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

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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

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)

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

Filters

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

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

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

Status of the WSO-UV International Collaboration

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