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

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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

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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