The World Space Observatory for UltraViolet Project WSO-UV

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• 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
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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 (R1500-2500) spectrograph
Focal Plane Instruments High resolution (R?60,000) UV spectrograph
Focal Plane Instruments Deep and diffraction limited UV optical imager
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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.

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COPERNICUSIUE ASTRON HST FUSE
GALEX
1970 1980 1990 2000 2010 2020

year
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WSO-UV collaboration
Country Main Contribution Funding Agencies /Institutions/Industries
Russia Telescope, FGS, Platform, Optical Bench, Launcher, Launch facilities, Ground Segment  FSA(Roscosmos) INASAN Lavochkin Ass.
China LSS (Long Slit Spectrograph), Ground Station CNSACAS(NAOC) NIAOT
Germany HIRDES (UVES VUVES Spectrographs) DLR Tuebingen University Kayser Threde
Italy FCU (Field Camera Unit) GS station ASI INAF Univ, of Florence Univ. of Padua Galileo Av. Thales-Alenia Space IT (MI)
Spain Ground Station (MOC, SOC) CDTI Ministerio de Industria UCM G.M.V. S.A. TCP Sistemas e Ingenieria
Ukraine Coating of optical T170-M elements National Space Agency of Ukraine Crimean 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)
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Telescope T-170
The WSO-UV telescope (T-170M) is under the
responsibility of Lavochkin Association (Russia).
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)
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.
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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.

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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.
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WSO-UV Payload
PMU frame

• 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)
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WSO-UV HIRDES

• High Resolution Double Echelle Spectrograph

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
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WSO-UV HIRDES
See poster by Werner et al.
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HIRDES effective area
Wavelength Range Resolwing Power COS Eff. Area
115-150 20.000 24.000 2.200 (gt4 times VUVES)
140-178 20.000 24.000 1.200 (gt3 times VUVES)
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Exposure time calculator

• http//astro.uni-tuebingen.de/groups/wso_uv/exptim
  e_calc.shtml

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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
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LSS Spectrograph
Parameter Requirements
Wavelength coverage FUV channel NUV channel 102190 nm (1 or 2 subchannels) 190320 nm
Width of slit 1? ? 82 ?m
Length of slit 75? ? 6.2 mm
Spectral resolution 15002500
Spatial resolution 0.51
Detectors MCPs
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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
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Main FCU parameters
Parameter Channel Channel Channel
  Far-UV Near-UV UV-Optical
Spectral Range 115-190 nm 150-280 nm 200-800 nm
Field of View 6.6x6.6 1x1 4.7x4.7
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.
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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 _at_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.

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FCU Layout
UVO Channel
Calibration Unit
FUV Channel
NUV Channel
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Filters
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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

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FCU Performances
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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_at_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.
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Simulations
The triple main sequence as obtained from
simulated UVO data.
The triple main sequence of NGC 2808 GC as
observed by the ACS_at_HST camera
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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?

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WSO-UV Key Science Drivers

arXiv0712.0970v1

• 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?

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WSO-UV Ground Segment

WSO/UV
Ground station
Ground station
Ground station
Co-located
Operation archive
Control center
Control center
Control center

• Ground stations under consideration are located
  at
• Argentina
• Canaria islands (Spain)
• Italy
• P.R. of China
• Russia
• South Africa
• - confirmed

MOC
Mission archive
SOC
Science center
Science center
Science center
Science archive
Users
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Status of the WSO-UV International Collaboration
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Agreements
SMP
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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

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Science Verification Working Team

• is appointed by the WSC
• Eligibility it shall be formed by a number (TBD)
  of experts including
• Project scientists,
• Instrument PIs and collaborators,
• Telescope and ground science operation
  scientists.
• Duties
• It will manage the Commissioning phase and the
  Calibration and Performance Science Verification
  Phase (CSVP)
• Duration
• tbd

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Time Allocation Committee

• The Time Allocation Committee (TAC) is appointed
  by the WSSC.
• Eligibility
• scientists of internationally recognized level
• members of the WSO team.
• Duties
• It will select the OP and the CP.
• Duration
• The TAC have to be renovated every two years.

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National Time Allocation Committees

• National Time Allocation Committees (NTAC) set up
  by FBs at national level
• Duties
• Produce the FBs observing programs before the TAC
  meets to evaluate the proposals for OP
• Eligibility, and duration are regulated by the
  FBs.

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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

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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?