The World Space Observatory for UltraViolet Project WSO-UV

1. The World Space Observatory for UltraViolet ProjectWSO-UV Isabella Pagano,  Martin Barstow, Noah Brosch, Ana Ines Gómez de Castro,  Mahoai Huang, Norbert Kappelmann, Giampaolo Piotto, Salvatore Scuderi, Mikhail Sachkov, Boris Shustov, Klaus Werner, Gang Zhao

2. WSO-UV General Information HST after SM4

3. Why UV? • Mostresonance transitionsfrom ions, atoms, molecules of astrophysical significance are in theultravioletwavelength domain.  • UVprovides the most sensitive tools: • to trace the distribution of (baryonic) matter in the Universe, • to diagnose the chemical composition, physical properties and kinematics of astronomical objects of all types. HST after SM4

4. WSO-UV SUVO ? 1970 1980 1990 2000 2010 2020 COPERNICUSIUEASTRONHSTFUSE GALEX year HST after SM4

5. WSO-UV collaboration

6. Telescope T-170 The WSO-UV telescope (T-170M) is under the responsibility of Lavochkin Association (Russia). Optical elements are being manufactured by the Lytkarino Optical Glass Factory (Russia). The main units of the structural model of the T-170 telescope have successfully passed vibrostatic and thermal vacuum tests.

7. The Navigator platform • The WSO-UV bus is the “Navigator” service module used for other Russian projects: e.g. “Electro” and “Radioastron” that will fly before WSO-UV, and Spectrum X-gamma which will follow WSO-UV. • The “Navigator” of WSO-UV requires adaptation of radio complex, antenna-feeder system and software of on-board control system in terms of precision telescope pointing. HST after SM4

8. WSO-UV Orbit • Geosynchronous • Altitude: 35860 km • Inclination: 51.8° For the chosen orbit the effects of the radiation belts will be negligible and the observing efficiency high. HST after SM4

9. WSO-UV Payload PMU frame FCU: 3-channel Imager: FUV, NUV, UVO FGS: Fine Guidance System (3 sensors 1kx1k) HIRDES: high-resechelle spectrographs: UVES (178-320nm) VUVES (102-180nm) LSS: 102- 320 nm, low-res long slit spectrograph Optical Bench (CeSiC) HST after SM4

10. High Resolution Double Echelle Spectrograph WSO-UV HIRDES Funding Agency: DLR Science Contractor: Universität Tübingen, Institut für Astronomie und Astrophysik Industry Contractor: Kayser Threde Principal Investigator: Prof. Dr. Klaus Werner (IAT) Instrument Scientist: Dr. Norbert Kappelmann (IAT) Heritage: ORFEUS flown on the Space Shuttle on two space shuttle flights in 1993 and 1996 (Barnstedt et al. 1999, Richter et al. 1999). STATUS: Phase B1 completed HST after SM4

11. WSO-UV HIRDES See poster by Werner et al. HST after SM4

12. HIRDES effective area HST after SM4

13. Exposure time calculator http://astro.uni-tuebingen.de/groups/wso_uv/exptime_calc.shtml HST after SM4

14. WSO-UV LSS • Long Slit Spectrograph Funding Agency: CNAS Science Contractor: National Astronomical Observatories of China Academy of Science (NAOC) Industry Contractor: to be selected Principal Investigator: Prof. Gang Zhao (CAS) STATUS: Phase A completed. Phase B1 end in Mar 2008 HST after SM4

15. LSS Spectrograph HST after SM4

16. WSO-UV FCU • Field Camera Unit Funding Agency: ASI Science Contractor: Istituto Nazionale di Astrofisica (INAF) Industry Contractor: to be selected Principal Investigator: Dr.Isabella Pagano (INAF-CT) Instrument Scientist: Prof. Giampaolo Piotto (UnIv. PD) Project Manager: Dr. Salvatore Scuderi (INAF CT) STATUS: Phase B1 completed HST after SM4

17. Main FCU parameters See poster by Scuderi et al. HST after SM4

18. FCU vs. ACS/WFC3 • UVO: 2 times larger field of view than ACS, and 3 times larger than WFC3/UVIS; high angular resolution (diffraction limit @500nm). Undersampled, but sampling as for ACS and WFC3 • FUV: same field as UVO; Much larger than the ACS/SBC field of view, (lower angular resolution, but still OK for many surveys) • NUV: high angular resolution similar to ACS/SBC + ACS/HRC, but four times larger field of view than ACS/SBC + ACS/HRC; unique spectropolarimetry facilities.

