新生SPICAの体制・観測系検討の現状

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SPICA現状報告

1. ESA-JAXA共同技術検討（CDF Study）とその後の技術検討

・検討結果が確定し公開された。・その後、サイエンス検討を重ねた結果、検討のベースラインを望遠鏡口径2.5ｍ、温度8K以下に冷却する「横置き」（Planck型）構造をベースラインとすることとした。（８－１１ページ参照）・以下のチームが核となり、ESAの技術検討結果および従来のSPICAの成果などを用いて、衛星全体の設計、冷却系・望遠鏡設計を進めている。来月には一次的な検討結果が得られる予定。２．SPICA CV M5 対応チーム設置（6/4所長決定）・宇宙研（JAXA）のΔMDR、SRRのための作業、および、ESAのCosmic Vision次回Mクラス公募への提案の作業を行うチームを組織し、設置した。・宇宙研赤外、国内赤外線天文学研究者、宇宙研宇宙物理学研究系、宇宙研工学、研究開発本部、SE/PO室、国際調整担当の合同チームチーム長：芝井、チーム長代理：小川博之、中川貴雄・プリプロジェクト再設置時までのチーム・SPICAステアリンググループ（所内外）とSPICAタスクフォース（所内）がチームの活動をウォッチ。光赤天連スペース将来計画シンポジウム 2015-07-08 1

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３. SPICAチームの活動

3/25-27 SPICA（SAFARI?）コンソーシアム会議（Utrecht）・ M5提案に向けて最終決断。・ SAFARIチームが欧州＋カナダ＋米国（一部研究者）に拡大・高分散中間赤外線分光機能、および系外惑星大気分光機能を搭載する方向で検討を進める。（３、４ページ参照） 3/31 SPICA全体会 5/18 学術会議天文宇宙分科会にて状況報告この間、サイエンス検討・深化を進めた。（５－７ページ参照） 6/3-5 米国遠赤外コミュニティーワークショップにて講演 6/19 SPICA 科学レビュー（宇宙研）

7/15 SPICA Science Case International Preview (Paris、宇宙研主催)

（１３ぺージ参照）

7/31 SPICA全体会

9月 SPICAコンソーシアム会議（Bordeaux、SAFARI主催）

（１２ぺージ参照）

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1. SPICA mission overview

SPICA

– Space Infrared Telescope for Cosmology and Astrophysics

3

 SPICA is a space mission optimized for mid- and far-IR astronomy.

 SPICA unveils the “dusty era” in the Universe (evolution of galaxies), and finds a route to habitable planets (formation of planetary systems).

 SPICA is launched at ambient temperature, and cooled down in space.

(The cryo-cooler system is a key heritage of JAXA from IRTS and AKARI.)  Japanese SMI is a mid-IR spectrometer covering 17-37 mm.

 European SAFARI is a far-IR spectrometer covering 34-230 mm.

 SPICA is a joint mission of JAXA and ESA with other international partners.  SPICA is now in its re-definition phase in JAXA, and will go to the open

competition as an M-class mission of the ESA Cosmic Vision program.

 Baseline specifications

 Telescope : 2.5 m aperture, cooled below 8 K  Core wavelength : 17–230 mm

(+ High-resolution spectrometer at 12–18 mm, Exoplanet instrument at 5–20 mm)

 Orbit : S-E L2 Halo Orbit  Launcher : JAXA H-3 Vehicle  Launch Year : 2027-2028

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H H

H H O

D H

20 30 40 Si O O O Mg O HRS 12 14 16 18 λ (μm) 17.2 17.3 20 40 60 λ (μm)

AKARI Mid-IR all-sky map

SPICA studies



how stars have been formed in galaxies along the history of the

Universe (Goal1: evolution of galaxies),

and



how planets have been formed in a disk around a forming star and

evolved to be habitable (Goal2: formation of planetary systems).

