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Large Aperture Millimeter/Submillimeter Telescopes in the ALMA Era 2011/9/12-13
Hideo Matsuhara, on behalf of SPICA preproject and Science Working GroupInstitute of Space & Astronautical ScienceJapan Aerospace Exploration Agency
Space Infrared Telescope for Cosmology & Astrophysics
SPICA: Current Status & Synergy with Large mm/submm Telescope
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
FPIA
STA
CRYO
SIA
SPICA: Next-Generation IR Space Observatory at Sun-Earth L2 point – 1.5 million km away from us
Sun
L1 L2
L4
L5
Earth
L3
Sun
L1 L2
L4
L5
Earth
L3
SPICA Mission Overview
Telescope: 3.2m (EPD 3.0m), 6 K Superior Sensitivity Good spatial resolution
Core wavelength: 5-210 μm MIR Instrument Far-Infrared Instrument (SAFARI)
Orbit: Sun-Earth L2 Halo Mission Life
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
5
Birth of StarsHeavy element production
Interstellar Gas(birth place)
Death of StarsMass Loss, SNe, Dust production / destruction
Gas & Dust
Transmigration of ISM
How the mass ejection related
stellar evolution?Can SNe form
dust or destruct only?
How the mass ejection related
stellar evolution?Can SNe form
dust or destruct only?
How did the Universe originate and what is it made of?What are the conditions for stellar and planetary formation ?
Our Science Goals
Most Important Requirements: Cooled Large Telescope !
Background will be 1 million times smaller than the warm (passively cooled ) telescope !!
Revolution of Design Philosophy
Make it light !
AKARI:Scientific Instruments: 42 kgCoolong system 460 kg
Cryostat shell dominated: 200 kg170 litters liq. He limits life
Key challenge -- Cooling systemMechanical Cooler for 4.5K
and 1.7K (J-T & 2ST)50mK ADR
2ST 冷凍機
1K-JT 冷凍機コンプレッサ
2ST 冷凍機 4K-JT 冷凍機コンプレッサ
2ST 冷凍機1K-JT 冷凍機コンプレッサ
2ST 冷凍機
4K-JT 冷凍機コンプレッサ
Sorption cooler + ADR 50mK
Huge Gain of Sensitivity !
2.5 orders
SPICASPICA
1.5 orders
Herschel
Photometry Spectroscopy
HerschelSpitzer
JWST
ALMA
Huge Gain of Mapping Speed
SPICA
Mapping a full 2x2 arcmin field covering the full wavelength range
Gain of 103 !
SPICA/SAFARI
Focal Plane Instruments
λ
v
2 m 20 m 200 m
100(3000 km s-1)
1000(300 km s-1)
10000(30 km s-1)
Herschel
JWST
SPICA
FPC-S
BLISS
MCS/HRS
SCISAFARI
MCS/WFC/LRS
MCS/MRS
Wavelength
Mid-IR Camera and Spectrometer (MCS)SPICA Coronagraph Instrument(SCI)SPICA Far-IR Instrument (SAFARI)Focal Plane Camera (Guider, Science) FPCUS proposed Instrument
Wavelength coverage vs Resolving Power
European Consortium
Korea
US
US Instrument pick-off (tbd)
Updated on 17th May, 2011
Field-of Views (with preliminary pick-off for US instrument)
MCS/WFC-S5’x5’
MCS/HRS MCS/MRS
MCS/WFC-L5’x5’
MCS/LRS
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
Concept study of the telescope is ongoing by two industries
Studies under the frame work of ESA Cosmic Vision
Europe (SAFARI) SRON (Netherlands) PI, 14 member countries Dedicated team has been working actively
Korea 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 powerDiffraction limited beam size of
SPICA/SAFARI @ 35-210m = beam size of 30m ASTE-II @ 350m-
2.1mmWavelength coverage
SAFARI: upto 210m, ~400m in case of US instrument onboard
With 30m ASTE-II, similar sensitivity with SPICA (3m space) can be expected at 400m, 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 SPICA Present 8.5Gyr ago
12.4Gyr ago
SPICA
SPICA
< Originally Kohno-san’s slide >
ASTE-II , CCAT
ASTE-II , CCAT
Simultaneous 34-210 μm spectroscopy
Power of SPICA :Deep Multi-object spectrograph
2 x 2 arcmin2 FoV unbiased spectroscopy of multiple sources
redshift? energy source diagnostics.
Ordially follow-up :One-by-one spectroscopy
Courtesy to SAFARI consortium
19
The first cosmological spectroscopic survey
~1 degree
~1 degree
Image Springel et al. 2006
SPICA /SAFARI
Herschel PACS
900 hoursOf Obs.
Gain of 103 !
Power of SPICA’s imaging capability
AKARIMid-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 20-210m imaging survey,
and ~1 deg2 35-210m 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] 158m, [NII] 205m 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.
CO redshift z=3.04 determined for H-ATLAS ID 81, blind determination
Z-Spec/ CSO
Negrello et al. (2010)
Z-Spec: Millimeter-wave broad band spectrometer (1)gravitationlly lensed bright submm galaxies
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 low-temperature 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
Resolution to image “snowlines” in local systems
0
0.2
0.4
0.6
0.8
1
1.2
1.4
0 50 100 150 200 250
Wavelength
k
26
Resolving Snow LineCrystalline
Amorphous
Malfait et al. 1999
Su et al. 2005
H2O ice is expected to play a crucial role in planetary formation Giant planets vs terrestrial
planets
Summary
SPICA is a cooled (<6K), large-aperture (3.2m) telescope with overwhelmingly high sensitivity in the mid- and far-infrared Cooled to <6K is mandatory, hence challenging Risk mitigation in the current phase is quite
importantSynergy with 30-50m ASTE-II and CCAT
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