はなしの概要 あかり 遠赤外線分光器FIS-FTS FIS-FTSによる観測 セレンディピタス分光サーベイ FIS-FTSのデータ解析 キャリブレーションと標準ツール 初期成果 銀河中心 Yasuda et al. 星形成領域 Okada et al. 今後の解析 LMC セレンディピタスサーベイ
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1 あかり 遠赤外線分光観測の成果 宇宙物理学研究室 赤外線グループ UIR 川田光伸 2009 宇宙ブロック研究発表会 エコトピア
2 はなしの概要 あかり 遠赤外線分光器FIS-FTS FIS-FTSによる観測 セレンディピタス分光サーベイ FIS-FTSのデータ解析 キャリブレーションと標準ツール 初期成果 銀河中心 Yasuda et al. 星形成領域 Okada et al. 今後の解析 LMC セレンディピタスサーベイ 将来の展望 遠赤外線分光サーベイの時代へ SPICA/SAFARI
3 あかり 遠赤外線分光器 撮像型フーリエ分光器 UIR研で開発したスペース用遠赤外線フーリエ分光器 特徴 天文観測用冷却遠赤外線フーリエ分光器 スペース用としてはCOBE/FIRASに次ぐ2番目の装置 分光と撮像が同時にできる 世界初 Herschel/SPIREに先んじる 空間分解能が高い 1分角を切る空間分解能での撮像分光 細かな空間構造でのスペクトル観測を効率よく行える ISO/LWSとの比較 Gratingによる分光 比分解能 R= Fabry-Perots分光器による高分解能モードあり R= シングルピクセル 空間分解能 80
4 AKARI FIS-FTS Optics Type Mirror Driving Type Position Sensor Spectral Coverage Maximum o.p.d. (L ) Spectra Resolution (R) [d = 1/(2L)] Mirror Scan Speed : polarized Michelson interferometer (Martin-Puplett type) : leaf springs axis support with voice coil actuator : optical scale (resolution: 2 µm in o.p.d. ) /wo zero path detector : cm-1 (50 180µm) : ~ cm : 0.19 cm-1 (Full-res. Mode; L=2.8 cm) 1.2 cm-1 (SED mode, L=0.42 cm) Kawada et al., 2008 : ~ 0.08 cm s-1 FIS (without top cover) Mirror Driving Mechanism 4
5 Martin-Puplett Interferometer FIS Design Two position Filter Wheel SW detector ( µm) SW detector 12mm 15mm LW detector - direct hybrid type - Ge:Ga + Si RO /w In bump - format: 3 x 20 & 2 x 20 LW detector ( µm) - compact stacking type - stressed Ge:Ga + Si RO - format: 3 x 15, 2 x 15 5
6 AKARI FIS-FTS Detector System: Detector Unit Name: Detector Type: Array Format: Pixel Size (pitch): Pixel FOV: FWHM (major/minor): Spectral Coverage: Sampling Rate: PSF (x: array major axis): 2D Photoconductive Detector Arrays (Ge:Ga) with CTIAs (Si) SW LW monolithic Ge:Ga array stressed Ge:Ga array 3 x 20 3 x (0.55) mm 0.9 (1.0) mm 26.8 x 26.8 arcsec x 44.2 arcsec2 44 / / cm cm Hz Hz PSFFTS (x, y) = PSFphot (x-7, y) + PSFphot (x+7, y) Array Alignment (on the sky) PSF PHOT x, y = exp SW LW x Neptune Image y 2 2 x y exp 2 2 x y 2 22 SW: e = 0.8; σ1 = 14 ; σ2 = 40 LW: e = 0.65; σ1 = 17 ; σ2 = 46 6
7 FIS-FTSによる観測 指向観測モードで観測 1回約20分間の観測 含む 約8分間のキャル測定 2種類の検出器で50 180μm同時観測 3 x 20 pixels / 3 x 15 pixels の撮像分光 分解能の選択 Full-res.: 0.2 cm-1; SED: 1.2 cm-1 観測の種類 プライマリーモード ターゲット提案に基づく観測 115点 MP OT DT パラレルモード IRCとの同時観測 IRC優先モード 452点 MP-FISS3 IRC指向観測の約1割
8 Observation Sequence sequence of one pointing observation 30 minutes SHUTTER CLOSE SHUTTER OPEN FTS MODE Internal B.B.(37K) (~362s) FW rotating FTS mode start CLOSE SCANNER MODE observing the sky (719s) FW rotating Seq. Restart FTS mode stop Pointing Observation: - up to 3 times in an orbital period the telescope is held to the specific directions. - duration time of one pointing observation is about 30 minutes - effective observing time is about 12 minutes ~7.5 round scans for full-res. mode, ~30 round scans for SED mode - internal blackbody source (~35K) is measured for about 6 minutes in SED mode prior to the observation - FIS FTS can operate with the IRC observation: parallel observation mode observing direction is different from the IRC view 8
9 Observations (2006/04/ /08/25) Total Number of Observations: 597 points (12 minutes each) PV phase Primary obs. Parallel obs. : 30 points : 115 points (MP: 62, OT-ISAS: 7, OT-ESA: 24, DT: 22) : 452 points (MP-FISS3) SED mode : 259 points (PV: 21, Primary / Parallel: 50 / 188) Full res. Mode : 338 points (PV: 9, Primary / Parallel: 65 / 264) (data for several obs. are lost by downlink troubles) Observing Area (Galactic coordinate) concentrated on the Galactic plane (~ 55%) & Large Magellanic Cloud (~30%) : Parallel Observations : Primary Observations SED mode / Full-res. mode LMC 9
10 データ解析 フーリエ分光器とは 2光束の光路差に対する干渉強度の変化 インターフェログラム 時間軸方向への分散 空間軸方向への分散 グレーティング インターフェログラムのフーリエ変換 スペクトル キャリブレーション Murakami et al. 2010) 標準天体 惑星 準惑星 Uranus, Neptune ISO/LWSとの比較 連続成分 輝線 [CII], [NII], [OIII] 高輝度領域に対して検証 中 低輝度領域への拡張が必要 標準ツールの提供 IDLベースの解析ツールを提供
