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SPICA FPC-S

SPICA FPC-S. Myungshin Im (Seoul National University). 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 (SAFARI) Orbit: Sun-Earth L2 Halo Mission Life

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SPICA FPC-S

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  1. SPICA FPC-S MyungshinIm (Seoul National University)

  2. 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 (SAFARI) • 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)

  3. Ｓｃｉｅｎｔｉｆｉｃ Goals Where are we from ? How did the Universe originate and what is it made of ? Are we alone ? What are the conditions for stellar and planetary formation and emergence of life? (From presentation by T. Nakagawa)

  4. 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)

  5. Infrared Space Telescopes IRAS, ISO: earlier missions Spitzer (0.83m): Cold but small AKARI (0.67m): Cold but small WISE (0.5m, 3-24 micron): Cold but small Herschel (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

  6. Requirements • High spatial resolution → 3m-class telescope • High sensitivity • → T<10K (From presentation by T. Nakagawa)

  7. SPICA Focal Plane Instruments • 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)

  8. Focal Plane InstrumentsWavelength coverage vs Resolving Power Herschel l/dl (dv) MCS/HRS SPICA 10000(30 km s-1) JWST MCS/MRS 1000(300 km s-1) US Inst λ SCI SAFARI 100(3000 km s-1) FPC-S MCS/WFC/LRS 2 mm 20 mm 200 mm Wavelength Unique Capability of SPICA/FPIs (From presentation by T. Nakagawa)

  9. SPICA Focal Plane (From presentation by T. Nakagawa)

  10. GOODS-N: 250/350/500 mm 10 arcmin 250 µm What are they ? 350 µm Spectroscopy 500 µm

  11. Huge Gain of Sensitivity

  12. 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

  13. Linear Variable Filter (LVF) Incoming Light Outgoing Light Detector Y-axis LVF Transmittance X-axis Wavelength transmittance along y-axis is variable ~ many narrow-band filters Wavelength

  14. Key Science Topics (Extragalactic) Time Galaxy formation/evolution: mass/SFR/environment (z=1-6) Proto-clusters & cluster of galaxies (z=1-4): 1-100 /deg^2 First SMBHs (Quasars), & First galaxies (z > 6): 50 deg^2 at 24 AB

  15. Cosmic NIR Background • Deep Imaging with LVF will identify CNIRB (shape, and the power-spectrum)  First stars! Matsumoto et al. (2010)

  16. Cosmic Star Formation History Elbaz et al. (2007) Shim, Im, et al. (2007) MIR/FIR  Star formation NIR  Mass, age, stellar population properties

  17. Why FPC-S? Mass+Age+SFR of Distant Galaxies Mass: Optical/NIR Age: Dn(4000) SFR: UV NIR Optical (Shim et al. 2007)

  18. SFR(FIR) + SFR(MIR) + Mass/Age(FPC-S) SAFARI MCS FPC-S

  19. SFR(FIR) + SFR(MIR) + Mass/Age(FPC-S) 4 x 1010 L⊙ 10-2 10-3 10-4 10-5 10-6 10-7 10-8 Flux density (μJy) SAFARI MCS FPC-S

  20. Lyman Break Galaxies LBGs will be identified in deep field or in parallel field to study star formation at high redshift

  21. Parallel Observations • Parallel observations with MCS/SCI are possible (multiple depth, area coverage)

  22. 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 - ?

  23. Possible Surveys • Deep survey: 1-2 deg2(cf. COSMOS), deeper survey • 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

  24. 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

  25. 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)

  26. 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 SPICA V. Wide

  27. GRB 100905A • BAT alert at 2010, Sept. 5 • UKIRT follow-up, 15min after the burst (z,J,H,K)  NIR afterglow (z-drop) z J H K (Im et al. 2010, GCN Circ.11222) BAT light curve (Marshall et al. 2010, GCN Report 299.1)

  28. SED Analysis: z = 6.7 – 8.3 Easy observation for SPICA/FPC-S! Spectral break at ~ 1 micron

  29. 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 deg2survey

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