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Panoramic View of Cluster Evolution Distant Clusters of Galaxies (Ringberg, 24 Oct 2005) Taddy Kodama (NAOJ), Masayuki Tanaka (Univ. of Tokyo), PISCES.

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Presentation on theme: "Panoramic View of Cluster Evolution Distant Clusters of Galaxies (Ringberg, 24 Oct 2005) Taddy Kodama (NAOJ), Masayuki Tanaka (Univ. of Tokyo), PISCES."— Presentation transcript:

1 Panoramic View of Cluster Evolution Distant Clusters of Galaxies (Ringberg, 24 Oct 2005) Taddy Kodama (NAOJ), Masayuki Tanaka (Univ. of Tokyo), PISCES team “Sunset at Mauna Kea” (24/05/05)

2 Members Members PI : T. Kodama (NAOJ) PI : T. Kodama (NAOJ) Co-I’s Co-I’s N. Arimoto, T. Yamada, M. Kajisawa, C. Kobayashi, N. Kashikawa, T. Okamoto, N. Tamura, F. Nakata (NAOJ), S. Okamura, K. Shimasaku, M. Tanaka (Univ of Tokyo), I. Tanaka (Tohoku Univ), H. Matsuhara, T. Tamura (ISAS), T. Hoshi (Meisei Univ), K. Umetsu (Taipei), R. Bower, I. Smail (Durham), M. Balogh (Waterloo)

3 Overview Panoramic Views of Cluster Scale Assemblies Panoramic Views of Cluster Scale Assemblies Environmental Dependence of Galaxy Evolution Environmental Dependence of Galaxy Evolution Down-Sizing in Galaxy Formation and Evolution Down-Sizing in Galaxy Formation and Evolution Based on Subaru Panoramic Imaging

4 Cluster Assembly and Galaxy Evolution Morphology-Density RelationN-body simulation (Dark matter) SCDM; Moore et al. (1998) Dressler et al. (1980; 1997) E Sp S0 “a priori” or “a posteriori” ? z= z=0

5 Panoramic Imaging and Spectroscopy of Cluster Evolution with Subaru Panoramic Imaging and Spectroscopy of Cluster Evolution with Subaru Panoramic imaging of ~15 Clusters at ) Panoramic imaging of ~15 Clusters at ) Spectroscopic follow-up with FOCAS (optical, 6’) and FMOS/MOIRCS (NIR, 30’/4’×7’) Spectroscopic follow-up with FOCAS (optical, 6’) and FMOS/MOIRCS (NIR, 30’/4’×7’)  Mapping Large Scale Structures in and around Clusters Cluster Scale Assembly Cluster Scale Assembly  Environmental Variation of Galaxy Properties Origin of Morphology-SFR-Density Relation Origin of Morphology-SFR-Density Relation Kodama et al. (2005)

6 Total Sample & Current Status Imaging : Suprime-Cam-BB CL0024, CL0939, CL0016, RX1716, RXJ0153, CL1604, CL1252, RXJ0849, CL0451, MS2054, MS1054, RD0910 (8 clusters completed, 4 clusters half-done, 3 not yet) Suprime-Cam-NB (Hα) CL0024 (z=0.39), CL0939 (z=0.41) WFCAM (NIR) CL1604 (z=0.9), CL1252 (z=1.23) Spectroscopy : FOCAS CL0939 (z=0.41), CL0016 (z=0.55), RXJ0153 (z=0.83) 15 X-ray detected clusters at 0.4

7 RX J (z=0.83) Suprime-Cam V : 120 min R : 116 min i’ : 75 min z’ : 79 min central 3’ x 3’ (1% out of 34’x27’) Courtesy: Ichi Tanaka “A Chain Cluster” Seeing ~ ”

8 Panoramic Views of Cluster Assembly CL CL CL z=0.41 (4.3 Gyr ago) z=0.55 (5.4 Gyr ago) z=1.24 (8.6 Gyr ago) 30 arcmin = 10, 12, and 15 Mpc (physical), respectively contours: 1.5, 2, 3, 4, 5 sigma Distribution of phot-z sliced galaxies (Δz = - 0.05~+0.03) Kodama, et al. (2005)

9 Spectroscopic confirmation of LSS out of 8 groups are confirmed to locate at cluster redshifts! (~10 members per group) Tanaka, Kodama, et al. (2005b) ⊿ Vr < 1000km/s Two sheets? z~0.837, 0.844

10 Colour-Density Relations RXJ0153 (z=0.83) CL0016 (z=0.55) SDSS (z~0) Colours change sharply at break densities, especially for faint galaxies (>M*+1). Tanaka, Kodama, et al. (2005a) bright faint 50% 25% 50% 25%

11 Star Formation vs. Morphology E+S0 S+I Kodama, Balogh, et al. (2004) Treu et al. (2003) Morphologies seem to react later (or at inner region) than SF. 0.5Mpc1.7Mpc0.5Mpc1.7Mpc 39 WFPC2 pointings across 25 arcmin! CL0024 Cluster (z=0.4) Suprime-Cam/Subaru

12 Galaxy evolution as a function of mass SDSS (z=0) Kauffmann et al. (2003) Massive galaxies are old, while less massive galaxies are younger or have more extended star formation:  “Down-sizing”! Kodama et al. (2004) see also De Lucia et al. (2004) critical mass SXDS (z=1, 1.2deg^2) red+bright blue+faint red+bright blue+faint log Mstar U-V = z’ (magnitude) R-z’ (colour)

13 Colour-Magnitude Diagrams as a function of environment Tanaka, Kodama et al. (2005a)

14 Environmental Dependence of Down-Sizing Deficit of Red+Faint Galaxies is Stronger in Lower Density Regions.  Environment = Evolutionary Stage Tanaka, Kodama, et al. (2005a) R(Giant/Dwarf) for red galaxies (><4 x 10 Mo) Degree of the Deficit of Red Faint Galaxies = 10

15 Summary Assembly of clusters of galaxies Assembly of clusters of galaxies * Large scale filamentary structures (>10Mpc) are seen in all clusters, providing good evidence for cluster scale assembly. * Large scale filamentary structures (>10Mpc) are seen in all clusters, providing good evidence for cluster scale assembly. Origins of morph-density/sfr-density relations Origins of morph-density/sfr-density relations * Truncation of SF is sharply seen in groups far out from cluster cores. * Truncation of SF is sharply seen in groups far out from cluster cores. * Truncation of SF and transformation of morphologies are driven by different physical processes (at least partly). * Truncation of SF and transformation of morphologies are driven by different physical processes (at least partly). Down-sizing in galaxy formation/evolution. Down-sizing in galaxy formation/evolution. * Massive galaxies form early while less massive galaxies (in final) form later or have more extended star formation. * Massive galaxies form early while less massive galaxies (in final) form later or have more extended star formation. * Down-sizing is a function of environment (=evolutionary stage). * Down-sizing is a function of environment (=evolutionary stage). high-density/high-mass  low-density/low-mass high-density/high-mass  low-density/low-mass


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