光赤外線天連シンポジウム

SPICAの進行状況報告

2015-09-15
芝井 広（大阪大）、他SPICAチーム戦略的中型としてスタートする見通しが立った。
日欧（米亜）の研究者の支援を結集する必要。

1

SPICA – Space Infrared Telescope for Cosmology and Astrophysics

中間赤外線、遠赤外線に最適化されたスペース天文学ミッション
The “dusty era” in the Universe (evolution of galaxies)
A route to habitable planets (formation of planetary systems).
常温で打ち上げて、スペースで冷却（IRTSとAKARIからの技術継承発展)
中間赤外線分光装置 SMI （日本）： 17–36 mm
遠赤外線分光装置 SAFARI （欧州）： 34–230 mm
日欧宇宙機関の共同ミッションプロジェクト（米国その他からも参加予定）
現在、JAXA内で「再定義フェーズ」。まもなく（Δ）ミッション定義審査を受けるとともに、ESAの M5 ミッションに応募。

口径と温度。遠赤外：フーリエ ⇒ グレイティング。サイエンス目的先鋭化。
宇宙科学の「戦略的中型」程度の規模。国内の総力を結集。日欧役割変更。
 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 H3 Vehicle
 Launch Year : 2027–20282

Importance of a cryogenically-cooled IR telescope
A cryogenically-cooled telescope significantly reduces thethermal emission from the telescope.

K105 reduction !
SPICA(8K)
SPICA

3

Dramatic Improvement in SensitivityAKARI FIS-FTS

Limiting Line Flux (5-1hr) / Wm-2

10-15

A cryogenically-cooled
telescope makes dramaticimprovements in thesensitivity in IR observations.

SOFIA

10-16

K

10-17
AKARI IRC

Spitzer

10-18

2010'sHERSCHEL

100 Improvement

10-19

ALMA

R=300

SPICA/SAFARI

R=25000

10-20

JWST/MIRI
R=30001020

SPICA (2.5m,8K)
100

Wavelength / mm

200

2020's350

1000
4Work-sharing plan
Telescope

Focal Plane Instrument Assembly
FIR Spectrometer（SAFARI）

Payload Module

NL + European countries+ Canada & US

Cryocooler
MIR Instrument （SMI）
BusModuleLauncher

Focal Plane Attitude Sensor

Exoplanet Spectroscopy（SPEChO）
European countries

SPICA Data Center(NAOJ)

Science Community
JP, Europe, US, KR, TW,,,

5

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。

5/18

学術会議天文宇宙分科会にて状況報告

6/3-5

米国遠赤外コミュニティーワークショップ

6/10

宇宙研内に「SPICA CV M5 対応チーム」設置

6/19
7/15

SPICA 科学レビュー（宇宙研）
SPICA Science Case International Preview (Paris、宇宙研主催)

9/19

宇宙研（Δ）ミッション定義審査

9/30-10/1

SPICAコンソーシアム会議（Bordeaux、SAFARI主催）
6周辺状況、関連事項••••

•

•

政府関連
• 大型研究計画予算の大幅削減
日本学術会議• 天文宇宙分科会（5/18）にてSPICA現状報告。重点大型計画として再確認。
光赤天連• SPICAタスクフォースの報告書が完成
宇宙研• SPICA CV M5対応チーム設置• SPICA国際科学評価実施、勧告受領• ΔMDR再開、JAXA内プロジェクト化準備審査予定。
欧州• PLATO、CHOPSが進行中• ARIEL（系外惑星大気分光ミッション）がM4第一段階審査で残る。
米国• TESS、JWSTが着実に進展。 WFIRSTがまもなくスタートの見込み

1

ESA Cosmic Vision M5 Call
SoI（提案意思表示） : 9月25日まで
Event
M5 Call release
Letters of Intent due
Proposals due
Evaluation process
Selection of proposals for study phase
Phase 0+A completion
Down-selection to one mission
Phase B1 completionMission Adoption Reviews
Mission adoption
Launch (for an ESA-only mission)

Tentative date
December 2015
January 2016
April 2016
May–June 2016
June 2016
June 2018
November 2018
June 2020
September 2020
November 2020
Mid–2029 to mid–2030

日本側は2027-2028年打ち上げ
ノミナル３年、ゴール５年の運用 で計画
8Project Schedule
CY

2015

2016

2017

2018

2019

2020

2021

2022

2023

2024

2025

2026

2027

2028

Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1

Reviews & Phases

Phase-A

JAXA

MDR

SRR

ESA

Phase-A PRR

Phase-B
SDR

Phase-C

Project Appr. Rev.
pre-PDR

Phase-B1 SRR

Sys-PDR

Phase-B2

Phase-D

pre-CDR

PDR

Phase-E

Sys-CDR

Phase-C

CDR

PSR
Phase-D

QR?

