f d l f l hSpace Infrared Telescope for Cosmology & Astrophysics

SPICA: C t St t & SSPICA: Current Status & Synergy with Large mm/submm TelescopeLarge Aperture Millimeter/Submillimeter Telescopes in

with Large mm/submm TelescopeLarge Aperture Millimeter/Submillimeter Telescopes in the ALMA Era 2011/9/12-13

Hideo Matsuhara, on behalf of SPICA preproject and Science Working GroupI tit t f S & A t ti l S iInstitute of Space & Astronautical ScienceJapan Aerospace Exploration Agency

List of My TalkList of My Talk

SPICA Mi i O i SPICA Mission Overview Current Status Synergy with Large Aperture mm/submm Synergy with Large Aperture mm/submm

telescope (hereafter ASTE-II according to Kawbe-san) and CCAT)

CRYO

FPIA

STA

SIA

SPICA: Next-Generation IR Space Observatory at Sun-Earth L2 point –1 5 million km away from us1.5 million km away from us

L4L4

L1 L2L3

Sun Earth

L5

SPICA Mission OverviewSPICA Mission Overview Telescope: 3 2m (EPD 3 0m) 6 K Telescope: 3.2m (EPD 3.0m), 6 K

Superior Sensitivity Good spatial resolutionp

Core wavelength: 5-210 μm MIR Instrument Far Infrared Instrument (SAFARI) Far-Infrared Instrument (SAFARI)

Orbit: Sun-Earth L2 Halo Mission Life

L4 3 years (nominal) 5 years (goal)

Weight: 3 7 tSun

L1 L2

Earth

L3

Weight: 3.7 t Launch: FY2018 (original plan) International mission

L5 Japan, Europe, USA, Korea, (Taiwan)

Where are we from?Where are we from?

Metal elements, fundamental constituent of our world, are formed in the Stars,

Transmigration of ISMGas & Dust

Interstellar Gas(birth place)

How the mass ejection related

stellar evolution?

How the mass ejection related

stellar evolution?Can SNe form dust or destruct

only?

Can SNe form dust or destruct

only?

5

Birth of StarsHeavy element production

Death of StarsMass Loss, SNe, Dust production / destruction

only?only?

Our Science GoalsHow did the Universe originate and

Our Science GoalsHow did the Universe originate and what is it made of?What are the conditions for stellar and planetary formation ?planetary formation ?

Most Important Requirements: C l d L T l !Cooled Large Telescope !

Background will be 1 million times smaller than the warm (passively cooled ) telescope !!

Revolution of Design Philosophye o ut o o es g osop y

AKARI:Scientific Instruments: 42 kgScientific Instruments: 42 kgCoolong system 460 kg

Cryostat shell dominated: 200 kg200 kg170 litters liq. He limits life

Make it light !

Key challenge -- Cooling systemM h i l C l f 4 5K2ST冷凍機

2ST冷凍機1K-JT冷凍機Mechanical 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

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

2ST冷凍機

Sorption cooler + ADR 50mK

Huge Gain of Sensitivity !Huge Gain of Sensitivity !Photometry Spectroscopy

Herschel

p py

HerschelSpitzer

1 5 orders

Herschel

2.5 orders

SPICA SPICA

1.5 orders

JWST

ALMA

JWST

Huge Gain of Mapping SpeedHuge Gain of Mapping Speed

Gain of 103 !Gain of 103 !

Mapping a full 2x2 arcmin field covering the full wavelengthSPICA/ covering the full wavelength

range

SPICA/SAFARI

SPICA

Focal Plane InstrumentsMid-IR Camera and Spectrometer (MCS)SPICA Coronagraph Instrument(SCI)SPICA Far-IR Instrument (SAFARI) European Consortium

Herschel

SPICA Far IR Instrument (SAFARI)Focal Plane Camera (Guider, Science) FPCUS proposed Instrument

European ConsortiumKorea

US

λ/δλ (δv)

10000 SPICAMCS/HRS

1000

10000(30 km s-1)

JWST

SPICA

MCS/MRS

λ100

(300 km s-1)BLISS

SCI SAFARI

MCS/MRS

(3000 km s-1) FPC-SSAFARI

MCS/WFC/LRS

2 μm 20 μm 200 μmWavelength

Wavelength coverage vs Resolving Power

Field-of Views(with preliminary pick-off for US instrument)(with preliminary pick-off for US instrument)

US Instrument pick-off (tbd)

MCS/WFC-S MCS/WFC-L5’x5’5’x5’ 5 x5

MCS/LRS

MCS/HRS MCS/MRS

Updated on 17th May, 2011

SPICA Project Status (1)SPICA Project Status (1) 2007: Mission proposals to ESA & JAXAp p

Selected as “Mission of Opportunity” in ESA cosmic vision, starting Assessment Study by ESA