Enrichment of the Universe with metal and dust

leading to the formation of habitable worlds

4

IR spectroscopy

1. Dust bands (organic matter, mineral, ice)

2. Extinction-free metal lines

3. Molecular hydrogen lines

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銀河成長と惑星系形成：

多様で豊かな宇宙を生んだ二大過程の解明

大目標

目的１. 銀河成長・物質進化過程の解明

- ダストに隠された銀河成長最盛期

（宇宙論的分光サーベイ、10平方度）

- 星生成と物質進化の相互作用（近傍銀河、4000個）

目的２．惑星系形成過程の解明

- ガスの精密定量による惑星形成シナリオの検証

- 惑星形成における水と氷の役割

- 惑星系外縁天体の起源

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Space infrared astronomy: from IRTS, AKARI to SPICA

6 IR lumino sit y densi ty ( L  / Mpc 3 ) Goto+ 2010,_{A&A 514, 6} redshift IR galaxy Luminous IR Ultra-luminous IR

AKARI (Japan, Korea, Europe) 2006 ~2011 Spitzer (US) 2003 ~ IRTS (Japan) 1995

Herschel (Europe, US) 2009〜2013

Photometry

Exploration

Physics

Spectroscopy

SPICA

AKARI

IRTS

survey

mid-IR

spectroscopy

far-IR

spectroscopy

Evolution of galaxies

z=3

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MIR Instrument （SMI）

Telescope

(NAOJ)

SPICA Data Center Launcher Science Community JP, Europe, US, KR, TW,,, Bus Module Payload Module Cryocooler

Focal Plane Instrument Assembly FIR Spectrometer （SAFARI） Exoplanet Spectroscopy （SPEChO） European countries NL + European countries + Canada & US

Focal Plane Attitude Sensor

Work-sharing plan

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Mirror M1 2.5 mf Mirror M2 Telescope Baffle PLM Metering Structure M2 Support Structure Telescope Optical Bench V-Groove thermal shields Supporting Bipod Telescope Shield (20 K) SVM Top Panel AOC StarTracker Cryo Warm Electronics

1K-JT Compressors 2ST Compressors 1K-JT Compressors

Planck-type PLM with a 2.5-m, <8K telescope

Current baseline configuration

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ESA Stations Mission Operation Center (MOC) Science Operation Center (SOC) Science Data Center (SDC) JAXA Stations JAXA ESA Instrument Control Centers (ICCs)

ESA Science Center (ESC) Non-European User Community (Japan) (East Asia)

European Data Archive Center (ESDC) TBD

European User Community

Operational Ground Segment Science Ground Segment

9

運用体制（案）

JAXA宇宙科学研究所

国立天文台

ESA

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プロジェクト推進体制－ SPICA コンソーシアム

SPICA

Consortium

SPICA-J Project SRON

日本

ESA SMI Consortium SPEChO Consortium SAFARI Consortium NAOJ M5 Proposal Scientists (outside the instrument teams) 10 中間赤外観測装置（日本）名大、東大他系外惑星大気分光装置（検討中）遠赤外線観測装置（欧州＋）装置チーム外研究者

欧州

JAXA

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（参考）国際評価委員会

目的

SPICA計画について、科学的観点からの評価を得る。

日時・場所

2015年7月15日 Paris

評価委員

Michael Rowan-Robinson (UK),

Martin Bureau (UK), Anthony Jones (FR)

Peter Barthel (NL) Anthony Peter Jones (FR) Martin Harwit (US), George Helou (US)

Kazuhisa Mitsuda (JP),

ISAS

Saku Tsuneta, Masaki Fujimoto, Munetaka Ueno, Ikko Funaki

SPICA

Hiroshi Shibai (PI), Takashi Onaka (PS),

Hidehiro Kaneda (PI補佐), Kotaro Kohno (PS補佐) Daisuke Ishihara, Takehiko Wada, Naoki Isobe, Peter Roelfsema (NL), Bruce Sibthorpe (NL)

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Space infrared astronomy: from IRTS, AKARI to SPICA

12

10 – 50 AU

Case study

SPICA

AKARI

IRTS

survey

AKARI (Japan, Korea, Europe) 2006 ~2011 Spitzer (US) 2003 ~ IRTS (Japan) 1995

Herschel (Europe, US) 2009〜2013

SPICA

AKARI

IRTS

survey

mid-IR

spectroscopy

far-IR

spectroscopy

Universality

~1 AU

Planet-forming disk

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Project schedule

13

Reviews & Phases

MDR SRR SDR Project Appr. Rev.pre-PDR Sys-PDR pre-CDR Sys-CDR PSR Launch

Phase-A PRR Phase-B1 SRR Phase-B2 PDR Phase-C CDR Phase-D QR? AR margin Phase-E1 Model & Tests

