PPanoramic anoramic IImaging and maging and SSpectroscopy of pectroscopy of CCluster luster EEvolution with volution with SSubaru ubaru

((PISCESPISCES))

FMOS meeting (Kyoto, 13-14/01/04)

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 ?What’s PISCES ?

Panoramic Imaging of 15 Clusters at 0.4<z<1.3 Panoramic Imaging of 15 Clusters at 0.4<z<1.3 with with Suprime-Cam Suprime-Cam (optical, 30’ = 10-14 Mpc)(optical, 30’ = 10-14 Mpc)

Spectroscopic Follow-up with Spectroscopic Follow-up with FOCASFOCAS (optical, 6’) (optical, 6’) and and FMOSFMOS (NIR, 30’) along the Structures (NIR, 30’) along the Structures

Mapping Large Scale Structure in and around Mapping Large Scale Structure in and around ClustersClusters

Cluster Assembly and Spatial BiasCluster Assembly and Spatial Bias Environmental Variation of Galaxy PropertiesEnvironmental Variation of Galaxy Properties Origin of Density-Morphology-SFR RelationOrigin of Density-Morphology-SFR Relation

Cluster Assembly and Galaxy Cluster Assembly and Galaxy EvolutionEvolution

Colour-Magnitude Relation

Density-Morphology Relation

N-body simulation (Dark matter)

Moore et al.

Terlevich et al.

Dressler et al.

E

Sp S

0

Cluster SampleCluster Sample15 X-ray selected clusters at 0.4<z<1.3

RX J0152.7-1357

(z=0.83)

Suprime-Cam V : 120 min R : 116 min i’ : 75 min z’ : 79 min

central 3’ x 3’ (outof 34’x27’)

Panoramic View of Cluster Panoramic View of Cluster AssemblyAssembly

CL 0016+16

CL 0939+47 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, respec

tively

contours: 1.5, 2, 3, 4, 5 sigma

Mapping the Three Major Mapping the Three Major Components of Matter in ClusterComponents 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

Environmental EffectsEnvironmental Effects“a priori” or “a posteriori”

Galaxy Transition in CL0939 Galaxy Transition in CL0939 Cluster (z=0.4)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 PISCESFMOS roles for PISCES

Radial VelocitiesRadial Velocities Physical Associations of Substructures,Physical Associations of Substructures, 3-D Structures, Recent Merger Histories3-D Structures, Recent Merger Histories Star Formation RatesStar Formation Rates Less affected by Dust and Metallicity. Less affected by Dust and Metallicity. Resolving the Recent Star Formation HistoriesResolving the Recent Star Formation Histories by combining with Balmer indices and colours.by combining with Balmer indices and colours.

~~~ Hα measurements over a large FoV ~~~Hα comes to FMOS window for 0.4<z<1.7 !

Velocity StructuresVelocity Structures

Clump

Clump

Radius

Vel

oci

ty

Czoske et al. (2002)

A high-speed line-of-sight collision?

~300 spectra across 8 Mpc (25’) around CL0024 cluster (z=0.395)

Hα Mapping of CL0024 Cluster (z=0.4)Hα Mapping of CL0024 Cluster (z=0.4)Suprime-Cam + BRz’ and NB912

Hα intensity is a good measure of on-going star formation rate

Hα LF

Kodama, Balogh, et al. (2004)

Global Star Formation History in Clusters Global Star Formation History in Clusters (Cl(Cluster counterpart of the Madau plot)uster counterpart of the Madau plot)

Kodama, Balogh et al. (2004)

SFR (z)

SFR (σ)

This work

This work

Starburst/Post-starburst Starburst/Post-starburst GalaxiesGalaxies

Hδ

g - r

OII

Spectral classification

Spectral indices

Dressler et al. (1999)

Poggianti et al. (1999)

Burst active

Age (Gyr)

Resolving Recent SF Histories

k+a

k

a+k

e(c)

e(a)

Dusty StarburstDusty Starburst

k+a

k+a

k+aa+k

a+k

Radio (VLA), 1.4GHz

Hα+NII

OII

Poggianti et al. 1999

Smail et al. 1999

Hα is a better tracer for on-going star formation activities

Down-sizing in Galaxy Down-sizing in Galaxy FormationFormation

Subaru/XMM Deep Field (1.2 sq deg)

z~1 passive galaxies in the

Field corrected CM diagram for z~1 galaxies down to M*+3

Galaxy Formation is Down-sizing!

Deficit!

Kodama et al. (2004)

From Distant Clusters to theFrom Distant Clusters to the Present-day Clusters Present-day Clusters

Kodama & Bower (2001)

Global SF History

z=0.43 0.33 0.23 0.0

Assembly

Evolution

Madau plot

Taddy plot!

SummarySummary FMOS will be an exellent facility for wide-field stFMOS will be an exellent facility for wide-field st

udies of distant clusters through Hudies of distant clusters through Hαα line. line. PISCES will provide panoramic views of hierarchPISCES will provide panoramic views of hierarch

ical growth of clusters through assembly and gaical growth of clusters through assembly and galaxy evolution therein since the Universe was onlaxy evolution therein since the Universe was only 1/3 of its present age.ly 1/3 of its present age.

Combining with the up-coming wide-field NIR imCombining with the up-coming wide-field NIR imagers such as WFCAM (UKIRT, 30’) and MOIRCagers such as WFCAM (UKIRT, 30’) and MOIRCS (Subaru, 4’x7’), we will be able to extend sucS (Subaru, 4’x7’), we will be able to extend such studies to z~1.7 (Hh studies to z~1.7 (Hαα) and far beyond (O) and far beyond (OIIII).).