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1 SPICA ICRR ISAS,JAXA

2 List of my talk Bright Source Catalog Science Highlights Warm Mission SPICA 2

3 地球大気の透過率 & 放射強度 3

4 地球大気の吸収を逃れる地球大気の放射から逃れるなぜ宇宙へ? 4,000m 級の高山に上っても大気の赤外線放射は宇宙から来る赤外線の 100 万倍 1,000 万倍方向による変化時間変化ポアソン揺らぎによる雑音ただし暖かい望遠鏡では望遠鏡からの熱放鏡射が強い極低温冷却望遠鏡 4

5 あかり : 日本初の赤外線天文衛星 M-V cm (Ritchey-Chretien 952kg 5

6 AKARI Operation Phases Launch Checkout Phase 1 (~180 days) Phase 2 (~300 days) 2nd PV Feb. 22, 2006 Apr. 14, 2006 May 7, 2006 Nov. 10, 2006 Checkout & Performance Verification All-Sky Survey: 1st priority LS+Some MP Pointed Obs MP + OT Pointed Obs. Supplemental Survey LHe boil-off (Aug. 26, 2007) Phase 3 (>365 days) p only NIR in operation MP + OT pointed Obs.

7 Onboard dinstruments t Photometric & Spectroscopic Capabilities AKARI Survey IRAS Survey

8 : 65, 90, 140, 160 µm : 9, 18 µm 98 % (FIR) 96 % (MIR) 2 IRAS (40-70arcsec@FIR)

9 98 % Sky coverage (FIS) 98.3 % 52.0 % NScanMap (WIDE-S)

10 AKARI IRC/FIS catalogues AKARI IRC/FIS catalogues, 18 µm, 90 µm

11 AKARI IRC/FIS catalogues, 18 µm, 90 µm IRC (MIR) FIS (FIR) (µm) 918 9, 65, 90, 140, , , & 130 mjy , , , 75Jy % 20 ~ 30 % ~7 arcsec ~1 arcmin 1 3arcsec ~6 arcsec ( AKARI Catalogue )

13 Comparison with IRAS IRAS b 10 deg IRAS Flux [Jy] IRAS 60 µm (FQUAL=3) IRAS 100 µm (FQUAL=3) IRAS AKARI Rate (%) IRAS AKARI Rate (%) ~ ~ ~ ~ ~ IRAS F60 = Jy, F100=10~ % LMC, Orion, Ophcus IRAS

14 Scientific Highlights AGN search IR LF in local Universe 21

15 AKARI All-Sky Mid-IR Survey Search for AGNs - method 1200 sources 22

16 23

Discovery of new dusty Active Galactic Nuclei A galaxy with

No evidences of AGN before AKARI An optical spectrum shows HII

Red NIR/MIR color is confirmed with the NIR spectrum taken

17 Discovery of new dusty Active Galactic Nuclei A galaxy with Lir~ Lsun at a redshift z~0.04. No evidences of AGN before AKARI An optical spectrum shows HII galaxy features. 2MASS color is not as red as that of AGN. Red NIR/MIR color is confirmed with the NIR spectrum taken with AKARI in Phase3. PAH Kim et al Brα Red continuum /10/16 24

18 IRAS detections 2MASS M82 M82+500K dust AKARI Wavelength(micron) Indicating the exist of hot dust AGN, but a central engine is completely obscured. Surprisingly, we miss this kind of AGNs in nearby universe. We are interested in the number density and the contribution of these sources to the Hard X-ray background. 2009/10/16 25

19 Local IR LF from AKARI all sky survey Revised Bright Galaxy Sample(Sanders+03): a complete sample of 629 galaxies with spec-z at S 60 >5.24Jy IRAS is only up to 100μm, missing i the peak of dust emission. AKARI reaches 160μm, Better measurement of L TIR

20 SED fit IRASはここまで 160μm is critical! AKARI is the only satellite to provide 160μm to all sky.

21 L TIR AKARI can better resolve cirrus, nearby sources.

22 Local IR LF 1/V max method, no completeness correction Agrees well with IRAS ΩΩ = TIR x % by LIRG, 0.4% 04%b by ULIRG 23x10 7 L su

23 34

24 星形成が活発な銀河のスペクトル塵がなかったとしたらこのくらい明るい ( 星の光 ) 星の光はチリに吸収されて暗くなってしまうあたたかいチリからの赤外線

25 ,000 8,000 15,18 μm Lee et al

26 100 ULIRG 全天サーベイ Goto et al in press

27 MIR color images Subaru/BRz N2 N3 N4 S7 S9W S11 L15 L18W L24 AKARI/IRC N2, N3, N4 S7, S9W, S11 L15, L18W, L24 Takagi et al. 2009

28 PAH-selected galaxies (1) Selection: [11/7μm or 15/9μm flux ratio] > 8 Redder than AGN with the steepest power-law ( 15/9μm ratio= 3.6) AKARI s unique MIR-colors F(11)/F(7)

