Next Generation Space Infrared Telescope SPICA 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
Overview of SPICA and Current Status
Outline of SPICA Telescope: 3.5m, 4.5 K JWST(20-40K), HSO(80K) Core λ: 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
大口径へ： 設計思想の改革 冷媒なし → Cryostat なし → 画期的な軽量化 従来デザインでは 搭載不可能
冷却方法 : 効率的な放射冷却＋機械式冷凍 機
HIIA で打上げられる最大口径 を
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
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 ( 年度） FM ( 年度 ) 打ち上げ (2010 年度 )
Detection Limits of SPICA - Assumption & Procedure -
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: for spectroscopy Detectors / Optical throughputs: (micron) Exposure/frameReadout noise Detector quantum efficiency Optical throughput sec10e sec20e sec60e sec3000e0.50.1
IR Sky observed with COBE/DIRBE Zodiacal Light Kelsall et al. (1998) ApJ 508, 44 Interstellar dust emission Arendt et al. (1998) ApJ 508, 74
SED of Natural Background Emission Old assumption, please forget this..
Detection Capability of SPICA - Broad-band Imaging -
SPICA Point Source Sensitivity 1 hour, 5sigma 3 rd March, 2003 revision
Comparision with Other Missions sorry, a bit old…
~3mJy Submm Galaxies & SPICA sensitivity(1hour, 5 )
A possible Scenario of massive Elliptical Formation & Evolution Building Blocks (clumps) Major Merger Galactic Wind Passive Evolution Phase Dusty ULIRG Phase !!
SED of Young Ellipticals Totani et al. (2001) Young Galactic wind z=2.7
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 M ◎ out to z~10! Courtesy to T. Kodama/NAOJ
Unfortunately in the FIR, SPICA ’ s beam is similar to that of SCUBA (15m, 850μm) = (3.5m, 200μm) SCUBA 8mJy Survey Fox et al. (2002) MNRAS 331, 839 radio ROSAT
Uniqueness of SPICA (Broad-band Imaging) JWST is more < 5 m Strongly confusion limited by faint > 200 m Hence core wavelength must be 5~200 m IR SED of Young starburst/super-wind phase of massive elliptical Stellar Mass can be traced out to even z~5-10
Detection Capability of SPICA - Spectroscopy -
Background Photons for SPICA Instruments
Line flux sensitivity – an advantage of SPICA Cooled telescope extremely low background photons at >5 m very long exposure (~1 hour/frame) is possible High sensitivity for lines! > 5 orders of magnitude improvement from ground-based / air-borne >5 m
3 rd March 2003 revision Line profile is unresolved >3 orders of magnitude improvement from ASTRO-F / SIRTF / ISO SPICA Line Sensitivity
It ’ s not a dream to achieve the flux limit down to W/m 2 （ 10 Jy ＠１０ m) !!
Fine Structure Lines from M82 at high-z Metal lines from dusty starburst (~10 10 L ◎ ) can be detected out to z~4
H , Br & [O II] for SFR=100 M ◎ yr -1, no extinction H blobs can be detected out to z=10 & SFR>10M ◎ yr -1 !
Uniqueness of SPICA (Spectroscopy) SPICA can detect H out to z~20! Complementary to JWST, which can detect Ly 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
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！