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Italian Part i cipation in the World Space Observatory / Ultraviolet Project

Italian Part i cipation in the World Space Observatory / Ultraviolet Project. The Field Camera Unit for WSO-UV. Dr. I sabella Pagan o INAF - Osservatorio Astrofisico di Catania PI of the WSO/UV Field Camera Unit (FCU) WSO/UV Implementation Committee member.

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Italian Part i cipation in the World Space Observatory / Ultraviolet Project

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  1. Italian Participation in the World Space Observatory / UltravioletProject The Field Camera Unit for WSO-UV Dr. Isabella Pagano INAF - Osservatorio Astrofisico di Catania PI of the WSO/UV Field Camera Unit (FCU) WSO/UV Implementation Committee member WSO/UV Italian web site:http://www.oact.inaf.it/wso/index.htm/

  2. WSO-UV @ INAF OACT • INAF OA Catania is the leading institute for the contract ASI/INAF No. I/085/06/0: Italian Participation in the World Space Observatory / Ultraviolet Project • Involvement in the international team of WSO-UV since the beginning of the effort to involve national agencies • Proposal submitted to ASI in Nov 2003 – approval Nov 2005 (Italian PASN) – contract Dec 2006. • KOM on Jan 18 2007 • Phase A review on Jul 12 2007 • Phase B1 review on Dec 20 2007 Visiting Committee @OACT

  3. WSO-UV in Italy • INAF • Catania Obs., Napoli Obs., Padova Obs., Milano IASF, Bologna IASF & Obs., Torino Obs., Trieste Obs., Cagliari Obs., Teramo Obs., Roma IASF. • Universities • DASS Firenze, Dip. Astr. Padova, Dip. Astr. Univ. Bologna, Univ. Pisa • Industrial support • Galileo Avionica, Thales Alenia Space Italy (MI) About 20 FTE involved in WSO-UV during 2007. Visiting Committee @OACT

  4. People involved @ INAF-OACT Researchers • Isabella Pagano (Principal Investigator, Project Manager) – 80% time • Salvatore Scuderi (System Engineer, Responsible for the UVO channel) - 80% time • Cristian Pontoni (Responsible for the Thermal-mechanical design) – full time • Matteo Munari (Optical design team) – full time • Giovanni Bonanno (Advisor) – 5% time • Massimo Turatto (Science Team) – from 2008 • In the past: • Marcello Rodonò Technicians • Saro Di Benedetto (Detectors) – 15% time • Vincenzo Greco (Electronics) – 5% time Administration • Daniela Recupero (Project assistant) – 10% time • In the past: • Giuseppe Caripoli (Project assistant) – 10% time (May 2006-Feb 2007) Visiting Committee @OACT

  5. WSO-UV General Information Visiting Committee @OACT

  6. WSO-UV Collaboration

  7. Telescope T-170 The WSO/UV telescope (T-170M) is a new version of the T-170 telescope designed in Russia by Lavochkin Association for Spectrum-UV mission. BAFFLES Visiting Committee @OACT

  8. The Navigator platform • The WSO-UV bus is the “Navigator” service module used for other Russian projects: e.g. “Electro”, and “Radioastron”. • 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. Visiting Committee @OACT

  9. WSO-UV Payload • HIRDES: R  60,000echelle spectrographs: • UVES (178-320nm) • VUVES (102-180nm) • LSS: 102- 320 nm, R~1500–2500 long slit (1x75 arcsec) spectrograph • FCU: 3-channel imaging cameras: • FUV • NUV • UVO • FGS: Fine Guidance System (3 sensors 1kx1k) Visiting Committee @OACT

  10. The Italian participation to WSO-UV

  11. Recommendation from the community Visiting Committee @OACT

  12. ASI Aero Space Plan 2006-2008 • Nov 2005: ASI release of the Italian National Aero-Space Plan (PASN) for 2006-2008  WSO/UV is inside the PASN Visiting Committee @OACT

  13. WSO-UV in the INAF LTP Visiting Committee @OACT

  14. 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 (see later) • Discretionary Director Time (DDT) up to a maximum of 2% Visiting Committee @OACT

  15. The Field Camera Unit Instrument

  16. Activities performed during the Phase A/B1 • Define the key science objectives of the imager  • Define the Top Level Requirements for the imager  • Produce the technical project of "Field Camera Unit" (FCU) Visiting Committee @OACT

  17. The Instruments Compartment…. other views Spectrographs Imagers Visiting Committee @OACT

  18. Our goal • Top Science • Build a compelling instrument and give the community tools: • to extend ambitious legacy program started with HST. • to complement other contemporary facilities in specific field: e.g. to perform astrometry with the same precision of GAIA in crowded fields where GAIA fails • to allow for the first time high resolution FUV imaging with a wide field Visiting Committee @OACT

  19. Key Science Drivers • The Italian WSO-UV Science Team released a document at the end of Phase A study (Jul 2007) where the Key Science Drivers for WSO-UV are discussed. • Following the structure of the “A Science Vision for the European Astronomy” document prepared by the European ASTRONET consortium, the Italian WSO-UV Science Team shows how WSO-UV contributes to answer, in the next decade, the four key questions: • 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? Visiting Committee @OACT

  20. WSO-UV Imager criteria • Large wavelength coverage (115-800nm) • Large field of view • High spatial resolution; this is mandatory to: • Morphological studies (e.g. planets, planetary nebulae, star formation regions, external galaxies) • High accuracy stellar photometry • High accuracy stellar astrometry • Resolve stars in crowded fields (e.g. in star clusters, external galaxies, star formation in AGNs) Visiting Committee @OACT