2008: Preproject established at JAXAp j 2008： Opt-IR community: SPICA taskforce established

Defines the SPICA Mission Requirement Document Call for Focal Instrument proposals Undertook the Domestic Call for Focal Instrument proposals, Undertook the Domestic

Review 2010/09： System Requirement Review (SRR) by

JAXA/SSSC was successful!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 thenext steps to System Definition Review (SDR) and the successive phase-up review

Detailed Design / technical development ongoing for the risk mitigation before the project phasemitigation before the project phase

Focal Plane Instrument: International Review is ongoing in order to define the instruments / functions onboard

SPICA Project Status (2)SPICA Project Status (2) Europe (ESA) 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 (N th l d ) PI 14 b t i SRON (Netherlands) PI, 14 member countries

Dedicated team has been working actively

Korea 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)ASTE-II & CCAT(1)

S S ti l R l i Same Spatial Resolving power Diffraction limited beam size of

SPICA/SAFARI @ 35-210μm = beam size of 30m ASTE-II @ 350 μm-

2.1mmWavelength coverageg g

SAFARI: upto 210μm, ~400μm in case of US instrument onboard

With 30m ASTE-II, similar sensitivity with SPICA (3m space) can be expected at ( p ) p400μm, 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 Coordination between SPICA & 30m ASTE II & CCAT is critically

important!

ASTE-II CCAT SPICA PresentASTE-II , CCAT SPICA Present8.5Gyr ago

SPICAASTE-II , CCAT

12.4Gyr ago

SPICA

< Originally Kohno-san’s slide >

ASTE-II , CCAT

Power of SPICA：Deep M lti object spectrograph

Si lt 34 210 t

Deep Multi-object spectrographCourtesy to SAFARI consortium

Simultaneous 34-210 μm spectroscopy

Ordially follow-up：

2 x 2 arcmin2 FoV

One-by-one spectroscopy

a c o unbiased spectroscopy of multiple sources redshift? energy source diagnostics.

The first cosmological t ispectroscopic survey

~1 degr ee

900 hoursOf Obs

SPICA /SAFARI

Of Obs.

Herschel PACSGain of 103 !103 !

19Image Springel et al. 2006

Power of SPICA’s imaging bilitcapability

AKARI SPICA (Mid IR simulation)Mid-IR deep survey

SPICA (Mid-IR, simulation)

Courtesy to Ko Arimatsu @U. Tokyo

Complementarities (2)t f ASTE II & CCAT-- 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 20-210μm imaging survey,

and ~1 deg2 35-210μm 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. ]d f b d b d t t-- need of broad-band spectrometer --

Dust Obscured Cosmic Star Formation History Dust Obscured Cosmic Star-Formation History For physical condition & metalicity diagnostics of

d t b d l i (i bl t bdust obscured galaxies (i.e. unable to observe even with TMT), wavelength covered by SPICA is not sufficient (ex redshifted [CII] 158μm [NII] 205μmsufficient (ex. redshifted [CII] 158μm, [NII] 205μm lines)

Broad band submm (multi object) spectrometer!! Broad-band submm (multi-object) spectrometer!!Broadband RX / grating spectrograph (Z-Spec, ZEUS)

Redshift identification at Far IR or submm not at Redshift identification at Far-IR or submm, not at optical / near-IR. Submm galaxies are likely to be gravitationally lensed by foreground optical/near-IRgravitationally lensed by foreground optical/near IR galaxies.

Z-Spec: Millimeter-wave broad band spectrometer (1)p ( )gravitationlly lensed bright submm galaxies

CO redshift z=3.04determined for H-ATLAS ID 81 bli d d t i tiID 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 d t t d f l l di AGNdetected from warm molecular gas surrounding AGNAPM 98279+5255 at z=3.91 Bradford et al. (2011)

NASA lNASA press release on 22nd July

Complementarities (3)G l ti S i / D b i Di kGalactic Science / Debris Disks

Solid State Science with Galactic & nearby galaxies’ 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.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 dusttemperature 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

1.2 Resolving Snow Line0.6

0.8

1

kg

Crystalline

H2O ice is expected to play a

0

0.2

0.4 Amorphous H2O ice is expected to play a

crucial role in planetary formation Giant planets vs terrestrial

0 50 100 150 200

WavelengthMalfait et al. 1999

pplanets

Resolution to image “snowlines” in local systems26

Su et al. 2005

SummarySummary

SPICA i l d (<6K) l t SPICA is a cooled (<6K), large-aperture (3.2m) telescope with overwhelmingly high sensitivity in the mid- and far-infraredsensitivity in the mid- and far-infrared Cooled to <6K is mandatory, hence challenging Risk mitigation in the current phase is quite Risk mitigation in the current phase is quite

important Synergy with 30-50m ASTE-II and CCATy gy

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