SPICAの現状
金田英宏（名大） 2015/6/5 第二回銀河進化研究会
OH
Mg Si OOO
203040HRS
17.2 17.32040λ (μm)

60121416λ (μm)

18OH

D HH HEnrichment of the Universe with metal and dust
leading to the formation of habitable world
OH
Mg Si O
OO
2030

OH40

 Evolution of galaxies
 Formation of planetary systems

IR spectroscopy
1. Dust bands (organic matter, mineral, ice)
2. Extinction-free metal lines
3. Molecular hydrogenlines
HRS
17.2 17.32040λ (μm)

60121416λ (μm)

18

D HH H

望遠鏡口径2.5 m, 温度8 K （← 3.2 m, 6 K）
O
H
Mg Si OOO

OH

D HH H

打ち上げ: 2027-2028 （← 2020年代前半）
2030

40

JAXA-ESA共同ミッション （← JAXA主導）

波長17-210 mm + α （← 5-210 mm + コロナグラフ、近赤外線）(1) 遠赤外線装置SAFARI（欧州） SAFARI, R=300, 3000 (=l/dl)(2) 中間赤外線装置SMI（日本、大学）, R=50, 1000, 25000(3) 系外惑星トランジット分光器（UK） SPEChO
冷却ミッション寿命： nominal 3年、goal 5年
HRS
17.2 17.3
2040
λ (μm)

60

121416λ (μm)

18Grating spectrometer with sensitivity ~5x10-20 W/m2

3 channels: LRS (10’ slit x 5 + 10’x10’ viewer), MRS, HRS (R=25000)

IR spectroscopy of galaxies
Star-forming galaxy at z = 3 (LIR = 1x1012 L)gas lines
flux (mJy)

PAH bands

[OIV]
[NeV]

Flux normalized at 27 mm

5Rest-frame wavelength (mm)102030 40 50

AGN
[NeV]
[SIII][SiII][S III][Ne II][Ne III](PAH band)

2030 40 50
100200Observed wavelength (mm)10Starburst
Tommasin et al. 2010

2030
Rest-frame wavelength (mm)

[Ne V], [O IV] are robust tracers of AGN.
EW (PAH): SF/AGN power ratio[Ne II], [S III], [O III], [N III], etc.: tracer of gas
density, temperature, metallicity.
PAH bands: much stronger thanGas Lines: reliable estimate of physical conditions gas linesof star formation activity.

How deep do we need to observe?
Integrated luminosity function suggests that major contributors to the IR luminosity(‘main sequence’ galaxies) become more luminous with redshift.
At z=3, galaxies with L=1x1012 L have to be observed to understand the IR luminosity
Evolution of luminosity function
density.
Integrated luminosity function

Log [LIR(L) f(Mpc-3 dex-1)]

98.5

z=0.0-0.3
z=0.3-0.45
z=0.45-0.6
z=0.6-0.8
z=0.8-1.0
z=1.0-1.2

contributors
for z=1-3

z=1.2-1.7
z=1.7-2.0
z=2.0-2.5
z=2.5-3.0
z=3.0-4.2

z=38

Gruppioni + 2013 MNRAS, 486 2875

Evolution of main sequence (MS) galaxies

7.5

present universe

76.5
891011Log L/L

121314
Whitaker+ 2012, ApJ 754, L29

For SF galaxies at z = 3 with L = 1x1012 LSMI

For SF galaxies at z = 3 with L = 1x1012 LH2SPICASMICALISTO whitepaper (2015)
By P. Appleton

Gas line & dust band diagnostics:
nearby Universe → distant Universe
Atomic gas line
[SIII] 18.7 μm[Cl IV] 20.4 μm

indicator
SFSFpurpose[ArIII] 21.8 μm

SF[FeIII] 22.9 μm[NeV] 24.3 μm[OIV] 25.9 μm[FeII] 26.0 μm[SIII] 33.5 μm[SiII] 34.8 μm

J-shock
AGNAGNJ-shockSF
J-shock/PDR

ne~105 cm-3(w JWST)
temperature[NeIII] 36.0 μm

SF[OIII] 51.8 μm

SF[NIII] 57.3 μm

SF[OI] 63.2 μm

PDR/C-shock[OIII] 88.4 μm

SF[NII] 121.7 μm[OI] 145.5 μm[CII] 157.7 μm[NII] 205.2 μm

SFPDRPDRSF

ne~104 cm-3

ne~104 cm-3
ne~105 cm-3
(w JWST)
ne~103 cm-3
metallicity
temperature
metallicitynH
ne~103 cm-3
metallicity
ne~102 cm-3
nH
NH
ne~102 cm-3

