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 Project WSO-UV
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The World Space Observatory for UltraViolet Project WSO-UV
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
China LSS (Long Slit Spectrograph), Ground Station
CNSACAS(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 aplanatAperture 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.
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
WSO-UV HIRDES
See poster by Werner et al.
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)
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
Width of slit 1 82 mLength of slit 75 6.2 mmSpectral resolution 1500~2500Spatial 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)
• 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.
• 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
FCU Performances
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
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