The WSO-UV mission. B. Shustov, A.I. G'omez de Castro and the WSO-UV team

Transcription

1 The WSO-UV mission B. Shustov, A.I. G'omez de Castro and the WSO-UV team

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3 UV missions and instruments (in the past and present) name OAO-2 TD-1A OAO-3 ANS IUE ASTRON EXOSAT X ROSAT X HST EUVE ALEXIS X MSX FUSE XMM X GALEX SWIFT γ,x launch year.month size of instrument cm x х35 (4) type of pointing sp s p p p p p sp p sp s s p p sp p mode of observ. is is s s s s is i isp is i i s is is i λλ angstrom

4 ASTRON An UV space observatory with 80 cm aperture telescope and scanning spectrometer onboard ( ). Significant results: first detection of H 2 O in Halley comet, UV spectroscopy of SN1987a, Pb lines in stellar spectra etc. (Photo of flight model at Lavochkin Museum) 4

5 Spektr (Спектр) missions for astrophysics Federal Space Program ( ) includes as major projects: Spektr-R (Radioastron) launched in 2011 Spektr-RG launch is planned for 2014 Spektr-UF (World Space Observatory Ultraviolet) launch International name is World Space Observatory Ultraviolet (introduced by Willem Wamsteker) 5

6 WSO-UV Project WSO-UV (World Space Observatory Ultraviolet) project is an international space observatory designed for observations in the UV ( nm) where some of the most important astrophysical processes can be efficiently studied with unprecedented capability. The observatory includes a 170 cm aperture telescope capable of high-resolution spectroscopy, long slit lowresolution spectroscopy, and deep UV and optical imaging. At present cooperation on the project includes Russia and Spain as major partners, Ukraine and Germany as minor ones. 6

7 WSO-UV mission model Telescope: T-170M, 1.7 m, f/10 Russia Spectrographs: WUVS, Russia Imagers: ISSIS, Spain Platform: Navigator, Russia Orbit: geosynchronous, i=51.6 o Launcher, launch: ZENIT 2SB, end of 2016, Russia Ground Segment: Russia and Spain 7

8 Cooperation in Russia INASAN major subcontractors Lavochkin Association + subcontractors Institute of Astronomy, RAS (INASAN) Lytkarino Optical Plant Physical Inst. RAS, ITMO-State Optical Inst. VNIIEF Luch Co. Space Research Inst. RAS (IKI) Primary contractor for the Project: The T-170M Telescope, Platform, Launch, Mission control center Primary subcontractor: Science Instrumentation Ground Segment (SOC) Manufacturing optics of the T-170M UV-spectrographs (detectors, optical elements, AIV) UV-spectrographs (mechanics) Coatings of optical elements On-board Sci. Instr. Control and Data Management System, Fine Guidance System

9 The WSO-UV S/C 9

10 Life time The Navigator platform Spacecraft mass (wet) Payload mass > 5 years 2 900Kg 1 600Kg The power consumption of P/L 750W Data transmission rate Stabilization and pointing accuracy using the FGS (3σ) 4 Mbit s arcsec The platform was successfully in-flight tested during: 1. Electro (remote sensing mission) 2. Spektr-R 10

11 The T-170M telescope Optical system Aperture diameter Telescope f-number 10.0 Field angular diameter Primary wavelength Scale Mass Optical quality Ritchey Chrètien aplanat 1700 mm 0.50 (300mm diameter) 200 nm 81 mkm/arc sec kg Diffraction optics at the center of FOV 11

12 T-170M Telescope Model at Lavochkin Association. 12

13 T-170M optics Al+MgF 2 coating deposition onto primary mirror in Luch (in Denton vacuum camera) 13

14 T-170M optics reflectivity Reflectivity is close to best reported Microroughness: rms 0.75 nm before coating, 1 nm after coating 14

15 T170M instrument compartment 15

16 WUVS (WSO-UV Spectrograph) Three channels (spectrographs) of the WUVS : Vacuum Ultraviolet Echele Spectrograph VUVES nm, R Ultraviolet Echele Spectrograph UVES nm, R Long Slit Spectrograph LSS nm, R=

17 WUVS CCD detector enclosure concept (e2v) Contract between e2v and Lebedev Physical Institute of the RAS is signed. Drive electronic (RAL) 17

18 WUVS optical system prototype in laboratory (at SOI) Echelle grating prototype 18

19 WUVS efficiency (factors) 19

20 WUVS efficiency (expected) 20

21 Two channels for imaging and slitless spectroscopy: The Far Ultraviolet Channel (FUV), providing the optimum sensitivity in the Å interval, and equipped with a CsI MCP detector The Near Ultraviolet Channel (NUV) covering wavelegnths in the Å range; the detector is a CsTe MCP. ISSIS (IMAGING AND SLITLESS SPECTROSCOPY INSTRUMENT FOR SURVEYS) ISSIS STM at SENER 21

22 Comparison of effective areas for ISSIS, GALEX and SBC in imaging mode. 22

23 WSO-UV Orbit WSO-UV geosynchronous orbit, i=51.6 o 23

24 WSO-UV Ground Segment The GS includes : The Mission Operation Center (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 (two fully mirror distributed parts located in Spain and Russia), which can be linked to various research centers. 24

25 Astrophysics in UV recent issues next ESO/NUVA/IAG Workshop on Challenges in UV Astronomy, ESO Garching, 7-11 October

26 WSO-UV Scientific Programs Core Program (CP): The CP of scientific observations with the WSO-UV is defined to allow the conduction of high impact or legacy scientific projects that deserve large amounts of observing time. They are selected on the basis of their scientific excellence. Open Program (OP): The Open Program consists of astronomical observations obtained with the WSO-UV by astronomers who may or may not belong to the WSO-UV international consortium. Funding Bodies Program (FBP): The Funding Bodies (FBs) Program is the guaranteed time granted to each one of the national bodies funding the WSO-UV project. 26

27 On the time sharing policy During the first year: 45% for CP, 45% for FBP, 8% OT, 2% DDT (Director Discretionary Time). During the second and third years: 30% for CP, 40% for FBP, 28% OT, 2% DDT. For the following years: 60% for FBP, 38% OT, 2% DDT. 27

28 The WSO-UV core program I. The Cosmic Web (history of reionization, search for baryons). II. III. IV. Stellar physics - activity on stars (obs. support of mass transfer theory in CB, physics of WD etc.). The early evolution of stars and role of UV in the evolution of the young planetary disks and astrochemistry in UV field. Atmospheres of (exo)planets

29 Important! We are grateful to all the scientists and technical experts from various countries who helped and help to implement the WSO-UV! We expect active international interest and scientific participation of the world astronomical community in the WSO-UV Project! 29

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