LaunchARmarginPhase-E1

Model & Tests

JAXA
PLM/CRYO Design

PLM Comp Dev.

manufacture

MCS Design / Manufacture

MCS Comp. Dev.

AIVT

PLM/CRYO-STM

AIVTAI

PLM/CRYOL

AIVTMCS

Launch Operation
Manufacture

manufacture

FAS Design

AIVT

FAS

AIVTPLM IVTAIVT PLM

System IVT

ESA
SVM Designmanufacture

AIVT

System IVT
SVM

SIA IV
Design

STA Manufacture

SIA IVTAIVTFM

FPI Warm Elechtronics

CQM (FPI)AIVEM/STMAIVT

STA Design / Manufacture

FPIA Design

CaptionAIVT

IOB-STMMCS-EM

FPIA

Front Loading

AIVT

FPIA IVTSMIManufacture

Consortium

SMI Design

manufacture

SMI

AIVTSAFARI

Manufacture

Consortium+SMI-CQM

Detector Modules

SMI Components Development

SAFARI Design
SAFARI Components Devekopment

Manufacture

AIVTSAFARI

AIVT

AIVT
SAFARI-CQM

Operation: 3 Years (Nominal), 5 Years (Goal)

9SPICA Management Structure (Japan)
ISAS (JAXA)
Director General
Saku Tsuneta

Japanese
SPICA TeamSPICA PI & Chief
Hiroshi Shibai (OsakaU)

Deputy Chief

Assistant
SPICA PI& SMI PI

Takao Nakagawa(ISAS)

Hidehiro Kaneda(Nagoya U)

Hiroyuki Ogawa(ISAS)

Deputy Chief

Chief
Satoshi Yamamoto (UProject Scientist
Tokyo)
Takashi Onaka (UTokyo)

Assistant PS

Toru Yamada (U Tohoku)

Assistant PS
Kotaro Kohno (U Tokyo)

Payload Module(JP)Hideo Matsuhara(ISAS)

Staff
in ISAS, JAXA,Universities
NAOJ

Science CoreTeam
SPICA Science T/F

SAFARI (JP)Yasuo Doi (UTokyo)

SPICA DataCenter
Issei Yamamura
SPICA Data Center(ISAS)

in Japan withNAOJ

Top-level science goal
To reveal the processes that enrichedO theH OUniverse
D HH H
with metal and dust,MgOOSi O H
leading to the formation of habitable worlds
2030

40

SPICA studies
 metal and dust enrichment through galaxy evolution (Goal 1), and planetary system formation to habitable systems (Goal 2)

IR spectroscopy
SPICA’s unique probes

20

40
λ (μm)

60

1. Dust bands HRS(organic matter, mineral, ice)
17.2 17.3
2. Extinction-freemetal lines
3. Molecularhydrogenlines
12141618
λ (μm)AKARI Mid-IR all-sky map

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SPICA’s uniqueness in extra-galactic astronomy
Sensitivity (5, 1 hour) of ALMA, SPICA, JWST and TMT, plotted on spectra of typicalstar-forming galaxies at z = 3 with different dust extinction values (AV = 0.3, 3, 30mag).
SPICA provides unique spectral tools
to study physics in dust-obscured galaxies.

SPICA
ALMA

AV = 0.3 mag

II Zw 96

TMT
JWST

SPICA fills the spectral gap between ALMA and JWST.

12Science goals and objectives
Top-level goal
Enrichment of the Universe with metal and dust,
leading to the formation of habitable worlds
SCIENCE GOALS
[SG1]
[SG2]
Metal and dust enrichment
Planetary formation tothrough galaxy evolution
habitable systems

Science objectives

Science objectives[SO1]
Star formation of distant galaxies[SO4]
Gas dissipation in planet-forming
disks

[SO2]
Dust-obscured AGNs and AGN
outflow[SO5]
Dust evolution in planet-forming
disks to solar system analogues[SO3]
Star formation in nearby galaxies[SO6] Optional
Exoplanet atmosphere13

[SG1] Metal and dust enrichment
through galaxy evolution
Spectroscopic studies of the processes of metal and dustenrichment and their interplay with star formation and
AGN activities through galaxy evolution from the early tothe present Universe.

Spatially-resolved,High-z analogs or relics

Over the peak of the cosmic
star-formation history

Beyond the peak,First mineral, aromatics

4,000 nearby galaxies
at <100 Mpc~60,000 galaxies at z = 0.5–3
1,000 SF galaxies & 1,000 AGNs
for detailed study~100 galaxies
at z = 4–10

Spectral mapping

Unbiased spectroscopic survey

Targeted spectroscopy

14

[SG2] Planetary formation
to habitable systems
Spectroscopic studies of the processes of gas dissipationand dust evolution in planet-forming disks at various
stages, and the resultant atmosphere of formed planets.

