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.