11 Data Processing & Calibration Raw Data First Data Reduction Second Data Reduction Interferograms Fourier Transform Raw Spectra Corrections Sky Spectra Murakami et al., non-linearity correction - differentiation - spike removing Calibration: - separate each scan - laboratory characterization - ZPD determination internal/external sources - opd correction - in flight correction - transient response correction - well-known astronomical sources - apodization - internal blackbody source - numerical integration of Fourier transform equation - phase correction - flat fielding - spectral response correction - absolute flux correction - fringe correction 11
12 Data Processing (1) LW07 SW32 First Data Reduction: non-linear correction differentiation & spike removing Second Data Reduction: ZPD determination & o.p.d. correction Fourier Transform: raw spectra & phase correction Data: SED mode 12
13 Data Processing (2) Flat Correction Fringe Correction (by model template method) SW SW LW (0.6~1.5) LW (0.2~7) (from measurement of aperture lid) LW array has much wider variety of responsivity Spectral Response Correction LW array has wider variety of spectral response LW01 60 LW LW Wavenumber [cm ] -1 SW (all)
14 Calibration Murakami et al., 2009 Lines - planets as the absolute calibrator, which have well defined spectral model - comparing with the ISO/LWS observations for lines and integrated power both ISO/LWS and AKARI/FTS calibration is consistent for brighter sources, at least Integrated Power 14
15 FIS-FTSによる初期成果 高い空間分解能と効率のよいマッピング能力 銀河中心領域 Quintuplet and Arches clusetes AKARI Far-Infrared Spectroscopic Observations of the Galactic Center Region Yasuda et al. (2009) 遠赤外線の禁制線 [OIII], [NII], [CII] を用いて クラスター近傍の物理構造を 明らかにした 銀河系内星形成領域 G , G , NGC3603, M17 Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI Okada et al., (2010) 遠赤外線輝線マップを用いて 星間物質の構造と隠れた励起星を明かにする 近傍銀河のスペクトルマッピング Takahashi et la. ηカリーナ領域のスペクトルマッピング Matsuo et al.
16 Scientific Results of AKARI/FTS (1) Line & Continuum Maps of the Galactic Center Region Yasuda et al. (2009) 88µm 5 pointing obs. [OIII] 88.4µm (MSX 12µm) 122µm [NII]122.0µm [CII] 157.7µm (20cm radio continuum) 16
17 Scientific Results of AKARI/FTS (2) 9um Line mapping of the Galactic HII regions Okada et al. (2010) 18um Full-range Spectrum of the AKARI/FTS G [OIII] 88µm [NII] 122µm [CII] 158µm 17
18 NGC3603 G [CII]158µm [OII]88µm 12min [CII]158µm [CII]158µm [OII]88µm [OII]88µm 30min 11min M17 contour: IRC 18µm / MSX 21µm 18
19 LMC領域の観測 LS-LMC IRCによるLMCの多バンド広域サーベイの裏観測 2期にわたり188点の観測 前半 SEDモード 30 Dor 近傍 後半 Full-res.モード それ以外 無バイアスな広域スペクトルサーベイ 複数の禁制線 [OIII], [CII] を検出 星形成領域 星間物質の空間構造を明かにする
20 AKARI/FTS Observations of the LMC region SED mode [CII]158µm Full-res. mode [OIII]88µm 188 observing points [CII]158µm AKARI 90µm map 6 deg 3 deg ~50 pixels for each points IRAS 100µm map 20
21 30 Dor Molecular Ridge領域の解析 AKARI 90um (ASS) RED : 90um GREEN : 65um
22 [OIII]輝線 強度マップ 3 x x 10-6 輝線強度 [W/m2/sr] 1 x
23 連続成分に対する [OIII]輝線強度 RED : AKARI 65um GREEN : MSX 8um BLUE : H
24 Wolf-Rayet O stars B stars (B0-B2.5) B stars (B3-B9) others 等価幅 EW と連続成分の強度 or 傾きとの相関
25 AKARI 65um map (ASS) Wolf-Rayet O stars B stars (B0-B2.5) B stars (B3-B9) others
26 将来への展望 遠赤外線分光サーベイの時代へ Herschel Space Observatory (3.5m telescope) - PACS (Photodetector Array Camera and Spectrometer) Integral Field Spectrometer: & um (47 x47 :5x5 pixels) - SPIRE (Spectral and Photometric Imaging Receiver) Imaging Fourier Transform Spectrometer: um (2.6' FOV: 37/19 pixels) - HIFI (Heterodyne Instrument for the Far Infrared Instrument) um (7bands/12-47 beam) R < 107 SPICA (Space Infrared telescope for Cosmology and Astrophysics) -SAFARI (SPICA Far Infrared Instrument) Imageing Fourier Transform Spectrometer: um (2'x2' FOV)
27 an off -source part of a 250 μ m ESA SPIRE publicity image (credit: ESA and the SPIRE consortium) Spitzer/AKARIによる近傍銀河 の近 中間赤外線分光診断を遠 方銀河 z< 5 に拡張する 個人的には オフソース領域の分光 背景放射の分光 に興味がある ライン構造だけでなくブロードな スペクトル構造を精密に決めた い フーリエ分光器に厳しい要求
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