The WSO-UV mission

B. Shustov, A.I. G'omez de Castro and the WSO-UV team

2 UV missions and instruments (in the past and present)

name launch size of type of mode λλ year.month instrument pointing of angstrom cm observ. OAO-2 1968.12 - 1973.01 20 sp is 1000-4250 TD-1A 1972.03 - 1974.05 28 s is 1350-2800+ OAO-3 1972.08 - 1981.02 80 p s 900-3150 ANS 1974.08 - 1977.06 22 p s 1500-3300+ IUE 1978.01 - 1996.09 45 p s 1150-3200 ASTRON 1983.03 - 1989.06 80 p s 1100-3500+ EXOSAT X 1983.05 - 1986. 2x30 p is 250+ ROSAT X 1990.06 - 1999.02 84 sp i 60- 200+ HST 1990.04 240 p isp 1150-10000 EUVE 1992.06 - 2001.01 12 sp is 70- 760 ALEXIS X 1993.04 - 2005.04 35 s i 130- 186 MSX 1996.04 - 2003 50 s i 1100-9000+ FUSE 1999.06 - 2007.07 39х35 (4) p s 905-1195 XMM X 1999.12 30 p is 1700-5500 GALEX 2003.04 50 sp is 1350-2800 γ SWIFT ,X 2004.11 30 p i 1700-65003 ASTRON

An UV space observatory with 80 cm aperture telescope and scanning spectrometer onboard (1983-1989). Significant results: first detection of H2O in Halley comet, UV spectroscopy of SN1987a, Pb lines in stellar spectra etc. (Photo of flight model at Lavochkin Museum) 4 “Spektr” (Спектр) missions for astrophysics

Federal Space Program (2006-2015) includes as major projects:

Spektr-R (Radioastron) – launched in 2011

Spektr-RG – launch is planned for 2014

Spektr-UF (World Space Observatory – Ultraviolet) – launch 2016. International name is World Space Observatory – Ultraviolet (introduced by Willem Wamsteker)

5 WSO-UV Project

WSO-UV (World Space Observatory – Ultraviolet) project is an international space observatory designed for observations in the UV (115 - 320 nm) where some of the most important astrophysical processes can be efficiently studied with unprecedented capability. The observatory includes a 170 cm aperture telescope capable of high-resolution spectroscopy, long slit low- resolution spectroscopy, and deep UV and optical imaging. At present cooperation on the project includes Russia and Spain as major partners, Ukraine and Germany as minor ones.

6 WSO-UV mission model

Telescope: T-170M, ∅1.7 m , f/10 Russia

Spectrographs: WUVS, Russia

Imagers: ISSIS, Spain

Platform: Navigator, Russia

Orbit: geosynchronous, i=51.6o

Launcher, launch: “ZENIT 2SB”, end of 2016, Russia

Ground Segment: Russia and Spain 7 Cooperation in Russia

Lavochkin Association Primary contractor for the Project: + subcontractors The T-170M Telescope, Platform, Launch, Mission control center Institute of Astronomy, RAS Primary subcontractor: (INASAN) Science Instrumentation Ground Segment (SOC)

Lytkarino Optical Plant Manufacturing optics of the T-170M Physical Inst. RAS, UV-spectrographs (detectors, ITMO-State Optical Inst. optical elements, AIV) VNIIEF UV-spectrographs (mechanics) “Luch” Co. Coatings of optical elements Space Research Inst. On-board Sci. Instr. Control and Data RAS (IKI) Management System,

INASAN INASAN major subcontractors Fine Guidance System The WSO-UV S/C

9 The Navigator platform Life time > 5 years Spacecraft mass (wet) 2 900Kg Payload mass 1 600Kg The power consumption of P/L 750W Data transmission rate 4 Mbit s−1 Stabilization and pointing accuracy using the FGS (3σ) 0.1 arcsec

The platform was successfully in-flight tested during: 1. Electro (remote sensing mission) 2. Spektr-R 10 The T-170M telescope

