SPICA:現状および観測制約について
Download
Report
Transcript SPICA:現状および観測制約について
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
Core wavelength: 5-210 μm
MIR Instrument
Far-Infrared Instrument (SAFARI)
Orbit: Sun-Earth L2 Halo
Mission Life
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
2008: Preproject established at JAXA
2008: Opt-IR community: SPICA taskforce established
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:
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)
Responsible to the Telescope Assembly, & ground segment
SRON (Netherlands) PI, 14 member countries
Dedicated team has been working actively
Korea
Studies under the frame work of ESA Cosmic Vision
Europe (SAFARI)
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
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)
Same Spatial Resolving power
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:
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:
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,
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
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
Synergy with 30-50m ASTE-II and CCAT
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