FMOS meeting Kyoto 13 140104 Panoramic Imaging and

FMOS meeting (Kyoto, 13 -14/01/04) Panoramic Imaging and Spectroscopy of Cluster Evolution with Subaru (PISCES) PI: Taddy Kodama (NAOJ) Arimoto, Futamase, Iye, Karasawa, Kashikawa, Kawasaki, Kitayama, Matsuhara, Nagashima, Nakata, Ohashi, Ohta, Okamoto, Okamura, Shimasaku, Suto, Tamura, Tanaka I. , Tanaka M. , Umetsu, Yahagi, and Yamada Thirsty?

What’s PISCES ? Panoramic Imaging of 15 Clusters at 0. 4<z<1. 3 with Suprime-Cam (optical, 30’ = 10 -14 Mpc) n Spectroscopic Follow-up with FOCAS (optical, 6’) and FMOS (NIR, 30’) along the Structures Mapping Large Scale Structure in and around Clusters Cluster Assembly and Spatial Bias Environmental Variation of Galaxy Properties n

Cluster Assembly and Galaxy Evolution N-body simulation (Dark matter) Colour-Magnitude Relation Terlevich et al. Density-Morphology Relation Sp Moore et al. S 0 E Dressler et al.

Cluster Sample 15 X-ray selected clusters at 0. 4<z<1. 3

RX J 0152. 71357 (z=0. 83) central 3’ x 3’ (outof 34’x 27’) Suprime. Cam V : 120 min R : 116 min i’ : 75 min z’ : 79 min

Panoramic View of Cluster Assembly CL 0939+47 CL 0016+16 RX J 0153－14 z=0. 41 (4. 3 Gyr ago) z=0. 55 (5. 4 Gyr ago) z=0. 83 (7. 0 Gyr ago) 30 arcmin = 10, 12, and 14 Mpc, respectively contours: 1. 5, 2, 3, 4, 5 sigma

Mapping the Three Major Components of Matter in Cluster Dark Matter (weak-lensing) XMM) Galaxies (photometric-redshift) RX J 0152. 7 -1357 (z=0. 83), Hot Gas (x-ray; 7 arcmin = 3. 2

Environmental Effects “a priori” or “a posteriori”

Galaxy Transition in CL 0939 Cluster (z=0. 4) Suprime-Cam + BVRI critical density Galaxies start to be truncated at relatively low density (groups) Kodama et al. (2001)

FMOS roles for PISCES ~~~ Hα measurements over a large Fo. V ~~~ Hα comes to FMOS window for 0. 4<z<1. 7 ! Radial Velocities Physical Associations of Substructures, 3 -D Structures, Recent Merger Histories n Star Formation Rates Less affected by Dust and Metallicity. Resolving the Recent Star Formation Histories n

Velocity Structures Velocity Clump ~300 spectra across 8 Mpc (25’) around CL 0024 cluster (z=0. 395) A high-speed line-of-sight collision? Radius Czoske et al. (2002)

Hα Mapping of CL 0024 Cluster (z=0. 4) Suprime-Cam + BRz’ and NB 912 Hα LF Kodama, Balogh, et al. (2004) Hα intensity is a good measure of on-going star formation rate

Global Star Formation History in Clusters (Cluster counterpart of the Madau plot) SFR (z) SFR (σ) This work Kodama, Balogh et al. (2004)

Starburst/Post-starburst Galaxies Spectral classification k Spectral indices g-r k+a Hδ a+k e(a) OII e(c) Burst active Age (Gyr) Poggianti et al. (1999) Dressler et al. (1999) Resolving Recent SF Histories

Dusty Starburst Radio (VLA), 1. 4 GHz OII k+a Hα+NII a+k k+a Poggianti et al. 1999 Smail et al. 1999 Hα is a better tracer for on-going star formation activities

Down-sizing in Galaxy Formation z~1 passive galaxies in the Subaru/XMM Deep Field (1. 2 sq deg) Field corrected CM diagram for z~1 galaxies down to M*+3 Deficit! Galaxy Formation is Down-sizing! Kodama et al. (2004)

From Distant Clusters to the Present-day Clusters z=0. 43 0. 33 0. 23 0. 0 Global SF History Madau plot Taddy plot! Evolution Assembly Kodama & Bower (2001)

Summary FMOS will be an exellent facility for widefield studies of distant clusters through Hα line. n PISCES will provide panoramic views of hierarchical growth of clusters through assembly and galaxy evolution therein since the Universe was only 1/3 of its present age. n Combining with the up-coming wide-field NIR imagers such as WFCAM (UKIRT, 30’) and MOIRCS (Subaru, 4’x 7’), we will be able to extend such studies to z~1. 7 (Hα) and far beyond (OII). n