Optical system Ritchey – Chrètien aplanat Aperture diameter 1700 mm Telescope f-number 10.0 Field angular diameter 0.50° (300mm diameter) Primary wavelength 200 nm Scale 81 mkm/arc sec. Mass 1570 kg Optical quality Diffraction optics at the center of FOV

11 T-170M Telescope Model at Lavochkin Association. 12 T-170M optics

Al+MgF2 coating deposition onto primary mirror in “Luch” (in Denton vacuum camera) 13 T-170M optics

reflectivity

Reflectivity is close to best Microroughness: reported rms 0.75 nm before coating,

1 nm – after coating 14 T170M instrument compartment

15 WUVS (WSO-UV Spectrograph)

Three channels (spectrographs) of the

WUVS :

Vacuum Ultraviolet Echele Spectrograph VUVES - 115-176 nm, R ≈ 50 000

Ultraviolet Echele Spectrograph UVES - 174-310 nm, R ≈ 50 000

Long Slit Spectrograph LSS - 115-310 nm, R=1000

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WUVS CCD detector enclosure concept (e2v)

Contract between e2v and Lebedev Physical Institute of the RAS is signed.

Drive electronic (RAL) 17 WUVS optical system prototype in laboratory (at SOI)

Echelle grating prototype 18 WUVS efficiency (factors)

19 WUVS efficiency (expected)

20 ISSIS (IMAGING AND SLITLESS SPECTROSCOPY INSTRUMENT FOR SURVEYS) Two channels for imaging and slitless spectroscopy: The Far Ultraviolet Channel (FUV), providing the optimum sensitivity in the 1150-1750 Å interval, and equipped with a CsI MCP detector The Near Ultraviolet Channel (NUV) covering wavelegnths in the 1850- 3200 Å range; the detector is a CsTe MCP.

ISSIS STM at SENER 21 Comparison of effective areas for ISSIS, GALEX and SBC in imaging mode.

22 WSO-UV Orbit

WSO-UV geosynchronous orbit, i=51.6o

23 WSO-UV Ground Segment

The GS includes :

The Mission Operation Center (two fully mirror distributed parts located in Spain and Russia) with co-located control centers and ground stations are parts of the Ground Control Segment.

The Science Operation Center (two fully mirror distributed parts located in Spain and Russia), which can be linked to various research centers. 24 Astrophysics in UV recent issues

2012

2011 next ESO/NUVA/IAG Workshop on Challenges in UV Astronomy, ESO Garching, 7-11 October 2013 25 WSO-UV Scientific Programs

Core Program (CP): The CP of scientific observations with the WSO-UV is defined to allow the conduction of high impact or legacy scientific projects that deserve large amounts of observing time. They are selected on the basis of their scientific excellence.

Open Program (OP): The Open Program consists of astronomical observations obtained with the WSO-UV by astronomers who may or may not belong to the WSO-UV international consortium.

Funding Bodies Program (FBP): The Funding Bodies (FBs) Program is the guaranteed time granted to each one of the national bodies funding the WSO-UV project.

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On the time sharing policy

During the first year: 45% for CP, 45% for FBP, 8% OT, 2% DDT (Director Discretionary Time) .

During the second and third years: 30% for CP, 40% for FBP, 28% OT, 2% DDT.

For the following years: 60% for FBP, 38% OT, 2% DDT.

27 The WSO-UV core program

I. The Cosmic Web (history of reionization, search for baryons).

II. Stellar physics - activity on stars (obs. support of mass transfer theory in CB, physics of WD etc.).

III. The early evolution of stars and role of UV in the evolution of the young planetary disks and astrochemistry in UV field.

IV. Atmospheres of (exo)planets.

28 28 Important!

We are grateful to all the scientists and technical experts from various countries who helped and help to implement the WSO-UV! We expect active international interest and scientific participation of the world astronomical community in the WSO-UV Project!

29 http://www.wso-uv.org