19. FCU Layout UVO Channel Calibration Unit FUV Channel NUV Channel HST after SM4

20. Filters HST after SM4

21. FCU Operation Modes • Optical Mode • Imaging (FUV, NUV, UVO) • Slitless spectroscopy (FUV, NUV, UVO) • Polarimetry (NUV, UVO) • Slitless spectropolarimetry (NUV) • Parallel Observing Mode • One Channel of FCU & one spectrograph • High Temporal Resolution Mode • Time Tag (MCP) • Windowing (CCD, MCP) • Calibration Mode HST after SM4

22. FCU Performances HST after SM4

23. Hubble Deep Field UV countpart Left: A true colour image of part of the UDF: the blue and green channels are respectively GALEX FUV (~1500A, ~75Ks) and GALEX NUV (~2000A, ~76 Ks), while the red channel is the VIMOS@VLT deep imaging (~36000Ks) in band U. Most of the red "noise" are objects detected in ground based U band imaging, but not detected in GALEX data. The depth of GALEX data is 25-26 AB, with a PSF of 4". The size of the image is 2'x2'. Right:A true colour image with a simulation of the same field of the previous image: the blue and green channels are the WSO-FUV and WSO-NUV respectively, while the red is U band image. HST after SM4

24. Simulations The triple main sequence as obtained from simulated UVO data. The triple main sequence of NGC 2808 GC as observed by the ACS@HST camera HST after SM4

25. WSO-UV Key Science Drivers WSO-UV is a multipurpose telescope. • It will give a big contribution to answer some of the key questions for the next decade recently formulated by ASTRONET in the documentScience Vision for the European Astronomy: • Do we understand the extreme of the Universe? • How do Galaxies form and Evolve? • What is the origin and evolution of stars and planets? • How do we fit in? HST after SM4

26. WSO-UV Key Science Drivers arXiv:0712.0970v1 Science Vision for the European Astronomy: • Do we understand the extreme of the Universe? • How do Galaxies form and Evolve? • What is the origin and evolution of stars and planets? • How do we fit in? HST after SM4

27. Status of the WSO-UV International Collaboration

28. Agreements SMP HST after SM4

29. WSO-UV SMP • Definition of authorities: • WSO Scientific Supervision Committee (WSSC) • Science Verification Working Team (SVWT) • Time Allocation Committee (TAC) • Definition of the Time Sharing Policy HST after SM4

30. Time Sharing Policy The telescope time available for astronomical observations will be divided in: • Guaranteed time: • funding bodies program (FBP): National time assigned proportionally to the financial contribution to the project • core or observatory program (CP) defined jointly by the WSO consortium (more info later) • Open Program (OP) to the whole astronomical community worldwide allocated by an International Committee • Discretionary Director Time (DDT) up to a maximum of 2% HST after SM4

31. Thanks For further info during the meeting: • Russian Team - M. Sachkov, E. Kilpio, A. Shugarov • HIRDES Team - K. Werner • FCU team - I. Pagano, S. Scuderi, G. Piotto, M. Turatto, F. Ferraro, E. Brocato, D. De Martino, C. Cacciari, L. Buson, E. Pian WEB Sites • Russia: http://wso.inasan.ru/ • Italy: http://www.oact.inaf.it/wso/index.htm • Germany: http://astro.uni-tuebingen.de/groups/wso_uv/ • China: http://earth.bao.ac.cn/wso • Spain: http://www.mat.ucm.es/wso/index.php?