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P anoramic I maging and S pectroscopy of C luster E volution with S ubaru ( PISCES )

FMOS meeting (Kyoto, 13-14/01/04). P anoramic I maging and S pectroscopy of C luster E volution with S ubaru ( PISCES ). PI: Taddy Kodama (NAOJ).

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P anoramic I maging and S pectroscopy of C luster E volution with S ubaru ( PISCES )

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  1. 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?

  2. What’s PISCES ? • Panoramic Imaging of 15 Clusters at 0.4<z<1.3 with Suprime-Cam (optical, 30’ = 10-14 Mpc) • 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 Origin of Density-Morphology-SFR Relation

  3. Cluster Assembly and Galaxy Evolution N-body simulation (Dark matter) Colour-Magnitude Relation Terlevich et al. Density-Morphology Relation Sp S0 E Moore et al. Dressler et al.

  4. Cluster Sample 15 X-ray selected clusters at 0.4<z<1.3

  5. RX J0152.7-1357 (z=0.83) central 3’ x 3’ (outof 34’x27’) Suprime-Cam V : 120 min R : 116 min i’ : 75 min z’ : 79 min

  6. Panoramic View of Cluster Assembly CL 0939+47 CL 0016+16 RX J0153－14 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

  7. Mapping the Three Major Components of Matter in Cluster Dark Matter Galaxies Hot Gas (weak-lensing) (photometric-redshift) (x-ray; XMM) RX J0152.7-1357 (z=0.83), 7 arcmin = 3.2 Mpc

  8. Environmental Effects “a priori” or “a posteriori”

  9. Galaxy Transition in CL0939 Cluster (z=0.4) Suprime-Cam + BVRI critical density Galaxies start to be truncated at relatively low density (groups) Kodama et al. (2001)

  10. FMOS roles for PISCES ~~~ Hα measurements over a large FoV ~~~ • Radial Velocities  Physical Associations of Substructures, 3-D Structures, Recent Merger Histories • Star Formation Rates  Less affected by Dust and Metallicity. Resolving the Recent Star Formation Histories by combining with Balmer indices and colours. Hα comes to FMOS window for 0.4<z<1.7 !

  11. Velocity Structures Clump Velocity Clump ~300 spectra across 8 Mpc (25’) around CL0024 cluster (z=0.395) A high-speed line-of-sight collision? Czoske et al. (2002) Radius

  12. Hα Mapping of CL0024 Cluster (z=0.4) Suprime-Cam + BRz’ and NB912 Hα LF Kodama, Balogh, et al. (2004) Hα intensity is a good measure of on-going star formation rate

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

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

  15. Dusty Starburst Radio (VLA), 1.4GHz OII k+a k+a a+k 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

  16. Down-sizing in Galaxy Formation z~1 passive galaxies in the Field corrected CM diagram for Subaru/XMM Deep Field (1.2 sq deg) z~1 galaxies down to M*+3 Deficit! Galaxy Formation is Down-sizing! Kodama et al. (2004)

  17. 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)

  18. Summary • FMOS will be an exellent facility for wide-field studies of distant clusters through Hα line. • 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. • Combining with the up-coming wide-field NIR imagers such as WFCAM (UKIRT, 30’) and MOIRCS (Subaru, 4’x7’), we will be able to extend such studies to z~1.7 (Hα) and far beyond (OII).

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