  21. Science Requirements • The requirements toward the imager instrument on board WSO-UV in order to fulfill its science objectivesare: • the possibility to obtain diffraction limited images for >230 nm (goal  >200 nm). • S/N=10 per pixel in one hour exposure time down to: • V=26.2 (21.5 – 11.1) for a O3 V (A0 V - G0 V) star in the band F150W • V=24.6 (21.9 – 19.5) for a O3 V (A0 V - G0 V) star in the band F250W • V=26.3 (26.3 – 26.3) for a O3 V (A0 V - G0 V) star in the band F555W • Spectral resolution: • R=100 at =150 nm • R>100 at 250 nm • R=250 at =500 nm. • Polarimetric filters • High time resolution imaging • The possibility to obtain wide field (~ 5x5 arcmin2) images from Far-UV to visual wavelengths. • Partial overlap between spectral range covered by FUV and NUV and NUV and UVO, for relative calibration purposes. Visiting Committee @OACT

  22. Main parameters of the FCU Visiting Committee @OACT

  23. FCU Layout UVO Channel Calibration Unit FUV Channel NUV Channel Visiting Committee @OACT

  24. The FCU in the Instrument Comparment 3D view of Scientific Instrumentation Compartment of WSO–UV. The FCU Optical Bench Assembly is shown on top of the S/C Optical Bench. Visiting Committee @OACT

  25. Filters Visiting Committee @OACT

  26. FUV & NUV Detectors • MCP-based detector in sealed configuration • Format: 2kx2k (40mm) • Pixel Size 20 m • Read-out system: CCD • Photocathodes: • CsI (FUV) • CsTe (NUV) Visiting Committee @OACT

  27. e2v CCD231-84 UVO Detector • Format: 4kx4k (61mm) • Pixel size: 15 micron • Back illuminated Visiting Committee @OACT

  28. 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 Visiting Committee @OACT

  29. FCU vs. HST ACS & WFPC3 Visiting Committee @OACT

  30. FCU Performances Visiting Committee @OACT

  31. FUV channel niche science • The FUV channel (115-190 nm) is unique for the coupling of a large field of view (400x400 arcsec) and a resolution of 0.2 arcsec/px. For the sake of comparison, HST/SBC which is sensible in the 115-170 nm range, has a 34x31 arcsec2 FoV (0.03 arcsec/px). Most of the following projects will be an original contribution of the FCU FUV channel, and will become part of its legacy. • Large high angular resolutions FUV surveys • FUV counterpart of GOODs survey • Star formation in early type galaxy in high-z cluster galaxies • Survey of Virgo cluster galaxies (e.g. extension of the UV upturn phenomenon, calibration SBF, etc.) • Age of unresolved young stellar systems • Exotica in star clusters • Survey of LMC clusters • Survey of shells in Novae and CVs • Stellar magnetic activity and YSOs in SFR and OCs. Visiting Committee @OACT

  32. 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. Visiting Committee @OACT

  33. NUV channel niche science • Main properties of the NUV channel (150-280nm) is its moderately large FoV (60x60 arcsec), coupled with the optimally sampled PSF with 0.03 arcsec/px (diffraction limited), and its spectro-polarimetric facilities. Main science drivers for this channel are: • AGN black holes accretion, outflows, and jets • Contributors to the UV light in nearby galaxies • GRB and SNe light curves in UV (thanks also to the quick response of WSO-UV telescope to ToO objects) • UV bright emitters in nearby early type stars • Exospheres and aurorae in Solar System planets, satellites, comets • UV light curve of transits of extrasolar planets • Imaging polarimetry and spectropolarimetry of AGN jets, GRBs, SNe, stellar jets, PNe and AGB shells. Visiting Committee @OACT

  34. UVO channel niche science • The UVO channel (200-800 nm) is characterized by a large field of view (286x286 arcsec) - two times larger than HST/ACS/WFI and three times larger than HST/WFPC3/UVIS - coupled with a 0.07arcsc/pix spatial resolution, that is diffraction limited at 500nm. • Main science objectives for the UVO channel are: • Optical couterparts of FUV surveys • High accuracy photometry in UV-optical • High accuracy astrometry • Extension of HST legacy (variabilty, proper motions, etc.) Visiting Committee @OACT

  35. 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 Visiting Committee @OACT

  36. Visiting Committee @OACT

  37. Programmatics Visiting Committee @OACT

  38. Funds WSO-UV FCU Phase A/B1: 364 keuro (total) • Subcontracts: • Univ. Florence • INAF IASF MI • INAF IASF BO • Univ. Padova • Univ. Trieste • Thales Alenia Space Italia – MI • Galileo Avionica • Catania: 89 Keuro • 60 Keuro salaries (1 fellow, 1 researcher) • 29 Keuro • 70% travel (also for Science Team members not in other participating units) • 5% software • 14% computers • 10% publications Related funds: • NUVA (Network for UltraViolet Astrophysics), a working group inside OPTICON, funded by EU (FP6) to trace a roadmap for UV astronomy in Europe (organize meetings, study reports, etcs) Visiting Committee @OACT

  39. Future funds • We expect ASI will give two contracts: • Industrial • Science Insitutes • We estimate for the next 5 years to manage from 4 to 8 Meuro. It depends from choices on some component procurements, mainly: • UV detectors • CCD detectors • Optics • Mechanisms (pick-up mirros subsystem, filter wheels etc.) Visiting Committee @OACT

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