Space Infrared Telescope for Cosmology & Astrophysics
SPICA: Current Status & Synergy
with Large mm/submm Telescope
Large Aperture Millimeter/Submillimeter Telescopes in
the ALMA Era 2011/9/12-13
Hideo Matsuhara, on behalf of SPICA preproject and
Science Working Group
Institute of Space & Astronautical Science
Japan Aerospace Exploration Agency
List of My Talk

SPICA Mission Overview
 Current Status
 Synergy with Large Aperture mm/submm
telescope (hereafter ASTE-II according to
Kawbe-san) and CCAT
CRYO
STA
SIA
FPIA
SPICA: Next-Generation IR Space
Observatory at Sun-Earth L2 point –
1.5 million km away from us
SPICA Mission Overview

Telescope: 3.2m (EPD 3.0m), 6 K

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Core wavelength: 5-210 μm




MIR Instrument
Far-Infrared Instrument (SAFARI)
Orbit: Sun-Earth L2 Halo
Mission Life


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Superior Sensitivity
Good spatial resolution
3 years (nominal)
5 years (goal)
Weight: 3.7 t
Launch: FY2018 (original plan)
International mission

Japan, Europe, USA, Korea, (Taiwan)
Where are we from?

Metal elements, fundamental constituent
of our world, are formed in the Stars
Transmigration of ISM
Gas & Dust
How the mass
ejection related
stellar evolution?
Can SNe form
dust or destruct
only?
Interstellar Gas
(birth place)
Death of Stars
Mass Loss, SNe, Dust
production / destruction
Birth of Stars
Heavy element production
5
Our Science Goals
How did the Universe originate and
what is it made of?
What are the conditions for stellar and
planetary formation ?
Most Important Requirements:
Cooled Large Telescope !
Background will be 1 million times smaller than the warm
(passively cooled ) telescope !!
Revolution of Design Philosophy
AKARI:
Scientific Instruments: 42 kg
Coolong system 460 kg
Cryostat shell dominated:
200 kg
170 litters liq. He limits life
Make it light !
Key challenge -- Cooling system
1K-JT冷凍機
コンプレッサ
2ST冷凍機
2ST冷凍機
1K-JT冷凍機
コンプレッサ
4K-JT冷凍機
コンプレッサ
2ST冷凍機
2ST冷凍機
4K-JT冷凍機
コンプレッサ
Sorption cooler +
ADR
50mK
 Mechanical
Cooler for 4.5K
and 1.7K (J-T & 2ST)
 50mK ADR
Huge Gain of Sensitivity !
Photometry
Spectroscopy
Herschel
Spitzer
Herschel
1.5 orders
2.5 orders
SPICA
SPICA
ALMA
JWST
Huge Gain of Mapping Speed
Gain of 103 !
Mapping a full 2x2 arcmin field
covering the full wavelength
SPICA/
SAFARI
range
SPICA
Focal Plane Instruments
 Mid-IR
Camera and Spectrometer (MCS)
 SPICA Coronagraph Instrument(SCI)
 SPICA Far-IR Instrument (SAFARI) European Consortium
 Focal Plane Camera (Guider, Science) FPC
Korea
US
 US proposed Instrument
Herschel
l/dl (dv)
MCS/HRS
10000
(30 km s-1)
1000
(300 km s-1)
100
(3000 km s-1)
SPICA
JWST
MCS/MRS
BLISS
SCI
FPC-S
2 mm
SAFARI
MCS/WFC/LRS
20 mm
Wavelength
Wavelength coverage vs Resolving Power
200 mm
λ
Field-of Views
(with preliminary pick-off for US instrument)
US Instrument pick-off (tbd)
MCS/WFC-L
5’x5’
MCS/LRS
MCS/WFC-S
5’x5’
MCS/HRS
MCS/MRS
Updated on 17th May, 2011
SPICA Project Status (1)

2007: Mission proposals to ESA & JAXA

Selected as “Mission of Opportunity” in ESA cosmic vision,
starting Assessment Study by ESA
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2008: Preproject established at JAXA
 2008： Opt-IR community: SPICA taskforce established

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Defines the SPICA Mission Requirement Document
Call for Focal Instrument proposals, Undertook the Domestic
Review

2010/09： System Requirement Review (SRR) by
JAXA/SSSC was successful!
 After SRR:

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Discussions are on-going in JAXA/SSSC in order to proceed
next steps to System Definition Review (SDR) and the
successive phase-up review
Detailed Design / technical development ongoing for the risk
mitigation before the project phase
Focal Plane Instrument: International Review is ongoing in
order to define the instruments / functions onboard
SPICA Project Status (2)

Europe (ESA)
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Responsible to the Telescope Assembly, & ground segment
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SRON (Netherlands) PI, 14 member countries
Dedicated team has been working actively
Korea
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Studies under the frame work of ESA Cosmic Vision
Europe (SAFARI)
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Concept study of the telescope is ongoing by two industries
Official Study Team formed with KASI as PI, collaborating with
SNU & Satrec etc.
Responsible for the FPC (guider and science)
US Status
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Assessment Study by 3 teams funded by NASA in 2010
Strong recommendation in the US Decadal Survey in 2010
Complementarities with
ASTE-II & CCAT(1)
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Same Spatial Resolving power

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Diffraction limited beam size of
SPICA/SAFARI @ 35-210mm
= beam size of 30m ASTE-II @ 350 mm2.1mm
Wavelength coverage
SAFARI: upto 210mm, ~400mm in case of
US instrument onboard
 With 30m ASTE-II, similar sensitivity with
SPICA (3m space) can be expected at
400mm, much deeper at 1mm (..tbc!!)

