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The World Space Observatory for UltraViolet Project WSO-UV. Isabella Pagano , Martin Barstow, Noah Brosch, Ana Ines G ó mez de Castro, Mahoai Huang, Norbert Kappelmann, Giampaolo Piotto, Salvatore Scuderi, Mikhail Sachkov, Boris Shustov, Klaus Werner, Gang Zhao. WSO-UV General Information. - PowerPoint PPT Presentation
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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
The World Space Observatory for
UltraViolet ProjectWSO-UV
Bologna, 31 Jan 2008 HST after SM4
WSO-UV General Information
Objective Provide spectroscopy and imaging access to the UV (102 nm)
Launch date 2012
Duration 5 years (+5years)
Payload
Telescope 1.7 m
Focal Plane Instruments
Low resolution (R~1500-2500) spectrograph
High resolution (R60,000) UV spectrograph
Deep and diffraction limited UV & optical imager
Bologna, 31 Jan 2008 HST after SM4
Why UV? Most resonance transitions from ions, atoms,
molecules of astrophysical significance are in the ultraviolet wavelength domain.
UV provides 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.
Bologna, 31 Jan 2008 HST after SM4
COPERNICUSIUE ASTRON
HST
FUSE GALEX
1970
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2020
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WSO-UV
SUVO ?
WSO-UV collaborationCountry Main Contribution Funding Agencies
/Institutions/Industries
Russia Telescope, FGS, Platform, Optical Bench, Launcher, Launch facilities, Ground Segment
FSA(Roscosmos)INASANLavochkin Ass.
China LSS (Long Slit Spectrograph), Ground Station
CNSA
CAS(NAOC) & NIAOT
Germany HIRDES (UVES & VUVES Spectrographs)
DLRTuebingen UniversityKayser Threde
Italy FCU (Field Camera Unit) & GS station
ASIINAF & Univ, of Florence & Univ. of PaduaGalileo Av. & Thales-Alenia Space IT (MI)
Spain Ground Station (MOC, SOC) CDTI – Ministerio de IndustriaUCMG.M.V. S.A. & TCP Sistemas e Ingenieria
Ukraine Coating of optical T170-M elements
National Space Agency of UkraineCrimean Astrophysical Observatory
Kazakhstan Money Bilateral agreement with Russia approved
South Africa, Argentina
Tracking stations
UK, France
Participation in LSS University of Leicester (UK)LAM (FR)
Optical System Ritchey-Chretien aplanat
Aperture diameter
170 cm
Telescope f-number
10.0
FOV 30’ (150 mm in diameter)
Wavelength range
100-310 nm (+visible)
Primary Wavelength
200 nm
Optical quality Diffraction limited in the center
Mass 1570 kg (1600 with adapter truss)
Size 5.67x2.30 m (transport)8.43x2.3 m (operational)
The WSO-UV telescope (T-170M) is under the responsibility of Lavochkin Association (Russia).
Telescope T-170
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.
Bologna, 31 Jan 2008 HST after SM4
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.
Bologna, 31 Jan 2008 HST after SM4
WSO-UV OrbitТрасса
1801701601501401301201101009080706050403020100-10-20-30-40-50-60-70-80-90-100-110-120-130-140-150-160-170
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• 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.
Bologna, 31 Jan 2008 HST after SM4
WSO-UV Payload FCU: 3-channel Imager:
FUV, NUV, UVO
FGS: Fine Guidance System (3 sensors 1kx1k)
HIRDES: high-res echelle spectrographs:
UVES (178-320nm)VUVES (102-180nm)
LSS: 102- 320 nm, low-res long slit spectrograph
Optical Bench (CeSiC)
PMU frame
Bologna, 31 Jan 2008 HST after SM4
WSO-UV HIRDES
• High Resolution Double Echelle Spectrograph
Funding Agency: DLRScience Contractor: Universität Tübingen, Institut für Astronomie und AstrophysikIndustry Contractor: Kayser ThredePrincipal 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
Bologna, 31 Jan 2008 HST after SM4
HIRDES effective area
WavelengthRange
Resolwing Power
COS Eff. Area
115-150 20.000 – 24.000 2.200 (>4 times VUVES)
140-178 20.000 – 24.000 1.200 (>3 times VUVES)
Bologna, 31 Jan 2008 HST after SM4
Exposure time calculator
http://astro.uni-tuebingen.de/groups/wso_uv/exptime_calc.shtml
Bologna, 31 Jan 2008 HST after SM4
WSO-UV LSS• Long Slit Spectrograph
Funding Agency: CNASScience 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
Bologna, 31 Jan 2008 HST after SM4
LSS Spectrograph
Parameter RequirementsWavelength coverage
• FUV channel• NUV channel
102~190 nm (1 or 2 subchannels)190~320 nm
Width of slit 1 82 m
Length of slit 75 6.2 mm
Spectral resolution 1500~2500
Spatial resolution 0.5”~1”
Detectors MCPs
Bologna, 31 Jan 2008 HST after SM4
WSO-UV FCU
• Field Camera Unit
Funding Agency: ASIScience 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
Bologna, 31 Jan 2008 HST after SM4
Main FCU parametersParameter Channel
Far-UV Near-UV UV-Optical
Spectral Range
115-190 nm 150-280 nm 200-800 nm
Field of View
6.6’x6.6’ 1’x1’ 4.7’x4.7’
Scale 0.2”/pix 0.06”/pix 0.07”/pix
Pixel Size 20 m 20 m 15 m
Array Size 2kx2k 2kx2k 4kx4k
Detector MCP (CsI) MCP (CsTe) CCD (UV optimized)
See poster by Scuderi et al.
Bologna, 31 Jan 2008 HST after SM4
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.
Bologna, 31 Jan 2008 HST after SM4
FCU Layout
Telescope Focal Plane
FCUFore-Optics
UVO
NUV
FUV
NUV Channel
FUV Channel
UVO Channel
Calibration Unit
Bologna, 31 Jan 2008 HST after SM4
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
Bologna, 31 Jan 2008 HST after SM4
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.
Hubble Deep Field UV countpart
Bologna, 31 Jan 2008 HST after SM4
Simulations
The triple main sequence of NGC 2808 GC as observed by the ACS@HST camera
The triple main sequence as obtained from simulated UVO data.
Bologna, 31 Jan 2008 HST after SM4
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?
Bologna, 31 Jan 2008 HST after SM4
WSO-UV Key Science
Drivers
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?
arXiv:0712.0970v1
Bologna, 31 Jan 2008 HST after SM4
Agreements
RussiaRoscosmos
INASANLavochkin
ChinaCNSACAStbd
UKLeicester Univ.
PhotekMCP - R&D
GermanyDLR
Univ. TuebingenKayser-Thrade
ItalyASI
INAFtbd
UKLeicester Univ.
PhotekMCP - R&D
SpainCDTICSICFilters
SpainCDTIUCMGMV
Ukraine
Crimean Obs.
SMP
Bologna, 31 Jan 2008 HST after SM4
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
Bologna, 31 Jan 2008 HST after SM4
Time Sharing PolicyThe 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%
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Thanks
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?
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
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