spica fpc-s
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SPICA FPC-S
Myungshin Im(Seoul National University)
Sun
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Earth
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SPICA Mission Overview• Telescope: 3.2m (EPD 3.0m), 6
K– Superior Sensitivity– Good spatial resolution
• Core wavelength: 5-210 μm– MIR Instrument– Far-Infrared Instrument (SA-
FARI)• Orbit: Sun-Earth L2 Halo• Mission Life
– 3 years (nominal)– 5 years (goal)
• Weight: 3.7 t• Launch: 2022• International mission
– Japan, Europe, Korea, Taiwan, USA(From presentation by T. Nakagawa)
How did the Universe origi-nate and what is it made of ?
What are the conditions for stellar and planetary forma-tion and emergence of life?
Where are we from ?
Are we alone ?
Scientific Goals
(From presentation by T. Nakagawa)
Scientific Motivation• How did the Universe originate and
what is it made of ?
Big Bang 1st generation of stars
→ Hidden Universe to be revealed by FIR Observations
(From presentation by T. Nakagawa)
Infrared Space TelescopesIRAS, ISO: earlier missions
Spitzer (0.83m): Cold but smallAKARI (0.67m): Cold but smallWISE (0.5m, 3-24 micron): Cold but smallHerschel (3m, 200-500 micron): Large, but warm
SPICA (3m): Cooled, large aperture telescope with 2-200 micron
Cold (high sensitivity) yes Large aperture (high sensitivity, resolution) yes Large wavelength coverage yes
Requirements
• High spatial resolution→ 3m-class telescope
• High sensitivity→ T<10K
(From presentation by T. Nakagawa)
SPICA Focal Plane Instru-ments
• SAFARI– Far-infrared imaging spectrometer– P.I. SRON (Netherlands) with SAFARI Consortium
• MCS – Mid-infrared camera & spectrometer– P.I. JAXA, Universities, and ASIAA (Taiwan)
• SCI – SPICA coronagraphic instrument– P.I. JAXA with Nagoya Univ.
• FPC (FPC-G + FPC-S)– Near-infrared camera and spectrometer– P.I. KASI (Korea)
• US Instrument (e.g. BLISS)– Far-infrared, sub-mm spectrometer– P.I. TBD (NASA funded)
Focal Plane InstrumentsWavelength coverage vs Resolving Power
λ
l/dl (dv)
2 mm
20 mm 200 mm
100(3000 km s-
1)
1000(300 km s-1)
10000(30 km s-1)
Herschel
JWST
SPICA
FPC-S
MCS/HRS
SCI SAFARIMCS/WFC/LRS
MCS/MRS
Wavelength
US Inst
Unique Capability of SPICA/FPIs(From presentation by T. Nakagawa)
SPICA Focal Plane
(From presentation by T. Nakagawa)
10 arcmin
250 µm
350 µm
500 µm
GOODS-N: 250/350/500 mm
What are they ?Spectroscopy
Huge Gain of Sensitiv-ity
FPC-S• Back-up of FPC-G
• 5 x 5 arcmin2 (3x fov of JWST)• Pixel: 0.3” (~PSF FWHM, comparable to Euclid)
• 0.7-5 μm (R=5 imaging, R=20 spectroscopy)
• 5 wide-band filters + 3 LVFs
• ~26.3 AB mag at 100 sec, 3-σ, imaging ~27.7 AB mag at 1 hr, 5-σ, or ~25 AB mag at 20 sec 5-σ
• 26.3 AB mag at 3- , 600 sec LVFs
Linear Variable Filter (LVF)
Y-axis
Detector
X-axis
IncomingLight
OutgoingLight
LVF
Wavelength
Transmittance
Wavelength transmittance along y-axis is variable ~ many narrow-band filters
Key Science Topics (Extragalac-tic)
Galaxy formation/evolution:mass/SFR/environment(z=1-6)
First SMBHs (Quasars),& First galaxies (z > 6):50 deg^2 at 24 AB
Proto-clusters & cluster of galaxies(z=1-4): 1-100 /deg^2
Time
Cosmic NIR Background• Deep Imaging with LVF will identify CNIRB
(shape, and the power-spectrum) First stars!
