Italian Part i cipation in the World Space Observatory / Ultraviolet Project

Dr. Isabella PaganoINAF - Osservatorio Astrofisico di CataniaPI of the WSO/UV Field Camera Unit (FCU)WSO/UV Implementation Committee member WSO/UV Italian web site:

http://www.oact.inaf.it/wso/index.htm/

Italian Participation in the World Space Observatory / Ultraviolet Project

The Field Camera Unit for WSO-UV



http://www.mi.iasf.cnr.it/index.php

Catania, 17 Dec 2007 Visiting Committee @OACT

WSO-UV @ INAF OACT

• INAF OA Catania is the leading institute for the contract ASI/INAF No. I/085/06/0:

Italian Participation in the World Space Observatory / Ultraviolet Project

• Involvement in the international team of WSO-UV since the beginning of the effort to involve national agencies

• Proposal submitted to ASI in Nov 2003 – approval Nov 2005 (Italian PASN) – contract Dec 2006.

• KOM on Jan 18 2007• Phase A review on Jul 12 2007• Phase B1 review on Dec 20 2007



INAF

Catania Obs., Napoli Obs., Padova Obs., Milano

IASF, Bologna IASF & Obs., Torino Obs., Trieste Obs.,

Cagliari Obs., Teramo Obs., Roma IASF.

Universities

DASS Firenze, Dip. Astr. Padova, Dip. Astr. Univ.

Bologna, Univ. Pisa

Industrial support

Galileo Avionica, Thales Alenia Space Italy (MI)

WSO-UV in Italy

About 20 FTE involved in WSO-UV during 2007.



People involved @ INAF-OACT

Researchers• Isabella Pagano (Principal Investigator, Project Manager) – 80% time• Salvatore Scuderi (System Engineer, Responsible for the UVO channel) - 80%

time• Cristian Pontoni (Responsible for the Thermal-mechanical design) – full time• Matteo Munari (Optical design team) – full time• Giovanni Bonanno (Advisor) – 5% time• Massimo Turatto (Science Team) – from 2008• In the past:

– Marcello Rodonò

Technicians• Saro Di Benedetto (Detectors) – 15% time• Vincenzo Greco (Electronics) – 5% timeAdministration• Daniela Recupero (Project assistant) – 10% time• In the past:

– Giuseppe Caripoli (Project assistant) – 10% time (May 2006-Feb 2007)



WSO-UV General Information

Objective: Provide spectroscopy and imaging access to the UV (110 - 300 nm) sky.

Launch date: 2012

Duration: 5 years (+5years)

Orbit: Circular/geosyncrhronous - 35860 Km - 1day period - 51.8° orbit inclination

Launcher: Zenith + Fregat


WSO-UV CollaborationCountry Main

ContributionFunding Agencies/Institutions/Industries

Status

Russia Telescope, FGS, Platform, Optical Bench, Launcher, Launch facilities, Ground Segment

FSA(Roscosmos)INASANLavochkin Ass.

Approved in the National Space Plan

China LSS (Long Slit Spectrograph), Ground Station

CNSA

CAS(NAOC) & NIAOT Approved in the National Space Plan. Agreement under negotiation

Germany HIRDES (UVES & VUVES Spectrographs)

DLRTuebingen UniversityKayser Threde

Funds in standby, completed Phase B1, waiting other payload at same level.

Italy FCU (Field Camera Unit) & GS station

ASIINAF & Univ, of Florence & Univ. of PaduaGalileo Av. & Thales-Alenia Space IT (MI)

Approved in the National Space Plan. Agreement under negotiation

Spain Ground Station (MOC, SOC)

CDTI – Ministerio de IndustriaUCMG.M.V. S.A. & TCP Sistemas e Ingenieria

Agreement signed

Ukraine Coating of optical T170-M elements

National Space Agency of UkraineCrimean Astrophysical Observatory

Approved

South Africa, Argentina

Tracking stations

UK, France

Participation in LSS University of Leicester (UK)LAM (FR)



BAFFLES

Optical System Ritchey-Chretien aplanat

Aperture diameter 1700 mm

Telescope f-number 10.0

FOV 30’ (150 mm in diameter)

Wavelength range 100-310 nm (+visible)

Primary Wavelength 200 nm

Optical quality Diffraction optics at the FOV 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 a

new version of the T-170 telescope

designed in Russia by Lavochkin

Association for Spectrum-UV mission.

Telescope T-170



The Navigator platform

• The WSO-UV bus is the “Navigator” service module used for other Russian projects: e.g. “Electro”, and “Radioastron”.

