparcos satellite, providing space motions when combined with the RVs. Using these, we hope to reconstruct the initial minimal volumes in which the star formation occurred which gave rise to the presently expanding Sco-Cen sub- 4180 4200 4220 4240 4260 4280 groups, and to discuss the possibility of wavelength (angstrom) sequential star formation (13). Part of the CASPEC spectrum of NGC 2244-201, a 10th magnitude B 1 V star. The strongest lines are 011 4185, 011 4 190, NII 4242, 011 4254, CII 4267, a complex of 011 lines around First Results 4277A, 011 4283, Slll4285 and 011 4286. Strictly within the frame of the key programme, the first spectra have been obtained on 3 nights in May 1990.
    [Show full text]
  • English and Russian Only
    A/AC.105/C.1/2013/CRP.22 18 February 2013 English and Russian only Committee on the Peaceful Uses of Outer Space Scientific and Technical Subcommittee Fiftieth session Vienna, 11-22 February 2013 International cooperation in the peaceful uses of outer space: activities of Member States* Note by the Secretariat I. Introduction 1. In the report on its forty-ninth session, the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space recommended that the Secretariat continue to invite Member States to submit annual reports on their space activities (A/AC.105/1001, para. 29). 2. In a note verbale dated 31 July 2012, the Secretary-General invited Governments to submit their reports by 19 October 2012. The present note was prepared by the Secretariat on the basis of a report received from the Russian Federation after 19 October 2012 in response to that invitation. 3. The replies contained in the present document are original documents, as submitted, and were not formally edited. __________________ * The present paper is reproduced in the form in which it was received. V.13-80960 (E) *1380960* A/AC.105/C.1/2013/CRP.22 II. Replies received from Member States Russian Federation [English] National activities and international cooperation of the Russian Federation in the exploration and use of outer space for peaceful purposes in 2012 (as at 31 December 2012) The national space activities of the Russian Federation in 2012 were carried out by the Russian Federal Space Agency (Roscosmos) under the Russian Federal Space Programme, the Global Navigation Satellite System (GLONASS) special federal programme and other special programmes, in cooperation with the Russian Academy of Sciences, the Ministry of Defence of the Russian Federation and other clients and users of space information and services.
    [Show full text]
  • The UV Perspective of Low-Mass Star Formation
    galaxies Review The UV Perspective of Low-Mass Star Formation P. Christian Schneider 1,* , H. Moritz Günther 2 and Kevin France 3 1 Hamburger Sternwarte, University of Hamburg, 21029 Hamburg, Germany 2 Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research; Cambridge, MA 02109, USA; [email protected] 3 Department of Astrophysical and Planetary Sciences Laboratory for Atmospheric and Space Physics, University of Colorado, Denver, CO 80203, USA; [email protected] * Correspondence: [email protected] Received: 16 January 2020; Accepted: 29 February 2020; Published: 21 March 2020 Abstract: The formation of low-mass (M? . 2 M ) stars in molecular clouds involves accretion disks and jets, which are of broad astrophysical interest. Accreting stars represent the closest examples of these phenomena. Star and planet formation are also intimately connected, setting the starting point for planetary systems like our own. The ultraviolet (UV) spectral range is particularly suited for studying star formation, because virtually all relevant processes radiate at temperatures associated with UV emission processes or have strong observational signatures in the UV range. In this review, we describe how UV observations provide unique diagnostics for the accretion process, the physical properties of the protoplanetary disk, and jets and outflows. Keywords: star formation; ultraviolet; low-mass stars 1. Introduction Stars form in molecular clouds. When these clouds fragment, localized cloud regions collapse into groups of protostars. Stars with final masses between 0.08 M and 2 M , broadly the progenitors of Sun-like stars, start as cores deeply embedded in a dusty envelope, where they can be seen only in the sub-mm and far-IR spectral windows (so-called class 0 sources).
    [Show full text]