Matsumoto et al. (2010)
Cosmic Star Formation History
Elbaz et al. (2007) Shim, Im, et al. (2007)
MIR/FIR Star formationNIR Mass, age, stellar population properties
Why FPC-S? Mass+Age+SFR of Dis-tant Galaxies
Optical
NIR
Mass: Optical/NIR
Age: Dn(4000)
SFR: UV
(Shim et al. 2007)
SFR(FIR) + SFR(MIR) + Mass/Age(FPC-S)
MCS FPC-SSAFARI
SFR(FIR) + SFR(MIR) + Mass/Age(FPC-S)
MCS FPC-SSAFARI
10-2
10-3
10-4
10-5
10-6
10-7
10-8
Flux
den
sity
(μJy
)
4 x 1010 L⊙
Lyman Break Galaxies LBGs will be identified in deep field or
in parallel field to study star forma-tion at high redshift
Parallel Observations• Parallel observations with MCS/
SCI are possible (multiple depth, area coverage)
Previous Surveys• Spitzer – GOODS (260 arcmin2, 25 AB mag),
SWIRE (50 deg2, 22 AB mag), COSMOS (2 deg2, 24 AB mag), SEDS (0.9 deg2, 25-26 AB mag)
• AKARI – NEP (5 deg2)
• Herschel – ATLAS (550 deg2@600hrs), HERMES (0.04-100 deg2@900hrs )
• JWST - ?• SPICA - ?
Possible Surveys• Deep survey: 1-2 deg2 (cf. COSMOS), deeper sur-
vey
• Wide survey: ~ 50 deg2 (cf. SWIRE/HERMES) – AGN/Galaxy clusters
• Shallow, wide survey: a few 100 deg2 (ATLAS/HERMES)
• Pure parallel survey (HST)
• 1 deg2 = ~150 FPC-S pointings ~27.7 AB mag at 1 hr, 5-σ, or ~25 AB mag at 20 sec 5-σ
Wide survey (~50 deg2)• T = 50 deg2 x 150 ptng/deg2 x 100 sec
x 5 filters = 1000 hrs • 5-σ at 25.7 AB mag
• Good for proto-cluster/cluster study, galaxy evolution in clusters, high-z quasars (10-50), ~100 bright LBGs at z > 7
Shallow survey (~400 deg2)• Parallel with MCS
• T = 400 deg2 x 150 ptng/deg2 x 20 sec x 3 filters = 1000 hrs
• 5-σ at 25 AB mag
• 20-100 QSOs at 7.5 < z < 8.5, 4-40 QSOs at 8.5 < z < 9.5 • At z = 3, > 2.5 x 109 M⊙, > 1010 L ⊙• > 400 clusters/proto-clusters, low-z, SDSS-type science, photo-z
Willott et al. (2009)
Very wide survey (~10,000 deg2)
• Post-Cryogen, KLM
• T = 10000 deg2 x 150 ptng/deg2 x 15 sec x 3 filters x 2.0 (overhead) = 4.3 yrs
• 5-σ at 24.7 AB mag
• 500-2500 QSOs at 7.5 < z < 8.5, 100-1000 QSOs at 8.5 < z < 9.5
• At z = 3, > 1 x 109 M⊙, > 0.7 x 1010 L ⊙
• > 10000 clusters/proto-clusters, low-z, SDSS-type science
SPICAV.
Wide
GRB 100905A• BAT alert at 2010, Sept.
5
• UKIRT follow-up, 15min after the burst (z,J,H,K)
NIR afterglow (z-drop)
BAT light curve (Marshall et al. 2010, GCN Report 299.1)
(Im et al. 2010, GCN Circ.11222)
z J
KH
SED Analysis: z = 6.7 – 8.3
Spectral break at ~ 1 micron
Easy observation for SPICA/FPC-S!
Summary• FPC-S is the Korean scientific instrument for
SPICA
• MCS (MIR) + SAFARI (FIR) + FPC-S (Optical/NIR)
mass, age, SFR of distant galaxies! (1-400 deg2), discovery of rare objects, first stars
• Post-cryogenic mission Synergy with Euclid: 10,000 deg2 survey
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