• 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.



WSO-UV Payload• HIRDES: R 60,000 echelle

spectrographs:• UVES (178-320nm)• VUVES (102-180nm)

• LSS: 102- 320 nm, R~1500–2500 long slit (1x75 arcsec) spectrograph

• FCU: 3-channel imaging cameras:• FUV • NUV• UVO

• FGS: Fine Guidance System (3 sensors 1kx1k)


The Italian participation to WSO-UV



Recommendation from the community



ASI Aero Space Plan 2006-2008

• Nov 2005: ASI release of the Italian National Aero-Space Plan (PASN) for 2006-2008

WSO/UV is inside the PASN



WSO-UV in the INAF LTP



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 (see later)

• Discretionary Director Time (DDT) up to a maximum of 2%

0

10

20

30

40

50

60

1styear

2nd &3th

year

Since4th

year

OP

CP

FBP

DDT


The Field Camera Unit Instrument



Activities performed during the

Phase A/B1• Define the key science objectives of the

imager

• Define the Top Level Requirements for the imager

• Produce the technical project of "Field

Camera Unit" (FCU)



The Instruments Compartment…. other views

Imagers

Spectrographs



Our goal• Top Science

• Build a compelling instrument and give the community tools:– to extend ambitious legacy program started

with HST.– to complement other contemporary facilities

in specific field: e.g. to perform astrometry with the same precision of GAIA in crowded fields where GAIA fails

– to allow for the first time high resolution FUV imaging with a wide field



Key Science Drivers• The Italian WSO-UV Science Team released a document at

the end of Phase A study (Jul 2007) where the Key Science Drivers for WSO-UV are discussed.

• Following the structure of the “A Science Vision for the European Astronomy” document prepared by the European ASTRONET consortium, the Italian WSO-UV Science Team shows how WSO-UV contributes to answer, in the next decade, the four key questions:– 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?



WSO-UV Imager criteria

• Large wavelength coverage (115-800nm)• Large field of view• High spatial resolution; this is mandatory to:

– Morphological studies (e.g. planets, planetary nebulae, star formation regions, external galaxies)

– High accuracy stellar photometry– High accuracy stellar astrometry– Resolve stars in crowded fields (e.g. in star

clusters, external galaxies, star formation in AGNs)



Science Requirements

• The requirements toward the imager instrument on board WSO-UV in order to fulfill its science objectives are:

• the possibility to obtain diffraction limited images for >230 nm (goal >200 nm).

• S/N=10 per pixel in one hour exposure time down to: – V=26.2 (21.5 – 11.1) for a O3 V (A0 V - G0 V) star in the band F150W – V=24.6 (21.9 – 19.5) for a O3 V (A0 V - G0 V) star in the band F250W – V=26.3 (26.3 – 26.3) for a O3 V (A0 V - G0 V) star in the band F555W

• Spectral resolution:– R=100 at =150 nm– R>100 at 250 nm– R=250 at =500 nm.

• Polarimetric filters• High time resolution imaging • The possibility to obtain wide field (~ 5x5 arcmin2) images from Far-UV

to visual wavelengths. • Partial overlap between spectral range covered by FUV and NUV and

NUV and UVO, for relative calibration purposes.

http://www.oact.inaf.it/wso/science.htm



Main parameters of the FCU

Parameter 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)



FCU Layout

Telescope Focal Plane

FCUFore-Optics

UVO

NUV

FUV

NUV Channel

FUV Channel

UVO Channel

Calibration Unit



The FCU in the Instrument Comparment

3D view of Scientific Instrumentation Compartment of WSO–UV.

The FCU Optical Bench Assembly is shown on top of the S/C Optical Bench.



Filters

FUV 1FUV 2

FUV 3FUV 4

FUV 5FUV 6

FUV 7FUV 8

FUV 9FUV 10

NUV 1NUV 2

NUV 3NUV 4

NUV 5NUV 6

NUV 7NUV 8NUV 9

NUV 10NUV 11

NUV 12NUV 13NUV 14

NUV 15NUV 16NUV 17

NUV 18NUV 19NUV 20

NUV 21NUV 22

NUV 23NUV 24NUV 25

NUV 26NUV 27

NUV 28NUV 29

UVO 1UVO 2

UVO 3UVO 4

UVO 5UVO 6

UVO 7UVO 8

UVO 9UVO 10

UVO 11UVO 12

UVO 13UVO 14

UVO 15UVO 16

UVO 17UVO 18

UVO 19UVO 20

1100 2100 3100 4100 5100 6100 7100 8100



FUV & NUV Detectors

• MCP-based detector in sealed configuration

• Format: 2kx2k (40mm)