AI L Launch Operation PLM Caption FM SIA CQM (FPI) EM/STM Front Loading Q2 Q3 Q4 Q1 Q2 Q3 2025 2027 Q4 Q1 Q4 Q1 Q2 Q3 Q4Q1 Q2 Q2 Q4 Q2 Q3 Q4 Q1 Q2 Q3 Q4Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 CY 2015 2016 2017 2018 2019 2020 2021 2022 2023 2024 2026 Q3 Q3 Q4 Q1 Q2 Q4 Q1 Q3 Q1 Q2 Q3 Q4 Q1 Q2 Q3 2028 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Phase-E JAXA ESA Phase-A System IVT ESA AIVT JAXA SVM AIVT PLM Comp Dev. SAFARI Consortium + SMI Consortium AIVT AIVT MCS Comp. Dev.

FPIA Design AIVT

FAS Design

Manufacture

FPIA IVT AIVT

PLM/CRYO Design manufacture

MCS Design / Manufacture MCS

SVM Design manufacture

FPIA FAS

STA Design / Manufacture

AIV IV STA Manufacture AIVT Manufacture SAFARI Design Manufacture

SAFARI Components Devekopment

AIVT

SMI Design manufacture

SMI Components Development

Phase-D Phase-C Phase-B AIVT AIVT SAFARI Manufacture AIVT manufacture SIA IVT AIVT SMI AIVT AIVT System IVT PLM IVT PLM/CRYO AIVT

FPI Warm Elechtronics

IOB-STM PLM/CRYO-STM MCS-EM SMI-CQM Detector Modules SAFARI-CQM Design

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SPICA

10

5

_{reduction !}

K

SPICA

(8K)

Importance of a cryogenically-cooled IR telescope

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AKARI FIS-FTS JWST/MIRI Li mi ting Li ne F lux (5  -1h r) / Wm -2 ₁₀-16 10-18 10-17 10-19 100 ₁₀₀₀ 20 200 350 Wavelength / mm

2010's

Dramatic improvement in the sensitivity

15 100 Improvement AKARI IRC

SPICA

2020's

ALMA 10-20 10 10-15 SPICA/SAFARI R=25000 R=300 SOFIA HERSCHEL Spitzer R=3000

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SPICA’s uniqueness in extra-galactic astronomy

16

ALMA

Sensitivity (5, 1 hour) of ALMA, SPICA, JWST and TMT, plotted on spectra of typical star-forming galaxies at z = 3 with different dust extinction values (A_V = 0.3, 3, 30 mag).

TMT

A_V= 0.3 mag

JWST

SPICA

SPICA fills the spectral gap between ALMA and JWST.

SPICA provides unique spectral tools

to study physics in dust-obscured galaxies.

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2.1. Overview

Science goals and objectives

17

Top-level goal

Enrichment of the Universe with metal and dust, leading to the formation of habitable worlds

[SG1]

Evolution of galaxies

[SG2]

Formation of planetary systems

[SO1]

Star formation of distant galaxies

[SO2]

AGN outflow

[SO3]

Star formation in nearby galaxies

[SO4]

Gas dissipation in PPDs

[SO5]

Debris disks to solar system

[SO6]

Exoplanet atmosphere

SCIENCE GOALS

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3.3. SPICA mission overview

Baseline design

18

Planck-type PLM with a 2.5 m, 8 K telescope

Front view

Side view

telescope baffle instrumentoptical _bench telescope thermal shield V-groove thermal shields primary mirror secondary mirror cryo-cooler system payload module service module

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3.3. SPICA mission overview

Telescope

19

 Optical design

 The 2.5 mφ optical design is scaled from the 2.0 mφ CDF study.

 Optical specifications

 Telescope type : Ritchey–Chrétien  Entrance Pupil Diameter : 2.5 m  Field of View : 30 arcmin

 Wave Front Error : <1.4 mm rms  Diffraction limited at 20 mm

 Temperature

 Launch: Room temperature  Operation: < 8 K

 Fabrication

 ESA is in charge of the procurement of the telescope.

 Technical Heritage

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3.3. Configuration and specifications

Mechanical cryo-coolers

Cooling performance & reliability have improved based on AKARI & SMILES (e.g., flexure

bearings to support the piston and displacer, inner outgas control, microphonics control).