29 PAH-selected galaxies (2) z~1.2 12PAHl luminous Selection: [15/9μm flux ratio] > 8 F(15)/F(9)

30 MIR Total-IR relation Ultra Luminous starbursts! Abs. AGN Estimation of PAH 7.7μm peak luminosity from IRC photometry: IR luminosity is obtained from optical-mir SED fitting SED estimations of 1.4 GHz fluxes are correct in ~50% for radio-detected sources

31 Warm Mission i 43

32 AKARI Warm Mission Temperature Profile 44

33 Detector Dark Current & hot pixels 10% of the whole pixels 45

34 QSO Hα - - log / z>4.5 QSO Hα Im 2009, z< z Im 2009, 47

35 あかりからから SPICAへ How did the Universe originate and what is it made of? What are the conditions for stellar and planetary formation? How did the universe evolve chemically? The emergence of life?

36 Credit: NASA One of the Science Goals: How did the Universe originate and what is it made of? SPICA Birth of 1st Stars Cosmic Re- ionization

37 Cool Mission! 50

38 Revolution of Design Philosophy Cryocoolers No Cryogen Large Telescope ISO: 2.6t for 60cm SPICA 3.7t for 3.2m

SPICA Overview COOLED (<6K) Space telescope 3-m

$diffraction limited at 5μm Space Observatory$ 5-210μm) JAXA ESA(Cosmic Vision M-class

from Korea & US Orbit: Sun-Earth L2 Halo

39 SPICA Overview COOLED (<6K) Space telescope 3-m mclassmonolithic monolithic primary mirror diffraction limited at 5μm Space Observatory mission, for mid- & far- IR astronomy (core 5-210μm) JAXA ESA(Cosmic Vision M-class candidate) Mission, with planned participation from Korea & US Orbit: Sun-Earth L2 Halo Mission Life: 3 years (nominal) 5 years (goal) Launch: FY2018 (H-IIA)

40 Overview of SPICA Weight: 3.7t Launching Vehicle: H-IIA (5S fairing) 11Mbps downlink in X-band TT&C in S-band

41 Heritage of Mechanical Cryocoolers AKARI 2-stage Stirling 20 K Long-life test > 5yrs 2006 SMILES JT 30mW@ 4.5 K 2009 SUZAKU ADR, 60mk reached 2005 Cryocooler technology is strategic techniquie for space science in Japan Future Missions: Kaguya, Planet-C, ASTRO-G, ASTRO- H, SPICA

42 Monolithic mirror 3m-class is technically a good choice Monolithic Mirror Ceramic material (SiC) No deployable mechanism Simple, Feasible, Reliable Smooth PSF Essential for Coronagraph Herschel & AKARI Heritage SPICA: WFE 0.35μm, 5K (3.5m) AKARI: WFE 0.35μm, 6K (70cm) Herschel: WFE 6μm, 80K (3.5m)

43 Focal Plane Instruments λ/δλ (δv) MIRHES Herschel (30 km s -1 ) SPICA JWST 1000 MIRMES (300 km s -1 ) BLISS 100 (3000 km s -1 ) FPC-S SCI SAFARI MIRACLE 2 μm 20 μm 200 μm λ Optional

44 SAFARI SPICA Far-infrared Instrument Leaded by SAFARI consortium in Europe Imaging Fourier-transform spectrometer covering μm FOV : 2 x 2 arcmin 2 Wavelength resolution 2000 at 100 μm is maximum

45 Flux Limit in 5σ (Jy) for imaging / photometry SAFARI Imaging Spectroscopy R~ , 1hr MIRACLE Imaging, 1hr JWST /MIRI Confusion limit!! (3m aperture) SAFARI Broad-band Imaging In only 10 min (!) 60

46 Sensitivity for spectral lines (1 hour, 5σ) IRSx0.1 BLISS (optional)

47 バリオン物質が描きだす宇宙構造の形成と進化宇宙初期物質輪廻の進化銀河誕生のドラマ? 惑星系のレシピ? 塵 ( ダスト ) ガス現在の宇宙従来の 100 倍の感度向上あかりの成果を基に日本が主導で塵 ( ダスト ) ガス独創的なSPICAの貢献が期待される

48 従来の 100 倍以上の感度向上で太古の宇宙の物質診断に挑む 63

49 Summary Faint Source Catalog Warm Mission JWST microns) o SPICA Warn Launch,

Wish list for US participation by SDR

Wish list for US participation by SDR 次世代赤外線天文衛星 SPICA の概要 2011 年 1 月 6 日中川貴雄 (JAXA) SPICA team 企画セッション :SPICA の挑戦概要次世代赤外線天文衛星 SPICA の概要 ( 中川 JAXA ) SPICA 観測装置 ( 片坐 JAXA ) 科学目的 SPICA の目指すもの ( 松原 JAXA ) SPICA で探る太陽系科学 ( 渡部天文台 ) SPICA による系外惑星研究