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Next Generation Space Infrared Telescope S PICA

Next Generation Space Infrared Telescope S PICA. Mini-Workshop @ Niigata Univ. “ Formation of the First Generation of Galaxies: Strategy for the Observational Corroboration of Physical Scenarios ” Hideo Matsuhara & SPICA WG The Institute of Space and Astronautical Science.

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Next Generation Space Infrared Telescope S PICA

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  1. Next Generation Space Infrared TelescopeSPICA Mini-Workshop @ Niigata Univ. “Formation of the First Generation of Galaxies: Strategy for the Observational Corroboration of Physical Scenarios” Hideo Matsuhara & SPICA WG The Institute of Space and Astronautical Science

  2. Overview of SPICAand Current Status

  3. Outline of SPICA • Telescope: 3.5m, 4.5 K • JWST(20-40K), HSO(80K) • Core λ: 5-200 μm • Complementary to JWST (Opt-NIR), HSO (Sub-mm) • Orbit: Sun-Earth L2 Halo • Warm Launch, Cooling on Orbit • Total Weight: 2.6 t • Launch: ～2010 by HIIA

  4. Baffle Shield #1 Telescope Tube Shield #2 Stressed Shield #3 Ge:Ga Mirror FPI Sun Shield Sun Shield MLI Conduction Radiation 20K Pre-cooler Bus Module 1.7 K Stage Cooler Bus MLI 4.5K Stage Cooler 冷却方法: 効率的な放射冷却＋機械式冷凍機

  5. HIIAで打上げられる最大口径を

  6. SPICA 技術検討、開発 • 予算 • 戦略的開発研究 • 科学技術振興調整費「次世代スペース・オプティクスの広域展開」 • 科研費 • 検討、開発項目 • ミッション系基礎技術開発 • 機械式冷凍機 • 軽量望遠鏡システム • 焦点面観測装置（検出器） • システム検討 • 熱・構造の最適化 • ハイブリッド姿勢制御システム

  7. SPICA計画・ロードマップ • 基礎技術開発 (2004年度まで) • システム全体の成立性の検討 • Critical Components の開発終了 • プロポーザル提出 (2004年度) • 基礎開発の成果、ASTRO-Fの成果 • PM (2005-7年度） • FM (2008-2010年度) • 打ち上げ (2010年度)

  8. Detection Limits of SPICA - Assumption & Procedure -

  9. Detection Limit of SPICA -Assumptions • Telescope : D=3.5m, cooled to 5K. Emissivity 5% • Pixel field-of-view: 0.1"(λ/2.5 micron)*(3.5m/D) • PSF: “pill-box” with diffraction limited diameter • 1.6(λ/D)=0.236“(λ/2.5 micron)*(3.5m/D) • Wavelength Band-width: l/Dl = 5, l/Dl= 3000 for spectroscopy • Detectors / Optical throughputs:

  10. IR Sky observed with COBE/DIRBE Zodiacal Light Interstellar dust emission Kelsall et al. (1998) ApJ 508, 44 Arendt et al. (1998) ApJ 508, 74

  11. SED of Natural Background Emission Old assumption, please forget this..

  12. Detection Capability of SPICA- Broad-band Imaging -

  13. SPICA Point Source Sensitivity1 hour, 5sigma3rd March, 2003 revision

  14. Comparision with Other Missions sorry, a bit old…

  15. ~3mJy Submm Galaxies & SPICA sensitivity(1hour, 5s)

  16. A possible Scenario of massive Elliptical Formation & Evolution Major Merger Galactic Wind Passive Evolution Phase Building Blocks (clumps) Dusty ULIRG Phase !!

  17. SED of Young Ellipticals Young Ellipticals @ Galactic wind z=2.7 HEROs @z=2.3 Totani et al. (2001)

  18. Limiting Mass(magnitudes) of ASTRO-F 70cm telescope • SPICA flux limit is ~20 times deeper than ASTRO-F at 10 micron • JWST + SPICA can reach down below 1010M◎out to z~10! Courtesy to T. Kodama/NAOJ

  19. Unfortunately in the FIR, SPICA’s beam is similar to that of SCUBA(15m,850μm) = (3.5m, 200μm) radio ROSAT SCUBA 8mJy Survey Fox et al. (2002) MNRAS 331, 839

  20. Uniqueness of SPICA (Broad-band Imaging) • JWST is more sensitive @ l < 5mm • Strongly confusion limited by faint galaxies @ l > 200mm • Hence core wavelength must be 5~200mm • IR SED of Young starburst/super-wind phase of massive elliptical galaxies@z~3 • Stellar Mass can be traced out to even z~5-10

  21. Detection Capability of SPICA- Spectroscopy -

  22. Background Photons for SPICA Instruments

  23. Line flux sensitivity –an advantage of SPICA • Cooled telescope  extremely low background photons at l>5mm  very long exposure (~1 hour/frame) is possible  High sensitivity for lines! • > 5 orders of magnitude improvement from ground-based / air-borne spectrometer @ l>5mm

  24. SPICA Line Sensitivity • 3rd March 2003 revision • Line profile is unresolved • >3 orders of magnitude improvement from ASTRO-F / SIRTF / ISO

  25. It’s not a dream to achieve the flux limit down to 10-21W/m2（10mJy＠１０mm) !!

  26. Fine Structure Lines from M82 at high-z • Metal lines from dusty starburst (~1010L◎) can be detected out to z~4

  27. Ha, Brg & [O II] for SFR=100 M◎yr-1, no extinction • Ha blobs can be detected out to z=10 & SFR>10M◎yr-1!

  28. Uniqueness of SPICA (Spectroscopy) • SPICA can detect Ha out to z~20! • Complementary to JWST, which can detect Lya out to z~20 • SPICA can detect many metal lines (optical ~ mid-IR in rest frame) from starburst galaxies out to z~5-10! • Complementary to ALMA, Herschel

  29. SPICAで狙うサイエンスワークショップ • 光赤外将来計画シンポジウム（8月21－22）でＳＰＩＣＡは高い評価（と期待） • 時期：12月、　場所は国立天文台か宇宙研 • 研究会の内容： • 観測装置の具体的な提案 • いろいろな分野からの狙うサイエンスについての提案 • みなさん、ぜひ一緒にかんがえましょう！

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