Design lifetime of 1K-JT has improved based on ASTRO-H 4K-JT with enhanced

contamination control. These technologies are reflected in the 2ST and 4K-JT coolers.

20K-class two-stage Stirling cooler (2ST) 4K-class J-T cooler (4K-JT) 1K-class J-T cooler (1K-JT) Cooling

objectives JT precooling STA + FPIA

FPIA (SAFARI+SMI) Cooling power (EOL) 200 mW@20 K, 1000 mW@100 K 40 [email protected] K 10 [email protected] K Input power < 90 W < 90 W < 75 W Lifetime > 3 years (goal: 5 years) >3 years (goal: 5 years) >3 years (goal: 5 years) Heritage AKARI (2006), JEM/SMILES (2009) ASTRO-H (2015) JEM/SMILES (2009) ASTRO-H (2015) Based on 4 K-JT

R&D status TRL6 (ASTRO-H) TRL6 (ASTRO-H) TRL5

Mechanical cryo-coolers in the baseline design have been developed in Japan.

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Focal-plane instruments

Spectral Resolution SPICA/SMI SPICA/SAFARI R = 3000 R = 300 Line Sensitivity Wavelength (mm) Wavelength (mm)

SPICA Far-IR Instrument: SAFARI

SPICA Mid-IR Instrument: SMI

EChO instrument on SPICA: SPEChO

(LRS) 17-37 mm, Si:Sb, prism:10’ slit x 5 + 10’x10’ slit viewer, high mapping speed (MRS) 18-36 mm, Si:Sb, grating:1’ slit + beam-steering mirror, high sensitivity

(HRS) 12-18 mm, Si:As, grating: 6” slit + beam-steering mirror, high resolution 34-230 mm, TES, grating: 4 beams + beam-steering mirror, high sensitivity

5-20 mm, Si:As, grating, high-stability (10-3.5 _{in one eclipse) monitoring}

R = 25000 R = 1000 JWST/MIRI-MRS Spitzer/IRS JWST/MIRI-LRS Spitzer/IRS 21

新生SPICAの体制・観測系検討の現状

SPICA現状報告

1. ESA-JAXA共同技術検討（CDF Study）とその後の技術検討

３. SPICAチームの活動

SPICA

H H

D H

SPICA studies



how stars have been formed in galaxies along the history of the

Universe (Goal1: evolution of galaxies),

and



how planets have been formed in a disk around a forming star and

evolved to be habitable (Goal2: formation of planetary systems).

Enrichment of the Universe with metal and dust

leading to the formation of habitable worlds

IR spectroscopy

1. Dust bands (organic matter, mineral, ice)

2. Extinction-free metal lines

3. Molecular hydrogen lines

銀河成長と惑星系形成：

多様で豊かな宇宙を生んだ二大過程の解明

大目標

目的１. 銀河成長・物質進化過程の解明

- ダストに隠された銀河成長最盛期

（宇宙論的分光サーベイ、10平方度）

- 星生成と物質進化の相互作用（近傍銀河、4000個）

目的２．惑星系形成過程の解明

- ガスの精密定量による惑星形成シナリオの検証

- 惑星形成における水と氷の役割

- 惑星系外縁天体の起源

Space infrared astronomy: from IRTS, AKARI to SPICA

Photometry

Exploration

Physics

Spectroscopy

SPICA

AKARI

IRTS

survey

mid-IR

spectroscopy

far-IR

spectroscopy

z=3

Work-sharing plan

Current baseline configuration

運用体制（案）

JAXA宇宙科学研究所

国立天文台

ESA

プロジェクト推進体制 － SPICA コンソーシアム

SPICA

Consortium

日本

欧州

（参考）国際評価委員会

目的

SPICA計画について、科学的観点からの評価を得る。

日時・場所

2015年7月15日 Paris

評価委員

ISAS

SPICA

Space infrared astronomy: from IRTS, AKARI to SPICA

10 – 50 AU

Case study

SPICA

AKARI

IRTS

survey

SPICA

AKARI

IRTS

survey

mid-IR

spectroscopy

far-IR

spectroscopy

プロジェクト推進体制－ SPICA コンソーシアム

_{reduction !}