Oct.10, 2007 EAMA7

Synergy with Thirty Meter Telescope

The next-generationInfrared astronomy mission

SPICA

Space Infrared Telescope for Cosmology & Astrophysics

Gopira Symposium 2009 (October 21-22, 2009) @ NAOJ Mitaka

H. Matsuhara (ISAS/JAXA) , Takuya Yamashita (NAOJ)SPICA pre-project / SPICA task-force / SPICA Science Working Group

How did the Universe originate and what is it made of ? What are the conditions for stellar and planetary formation ?How did the universe evolve chemically ? The emergence of life ?

Ｏｕｒ Ｓｃｉｅｎｔｉｆｉｃ Goals

SPICA Overview

COOLED (<6K) Space telescope3-m class monolithic primary mirror diffraction limited at 5m

Space Observatory mission, for mid- & far-IR astronomy (core 5-210m)

JAXA – ESA(Cosmic Vision M-class candidate) Mission, with planned participation from Korea & US Orbit: Sun-Earth L2 Halo Mission Life: 3 years (nominal) 5 years (goal) Launch: 2018 (H-IIA)

Sensitivity for spectral lines (1 hour, 5)

BLISS (optional)

IRSx0.1

5

Imaging Spectroscopy R~100, 1hr

Broad-band Imaging10 min (!) Imaging, 1hr

JWST /MIRI Confusion limit (3m aperture)

Flux Limit in 5(Jy)

Uniqueness of SPICA

Overwhelming Imaging Sensitivity at 20-100 m (MIRACLE, SAFARI) Overwhelming mapping speed !! MIRACLE should have large FoV as much as

possible (at least 4’x4’)

Capability of spectro-imaging at 35-210m (SAFARI, 2’x2’ FoV)

Overwhelming Spectroscopic sensitivity at 20 – 400 m (MIRMES, SAFARI, BLISS)

High-dispersion spectroscopy at 4-8, 12-18m

Example of Key Sciences with SPICA:

Metallicity Evolution at 0 < z < 3?

Maiolino, Nagao, et al. (2008)

Chemical Version of the “Down-Sizing” seen in Mass – Metallicity relation

Possible caveat: selection bias ~ using “rest-frame optical” diagnostics observing only “un-obscured” galaxies ~ how about “obscured” galaxies??

Courtesy to Tohru Nagao (Ehime U.)

Method : Diagnostics with FIR line ratio metallicity diagnostics physical properties

Very limited work is possible with ISO dataStill low-z samples can be done with Herschel

Data: Colbert+99, Unger+00, Fischer+96, Spinoglio+05

Nagao, et al., in prep.

SAFARI GOAL

BLISS

• [NIII] 57m– M82 (dwarf SB) :

detectable out to z~1 with BLISS

– ULIRGs are detectable out to z~2 with SAFARI

Feasibility

SPICA’s probe for re-ionization Era (z~10) in Synergy with TMT & JWST

Probes free from the confusion limitPAH EmitterCosmic Far-IR Background Fluctuations Gravitational lens H2 emitter

Dust-obscured hyper-luminous AGN Dust-cocooned GRB afterglow

Evidence of Formation of dust / metals in the re-ionization eraULIRGs at z~10 : if exit, how they are related to the 1st stars?

Strong PAH emitter search upto z~10

• 7.7um PAH luminosity of z~2 SMGs: ~5e1010 L for the most luminous ones (Pope et al. 2008) Requires a flux sensitivity of ~10-19 Wm-2 to detect up to z~10 @ R~20 is enough with SAFARI

• Blank Field Survey with SAFARI• Targeted Spectroscopy with BLISS

z~2 SMG(Pope+ 2008)

PAH luminous galaxies @z=0.6

Courtesy to Eiichi Egami (U. Arizona)

Cosmic Infrared Background Excess emissions which cannot be nearby galaxies• Proto-galaxies (e.g. pop-III stars, mini-quasars) at z~10?• Measuring the anisotropy is powerful to identify them.

If substantial fraction of the energy of the NIR background is converted to dust emissions (IGM dusts, mini-quasars(AGN), etc.), it may form the far-infrared background.

Courtesy to Shuji Matsuura (ISAS, JAXA)

SPICA SHALL UNVEIL INVISIBLE UNIVERSE OBSCURED BY DUST

Key Words expressing SPICA Mission Objective..

1ST METALS IN EARLY UNIVERSECOSMIC SFH/BHGHORIGIN OF OUR SOLAR SYSTEM

WHAT IS ESSENTIAL IS INVISIBLE TO THE EYE, BUT VISIBLE TO SPICA’S HEART

大切なものは目で見えないんだよ。l'essentiel est invisible pour les yeux