Gas dissipation in protoplanetary disks

Changes of mineral and ice
properties in debris disks

Atmosphere ofhabitable planets>200 protoplanetary disks>1,000 debris disks with
mid-IR excess down to
the solar system level~10 M-type stars

Targeted spectroscopy

15

Unbiased spectroscopic survey

Transit spectroscopy

15

国際科学評価委員会
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),David Elbaz (FR), Anthony Peter Jones (FR)Peter Barthel (NL),
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)16

Executive Summary
The SPace Infrared telescope for Cosmology and Astrophysics (SPICA) is a
mid- and far-infrared spectroscopic mission to reveal the processes thatenriched the Universe with complicated materials and led to the formation of
our world today. This scientific goal and derived scientific objectives havebeen set by the SPICA team, and were evaluated by an international review
committee. This Short Report summarizes the key findings of the committee,and will be followed by a more detailed report. The Committee is mostappreciative of the team’s work in preparing the material for the Preview, andof the quality of the presentations.
1.

The committee strongly supports the mission concept of a 2.5m telescope
cooled to 8K with powerful spectrometers in the focal plane; it represents
two orders of magnitude improvement in sensitivity over Herschel, andoffers major discovery potential. The Committee feels however that this isa minimum configuration, i.e. there is no margin for reducing sensitivity orresolution requirements. (NB: Based on discussions during the Preview,
the Committee assumes that the SAFARI instrument is photometrycapable, even though the specifics of that capability were not presented)

2.

The science case as stated is compelling, both today and in the anticipatedenvironment of the 2020’s.
3.
The science case can be strengthened by (a) integrating more closely inthe statement of each Science Objective scientific synergies with otherfacilities of the 2020’s (e.g. TMT/ELT; ALMA; JWST; Euclid & WFIRST;ATHENA; SKA, etc); and (b) identifying more science topics to engage andserve the science community beyond traditional users of IR missions (e.g.
stellar astrophysics, baryon circulation between galaxies and inter-galactic
medium, exoplanet science, etc). Item (b) might be accomplished byidentifying “key questions” in major community reports to which SPICA
could contribute.
4.

The summary science justification (slide entitled “Science goals andobjectives”) can be strengthened as follows: (a) Keep the vision of heavy
element enrichment and push it both to earlier epochs and to the lowredshift Universe by emphasizing the potential for great advances in ourestimation of the abundances of chemical elements; (b) modify SO2 toemphasize heavily obscured and Compton-thick systems [strong synergywith ATHENA];

(3) bring in as SO the detection of SiO and Aromatics at redshifts of 3 to 6;(4) bring in as SO something related to the top-level goal, such as
metallicity evolution using Fine-Structure Line observations. Moresignificantly, (5) move SO6 to an appendix (along with SPEChO); thereason is that if SPEChO is essential to mission success, then it brings toSPICA asignificant risk of very limited science return as it flies a decade afterJWST, at a high cost in observing time.

5.
Even after removing SO6, the mission has too large a fraction of timecommitted to pre-determined observing programs; the committee feels thiswould lessen community interest, and would weaken the science case in
the context of the ESA competitive processes. As a guideline, predetermined “key science” programs should fit within a year of wall-clocktime.
6.
The placement of “PAH survey” on the sky is critically important: theSPICA Team is advised to exploit existing fields which already have deep
coverage at a variety of wavelengths to leverage extant data for enhanced
science, and more readily engage with other communities and additional
science themes.

7.
In stating the case for Evolution of Galaxies, model shortfalls were overemphasized; the science case could mention those shortfalls as
motivation, but then emphasize the need for essential or unique data that
address the underlying physics, both in processes and in dust properties.
Where appropriate, the science case could include testing specifichypotheses (e.g. Initial Mass Function variations). The same point applies tothe discussion of proto-planetary disk science.

8.
Before ESA’s M5 competition gets under way, the SPICA team should
address the question of the programmatic organization of time allocationand science responsibility, and in particular express their views on how tostimulate a vigorous, competitive open time program.

9.
Before ESA’s M5 competition gets under way, the SPICA team should
address the means and plans to enable rapid data reduction and calibration.
10.
The committee couldn’t help but notice the all-male cast on the SPICA teamand on the review committee itself. It is in the best interests of the future ofJapanese (infrared space) astronomy to address this gender imbalance.
Apart from that, the imbalance may become an issue in the context of theESA competitive process.