• Pixel Size 20 m• Read-out system: CCD • Photocathodes:

– CsI (FUV)– CsTe (NUV)



UVO Detector• Format: 4kx4k (61mm)• Pixel size: 15 micron• Back illuminated e2v CCD231-84

QE: -100°C e2v Typical QE Astronomy Process with UV coating

0%

10%

20%

30%

40%

50%

60%

70%

80%

90%

100%

200 300 400 500 600 700 800 900 1000

Wavelength (nm)

QE



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



FCU vs. HST ACS & WFPC3 WSO-UV HST

FCU-FUV ACS-SBC

Range 115-190 nm 115-170 nm

FoV 6.6'x6.6' 31"x35"

Scale 0.2"/pix 0.032"/pix

FCU-NUV ACS-HRC

Range 150-280 nm 200-1100 nm

FoV 1'x1' 26"x29"

Scale 0.03"/pix 0.027"/pix

FCU-UVO ACS-WFC WFPC3-UVIS

Range 200-800 nm 370-1100 nm 200-1000 nm

FoV 4.7'x4.7' 3.4'x3.4' 2.7'x2.7'

Scale 0.07"/pix 0.05"/pix 0.04"/pix



FCU Performances



FUV channel niche science

• The FUV channel (115-190 nm) is unique for the coupling of a large field of view (400x400 arcsec) and a resolution of 0.2 arcsec/px. For the sake of comparison, HST/SBC which is sensible in the 115-170 nm range, has a 34x31 arcsec2 FoV (0.03 arcsec/px). Most of the following projects will be an original contribution of the FCU FUV channel, and will become part of its legacy.– Large high angular resolutions FUV surveys– FUV counterpart of GOODs survey– Star formation in early type galaxy in high-z cluster galaxies– Survey of Virgo cluster galaxies (e.g. extension of the UV

upturn phenomenon, calibration SBF, etc.)– Age of unresolved young stellar systems– Exotica in star clusters– Survey of LMC clusters– Survey of shells in Novae and CVs– Stellar magnetic activity and YSOs in SFR and OCs.



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



NUV channel niche science

• Main properties of the NUV channel (150-280nm) is its moderately large FoV (60x60 arcsec), coupled with the optimally sampled PSF with 0.03 arcsec/px (diffraction limited), and its spectro-polarimetric facilities. Main science drivers for this channel are:

– AGN black holes accretion, outflows, and jets – Contributors to the UV light in nearby galaxies – GRB and SNe light curves in UV (thanks also to the

quick response of WSO-UV telescope to ToO objects)– UV bright emitters in nearby early type stars– Exospheres and aurorae in Solar System planets, satellites,

comets– UV light curve of transits of extrasolar planets– Imaging polarimetry and spectropolarimetry of AGN

jets, GRBs, SNe, stellar jets, PNe and AGB shells.



UVO channel niche science

• The UVO channel (200-800 nm) is characterized by a large field of view (286x286 arcsec) - two times larger than HST/ACS/WFI and three times larger than HST/WFPC3/UVIS - coupled with a 0.07arcsc/pix spatial resolution, that is diffraction limited at 500nm.

• Main science objectives for the UVO channel are:– Optical couterparts of FUV surveys– High accuracy photometry in UV-optical – High accuracy astrometry – Extension of HST legacy (variabilty, proper motions, etc.)



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.





Programmatics



FundsWSO-UV FCU Phase A/B1: 364 keuro (total)• Subcontracts:

– Univ. Florence– INAF IASF MI– INAF IASF BO– Univ. Padova– Univ. Trieste– Thales Alenia Space Italia – MI– Galileo Avionica

• Catania: 89 Keuro– 60 Keuro salaries (1 fellow, 1 researcher)– 29 Keuro

• 70% travel (also for Science Team members not in other participating units)• 5% software• 14% computers• 10% publications

Related funds:• NUVA (Network for UltraViolet Astrophysics), a working group inside OPTICON,

funded by EU (FP6) to trace a roadmap for UV astronomy in Europe (organize meetings, study reports, etcs)



Future funds

• We expect ASI will give two contracts:– Industrial– Science Insitutes

• We estimate for the next 5 years to manage from 4 to 8 Meuro. It depends from choices on some component procurements, mainly:

– UV detectors– CCD detectors– Optics– Mechanisms (pick-up mirros subsystem, filter

wheels etc.)


Documents

Italian Part i cipation in the World Space Observatory / Ultraviolet Project