SPICA FPC-S

Myungshin Im(Seoul National University)

Sun

L1 L2

L4

L5

Earth

L3

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