Systematic survey of rest-mid and far-IR fine structure lines
 Coordination between SPICA & 30m ASTE-II & CCAT is critically
important!
ASTE-II , CCAT
ASTE-II , CCAT
ASTE-II , CCAT
< Originally Kohno-san’s slide >
SPICA
Present
8.5Gyr ago
SPICA
SPICA
12.4Gyr ago
Power of SPICA：
Deep Multi-object spectrograph
Courtesy to SAFARI consortium
Simultaneous 34-210 μm spectroscopy
Ordially follow-up：
One-by-one spectroscopy
2 x 2 arcmin2 FoV
 unbiased spectroscopy of multiple sources
 redshift? energy source diagnostics.
The first cosmological
spectroscopic survey
~1 degree
900 hours
Of Obs.
SPICA /SAFARI
Gain of
103 !
Herschel PACS
19
Image Springel et al. 2006
Power of SPICA’s imaging
capability
AKARI
Mid-IR deep survey
SPICA (Mid-IR, simulation)
Courtesy to Ko Arimatsu @U. Tokyo
Complementarities (2)
-- request for ASTE-II & CCAT -
SPICA’s Field-of-View / Survey (Mapping)
Speed

Survey with SAFARI: 2x2 arcmin2, MCS-WFC:
5x5 arcmin2 can provide:
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10-100 deg2 multi-color 20-210mm imaging survey,
and
~1 deg2 35-210mm spectral image (R~1000)
ASTE-II is requested to be equipped with:

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Large-format (similar to SPICA/SAFARI)
submm multi-band camera
And (multi-object) broad-band spectrometer..
Complementarities (2) [cont. ]
-- need of broad-band spectrometer

--
Dust Obscured Cosmic Star-Formation History
For physical condition & metalicity diagnostics of
dust obscured galaxies (i.e. unable to observe even
with TMT), wavelength covered by SPICA is not
sufficient (ex. redshifted [CII] 158mm, [NII] 205mm
lines)
 Broad-band submm (multi-object) spectrometer!!

 Broadband

RX / grating spectrograph (Z-Spec, ZEUS)
Redshift identification at Far-IR or submm, not at
optical / near-IR. Submm galaxies are likely to be
gravitationally lensed by foreground optical/near-IR
galaxies.
Z-Spec: Millimeter-wave broad band
spectrometer (1)
gravitationlly lensed bright submm galaxies
CO redshift z=3.04
determined for H-ATLAS
ID 81, blind determination
Z-Spec/ CSO
Negrello et al. (2010)
Z-Spec (2): Water Vapor Detection from
Quaser at 12 Gyr ago
Rotational transitions of Water vapor molecules are
detected from warm molecular gas surrounding AGN
APM 98279+5255 at z=3.91
Bradford et al. (2011)
NASA press release
on 22nd July
Complementarities (3)
Galactic Science / Debris Disks

Solid State Science with Galactic & nearby galaxies’
SFR

With SPICA over a few arcsec – arcmin scale,

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Composition, ionization of dust, at different environment
Emission from dust newly formed by SNe
can be done over a few 100 nearby galaxies.
 Need of submm wide-field camera with ASTE-II (same
spatial resolution as SPICA!!) to determine the lowtemperature component, and obtain total amount of dust

Debris Disks
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SPICA can resolve the Snow Line!
ALMA (FoV 20”) is not easy to cover the entire
distribution of matter. Wide-field submm camera is quite
complementary
Resolving Snow Line
1.4
1.2
1
Crystalline
k
0.8
0.6
Amorphous
0.4

0.2
0
0
50
Malfait et al. 1999
100
150
Wavelength
200
250
H2O ice is expected to play a
crucial role in planetary formation
 Giant planets vs terrestrial
planets
Su et al. 2005
26
Resolution to image “snowlines” in local systems
Summary

SPICA is a cooled (<6K), large-aperture
(3.2m) telescope with overwhelmingly high
sensitivity in the mid- and far-infrared

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Synergy with 30-50m ASTE-II and CCAT
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Cooled to <6K is mandatory, hence challenging
Risk mitigation in the current phase is quite
important
Same Spatial Resolving power
Complementary wavelength coverage
ASTE-II and CCAT should be equipped
with


submm multi-color wide-field camera
Broad-band (multi-object) spectrometer