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Italian Participation in the
World Space Observatory / Ultraviolet Project
The Field Camera Unit for
WSO-UV
Dr. Isabella Pagano
INAF - Osservatorio Astrofisico di Catania
WSO/UV Italian web site:
http://www.oact.inaf.it/wso/index.htm/
PI of the WSO/UV Field Camera Unit (FCU)
WSO/UV Implementation Committee member
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
Catania, 17 Dec 2007
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WSO-UV in Italy
 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)
About 20 FTE involved in WSO-UV during 2007.
Catania, 17 Dec 2007
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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% time
Administration
• Daniela Recupero (Project assistant) – 10% time
• In the past:
– Giuseppe Caripoli (Project assistant) – 10% time (May 2006-Feb 2007)
Catania, 17 Dec 2007
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WSO-UV General Information
Objective:
Launch date:
Duration:
Orbit:
Launcher:
Catania, 17 Dec 2007
Provide spectroscopy and imaging
access to the UV (110 - 300 nm) sky.
2012
5 years (+5years)
Circular/geosyncrhronous - 35860 Km
- 1day period - 51.8° orbit inclination
Zenith + Fregat
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WSO-UV Collaboration
Country
Main Contribution
Funding
Status
Russia
Telescope, FGS,
Platform, Optical Bench,
Launcher, Launch
facilities, Ground
Segment
FSA(Roscosmos)
INASAN
Lavochkin Ass.
Approved in the National Space
Plan
China
LSS (Long Slit
Spectrograph), Ground
Station
CNSA
Approved in the National Space
Plan. Agreement under
negotiation
Germany
HIRDES (UVES & VUVES
Spectrographs)
DLR
Tuebingen University
Kayser Threde
Funds in standby, completed
Phase B1, waiting other payload
at same level.
Italy
FCU (Field Camera Unit)
& GS station
ASI
INAF & Univ, of Florence & Univ. of Padua
Galileo Av. & Thales-Alenia Space IT (MI)
Approved in the National Space
Plan. Agreement under
negotiation
Spain
Ground Station (MOC,
SOC)
CDTI – Ministerio de Industria
UCM
G.M.V. S.A. & TCP Sistemas e Ingenieria
Agreement signed
Ukraine
Coating of optical T170M elements
National Space Agency of Ukraine
Crimean Astrophysical Observatory
Approved
South Africa,
Argentina
Tracking stations
UK,
France
Participation in LSS
Agencies/Institutions/Industries
CAS(NAOC) & NIAOT
University of Leicester (UK)
LAM (FR)
Telescope T-170
BAFFLES
Catania, 17 Dec 2007
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.
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)
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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”.
• 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.
Catania, 17 Dec 2007
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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)
Catania, 17 Dec 2007
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The Italian participation to
WSO-UV
Recommendation from the
community
Catania, 17 Dec 2007
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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
Catania, 17 Dec 2007
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WSO-UV in the INAF LTP
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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 (see later)
•
Discretionary Director Time
(DDT) up to a maximum of 2%
Catania, 17 Dec 2007
60
50
40
OP
CP
FBP
DDT
30
20
10
0
1st
year
2nd & Since
4th
3th
year
year
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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)
Catania, 17 Dec 2007
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The Instruments Compartment
…. other views
Imagers
Catania, 17 Dec 2007
Spectrographs
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• Top Science
Our goal
• 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
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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?
Catania, 17 Dec 2007
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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)
Catania, 17 Dec 2007
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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.
Catania, 17 Dec 2007
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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)
Catania, 17 Dec 2007
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FCU Layout
UVO Channel
UVO
Calibration
Telescope
Unit
FCU
Fore-Optics
Focal Plane
NUV
FUV
FUV Channel
NUV Channel
Catania, 17 Dec 2007
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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.
Catania, 17 Dec 2007
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Filters
UVO 20
UVO 19
UVO 18
UVO 17
UVO 16
UVO 15
UVO 14
UVO 13
UVO 12
UVO 11
UVO 10
UVO 9
UVO 8
UVO 7
UVO 6
UVO 5
UVO 4
UVO 3
UVO 2
UVO 1
NUV 29
NUV 28
NUV 27
NUV 26
NUV 25
NUV 24
NUV 23
NUV 22
NUV 21
NUV 20
NUV 19
NUV 18
NUV 17
NUV 16
NUV 15
NUV 14
NUV 13
NUV 12
NUV 11
NUV 10
NUV 9
NUV 8
NUV 7
NUV 6
NUV 5
NUV 4
NUV 3
NUV 2
NUV 1
FUV 10
FUV 9
FUV 8
FUV 7
FUV 6
FUV 5
FUV 4
FUV 3
FUV 2
FUV 1
1100
2100
Catania, 17 Dec 2007
3100
4100
5100
6100
7100
8100
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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)
Catania, 17 Dec 2007
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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
100%
90%
80%
70%
QE
60%
50%
40%
30%
20%
10%
0%
200
300
400
500
600
700
800
900
1000
Wavelength (nm)
Catania, 17 Dec 2007
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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
Catania, 17 Dec 2007
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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
Catania, 17 Dec 2007
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FCU Performances
Catania, 17 Dec 2007
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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.
Catania, 17 Dec 2007
Visiting Committee @OACT
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@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.
Catania, 17 Dec 2007
Visiting Committee @OACT
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.
Catania, 17 Dec 2007
Visiting Committee @OACT
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.)
Catania, 17 Dec 2007
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Simulations
The triple main sequence of NGC
2808 GC as observed by the
ACS@HST camera
Catania, 17 Dec 2007
The triple main sequence as
obtained from simulated UVO data.
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Catania, 17 Dec 2007
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Programmatics
Catania, 17 Dec 2007
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Funds
WSO-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)
Catania, 17 Dec 2007
Visiting Committee @OACT
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:
–
–
–
–
Catania, 17 Dec 2007
UV detectors
CCD detectors
Optics
Mechanisms (pick-up mirros subsystem, filter wheels
etc.)
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