Oct.10, 2007EAMA7 Synergy with Thirty Meter Telescope The next-generation Infrared astronomy mission SPICA Space Infrared Telescope for Cosmology & Astrophysics Gopira Symposium 2009 (October 21-22, 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 telescope 3-m class monolithic primary mirror diffraction limited at 5  m Space Observatory mission, for mid- & far- IR astronomy (core  m) 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 Imaging 10 min (!) Imaging, 1hr JWST /MIRI Confusion limit (3m aperture) Flux Limit in 5  (Jy)

Uniqueness of SPICA Overwhelming Imaging Sensitivity at  m (MIRACLE, SAFARI) Overwhelming mapping speed !! MIRACLE should have large FoV as much as possible (at least 4’x4’) Capability of spectro-imaging at  m (SAFARI, 2’x2’ FoV) Overwhelming Spectroscopic sensitivity at 20 – 400  m (MIRMES, SAFARI, BLISS) High-dispersion spectroscopy at 4-8,  m

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 data Still 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] 57  m – 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 limit PAH Emitter Cosmic Far-IR Background Fluctuations Gravitational lens H 2 emitter Dust-obscured hyper-luminous AGN Dust-cocooned GRB afterglow Evidence of Formation of dust / metals in the re-ionization era ULIRGs at z~10 : if exit, how they are related to the 1 st stars?

Strong PAH emitter search upto z~10 7.7um PAH luminosity of z~2 SMGs: ~5e10 10 L  for the most luminous ones (Pope et al. 2008)  Requires a flux sensitivity of ~ Wm -2 to detect up to R~20 is enough with SAFARI Blank Field Survey with SAFARI Targeted Spectroscopy with BLISS z~2 SMG (Pope+ 2008) PAH luminous 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.. 1 ST METALS IN EARLY UNIVERSE COSMIC SFH/BHGH ORIGIN 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