Molecular gas lines indicator
H2 17.0, 28.2 μm
PDR/
C-shock
HD 56, 112 μm
PDR
OH 53, 84, 119, 163μm
High-J CO
H2Opurpose
NH2CO-dark
gas tracer

PDR/
C-shock
C-shock
SFDust bandindicator
H2O ice 44, 62 μm PDR/MCpurpose
crystallinity

Crystalline silicate PDR/MC/C mineralogy,
crystallinity
24 – 69 μm
SM/SNRgraphite 30 μm

PDR/XDR

FeO 20 μm

SNRMgS 30 μm

CSM/SNRFeS 30-50 μm

SNR

Carbonate 20-100μm

temperature
crystallinity

Evolution of galaxies
How well do simulations simulate our Universe ?
Cosmological hydro-dynamical simulations(CHS) are performed based on the first principle

Semi-analytical models (SAM) can
explore a large parameter space

Illustris: Vogelsberger et al. Nature 509, 177 (2014)

Latest simulations successfully reproduce
a snapshot of the present universe
with ~1010 resolution elements

DM halo N-body simulation(Ishiyama+15)+
Mitaka model(Makiya+15 in prep)11

Evolution of galaxies
How well do simulations simulate our Universe ?
Cosmological hydro-dynamical simulations(CHS) are performed based on the first principle
Illustris: Vogelsberger et al. Nature 509, 177 (2014)

Latest simulations successfully reproduce
a snapshot of the present universe
with ~1010 resolution elements-1

Cosmic star-formation history
N-body DM simulation(Ishiyama+15 in press)+modelMitaka model(Makiya+15 in prep)

Galaxy Stellar Mass Function at z=0

model-2

Log N (dex-1 Mpc-3)

Semi-analytical models (SAM) canexplore a large parameter space

Mitaka model (SAM) (Makiya et al. priv. comm.)-3-4Model-5

Baldry+ 2012
Li & White 2009

-6-7-8

Shimizu priv. comm.
Based on Okamoto+14 model
678910Log M* (M)

11121312

Discrepancy in IR luminosity density (Herschel)
Total IR luminosity density vs redshiftobservations

IRUV

Well reproducedx5modelmodel

Data : Gruppioni+ 2013
Model

Dust: Draine & Li 2007

redshiftMitaka model (SAM) (Makiya et al. priv com) Top-heavy IMF in starburst is proposed to solve the discrepancy.

 Dust process (growth and destruction) needs to be correctly treated in simulations.

Key issues to be answered by SPICA
There are still significant discrepancies between observations andsimulations.

Key issues to be answered:(1) AGN contribution to IR luminosity at z~1-3→ To correctly estimate star-formation contribution to IR luminosity(2) Variations, if any, in IMF in IR-bright galaxies as a function of redshift→ To understand the discrepancy in IR luminosity density at z=1-3(3) Evolution of metallicity and dust as a function of redshift→ To understand the dust process in dusty IR bright galaxies correctly(4) Effects of AGN feedback on the star-formation as a function ofredshift→ To understand the decline of SFRD for z<1 and the GSMF

Observations of AGN feedback
To study quenching star formation, molecular outflow has to be investigated.
P Cygni profile of OH lines detected by Herschel/PACS unambiguously shows thepresence of molecular outflow of ~200 km/s. Multiple H lines for z = 0 – 2 &2OH

P Cyg profiles of CO (v = 1-0) lines
for z = 1.5-2.5 with SMI-HRS

CO v=1-0Extinction
H2S(9)
Spoon+ 2013 ApJ 775, 127

P Cyg profiles ofOH lines for z < 1.5with SAFARI

Gonzáles-Alfonso +2014
A&A, 561, A27

S(7)
S(5)

+

CO v=1-0 simulation
by Baba et al. priv. comm.

Multiple atomic & ionic lines with SAFARI & SMI

The first formation of mineral & organic matter
How were the first mineral & organic matter formed?
MIR & FIR targeted spectroscopy of high-z quasars & star-forming galaxies
High-z quasars (1x1013 L)－z=7－z=5SPICA (R=50, 10 hrs, 5σ)
R=300 with sensitivities,
5x10-20 W/m2 (1 hr, 5σ)

Flux (μJy)

silicate band

Flux (μJy)－ z = 10－z=6High-z star-forming galaxies (1x1013 L)

SPICA (R=50, 10 hrs, 5σ)
R=50 with sensitivities,
7x10-20 W/m2 (1 hr, 5σ)
JWST / MIRI
(R = 50, 10 hrs, 5σ)
204060 80 100
200
Wavelength (μm)

PAH bands
JWST / MIRI
(R = 50, 10 hrs, 5σ)
2040
60 80 100
Wavelength (μm)

200

 Detection of dust from z = 10 quasars. Only ~ 50 M dust is detectable,
thanks to high dust temperature.
 Study of all the bands of PAHs in z = 7 star-forming galaxies.
Not only detection, but also characterization of the first mineral & organic matter.

Observation plan
Targets observed by

Follow-up observations

AKARI, Subaru, Spitzer, Herschel, ALMA,JWST, Euclid, SKA, TMT, ATHENA, TESS, PLATO,,, high-z galaxies, AGN outflow,
nearby dwarf galaxies,,, proto-planetary disks, debris
disks, exo-planets,,,

Unbiased survey SMI-LRS(17-37 mm, R=50-100) + (34 mm R=5)
 10 deg2 blind survey (600 hrs)
Better statistics(51,000 PAH galaxies 3,700 AGNs 13,000 MS stars)

 1 deg2 blind survey(500 hrs)

Fainter objects(sub-L* galaxies, Debris disks with ~2 zodi)

SAFARI

SMI-HRS

SMI-MRSSPEChO

 Pointed spectroscopy
 Spectral mapping of nearbygalaxies
 Spectral mapping of Galacticobjects

SPICAプロジェクトの経緯
2007年度 大型衛星計画に提案。これまでのMロケットを用いた衛星の規模（中型衛星計画）を超えた、多くの分野が共同して支え、実施する、フラッグシップミッション。
2008年度 大型衛星計画としてミッション定義審査MDR 合格
以降プリプロジェクト発足
2010年度 大型衛星計画としてシステム要求審査SRR 合格
2011年度 中型衛星を超える規模ならば、宇宙科学の外側からの貢献（資金、人的体制）が必要
以降、リスク低減フェーズ
宇宙科学ロードマップ、大型は難しくなる
戦略的中型
コストオーバーラン問題
2014年度 PLAN-D（SPICA再定義） ESA-JAXA共同技術検討
2015年度 JAXA側：国際評価委員会、（ΔMDR＋SRR相当）審査、計画変更審査。 ESA側：2016年1月募集開始予想のM5に提案。
2013年度 PLAN-Bへの変更

Work-Sharing Plan
Telescope(ESA）

Focal Plane Instrument Assembly
FIR Spectrometer（SAFARI）

Payload Module

NL + European countries+ Canada & US

Cryocooler
MIR Instrument （SMI）
Bus Module

Launcher
SPICA Data Center(NAOJ)

Exoplanet Spectroscopy（SPEChO）

Focal Plane Attitude Sensor

UK & European countries

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

19

まとめ 赤外線分光による「銀河成長・物質進化過程」とO
H O
D HH H
Mg Si O
「惑星系形成過程」の解明
HOO

 望遠鏡口径2.5 m, 温度8 K, 2027-2028年打ち上げ
2030

40

 JAXA-ESA共同ミッション。
JAXA審査：今夏、ESA: 来年1月C-V proposal call予定 コア波長：17-210 mm、ライン感度：～5x10-20 W/m2
・ 17-37 mm低分散分光撮像 ＋ 34 mm広帯域撮像
・ 高分散 12-18 mm, ～2x10-20 W/m2
(1) 遠赤外線装置SAFARI（欧州） SAFARI, R=300, 3000
(2) 中間赤外線装置SMI（日本、大学）, R=50, 1000, 25000(3) 系外惑星トランジット分光器（UK） SPEChO
HRS

17.2 17.3

ひきつづきのご支援・ご協力をよろしくお願いいたします。

2040λ (μm)

60121416λ (μm)

18

Most important: very low IR background

KSPICA105 reduction !

8 K (SPICA)