Ringberg Castle, 7th July 2005 Panoramic View of Cluster Evolution Taddy Kodama (NAOJ / ESO), Masayuki Tanaka (Univ. of Tokyo), PISCES team Cygnus Vega.

Ringberg Castle, 7th July 2005

Panoramic View of Cluster EvolutionPanoramic View of Cluster Evolution

Taddy Kodama (NAOJ / ESO), Taddy Kodama (NAOJ / ESO), 　　　　　　　　　　　　 Masayuki Tanaka (Univ. of Tokyo), PISCES teamMasayuki Tanaka (Univ. of Tokyo), PISCES team

Cygnus

Vega

Altair♂

♀

OverviewOverview Panoramic Views of Cluster Scale AssembliesPanoramic Views of Cluster Scale Assemblies

Environmental Dependence of Galaxy Environmental Dependence of Galaxy EvolutionEvolution

Down-Sizing in Galaxy Formation and Down-Sizing in Galaxy Formation and EvolutionEvolution

Based on Subaru Panoramic ImagingBased on Subaru Panoramic Imaging

Cluster Assembly and Galaxy Cluster Assembly and Galaxy EvolutionEvolution

Morphology-Density Relation

N-body simulation (Dark matter)

SCDM; Moore et al. (1998)

Dressler et al. (1980; 1997)

E

Sp S

0

“a priori” or “a posteriori” ?

z=50

10

3 1

0.5

z=0

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

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’ = 10-15 Mpc) (optical, 30’ = 10-15 Mpc) and and WFCAM WFCAM (NIR, 52’ by 2×2 pointings for (NIR, 52’ by 2×2 pointings for z>0.5) z>0.5)

Spectroscopic follow-up with Spectroscopic follow-up with FOCASFOCAS (optical, 6’) (optical, 6’) and and FMOS/MOIRCSFMOS/MOIRCS (NIR, 30’/4’×7’) (NIR, 30’/4’×7’)

Mapping Large Scale Structures in and around Mapping Large Scale Structures in and around ClustersClusters

Cluster Scale Assembly Cluster Scale Assembly

Environmental Variation of Galaxy PropertiesEnvironmental Variation of Galaxy Properties

Origin of Morphology-SFR-Density RelationOrigin of Morphology-SFR-Density Relation

Kodama et al. (2005)

Panoramic Optical Imaging with SupPanoramic Optical Imaging with Suprime-Cam on Subarurime-Cam on Subaru

Suprime-Cam (34’ x 27’)

10 － 15 Mpc @ 0.4<z<1.3

Panoramic NIR Imaging Panoramic NIR Imaging with WFCAM on UKIRTwith WFCAM on UKIRT

WFCAM (52’ x 52’ by 4 pointings)

Panoramic Optical Panoramic Optical Spectroscopy with FOCAS Spectroscopy with FOCAS

on Subaruon Subaru

FOCAS (~30 multi-slits, 6’φ)

selected regions along large scale structures

Panoramic NIR Panoramic NIR Spectroscopy with FMOS / Spectroscopy with FMOS /

MOIRCS on SubaruMOIRCS on Subaru

FMOS(~400 fibers, 30’φ)

MOIRCS (~30 multi-slits, 4’×7’)

MembersMembers

PIPI ： ： T. KodamaT. Kodama (NAOJ) (NAOJ)

Co-I’sCo-I’sN. Arimoto, T. Yamada, N. Kashikawa, M. Iye, F. Nakata, M. Kajisawa N. Arimoto, T. Yamada, N. Kashikawa, M. Iye, F. Nakata, M. Kajisawa (NAOJ), (NAOJ), S. Okamura, Y. Suto, K. Shimasaku, M. Tanaka, H. YahagiS. Okamura, Y. Suto, K. Shimasaku, M. Tanaka, H. Yahagi(Univ of Tokyo), (Univ of Tokyo), K. Ohta, M. NagashimaK. Ohta, M. Nagashima (Kyoto Univ), (Kyoto Univ),T. Futamase, I. Tanaka, Y. KarasawaT. Futamase, I. Tanaka, Y. Karasawa (Tohoku Univ), (Tohoku Univ),H. Matsuhara, T. TamuraH. Matsuhara, T. Tamura (ISAS), (ISAS), T. HoshiT. Hoshi (Meisei Univ), (Meisei Univ),T. KitayamaT. Kitayama (Toho Univ), (Toho Univ), T. OhashiT. Ohashi (Tokyo Metro Univ), (Tokyo Metro Univ),N. Tamura, T. Okamoto, R. Bower, I. SmailN. Tamura, T. Okamoto, R. Bower, I. Smail (Durham, UK) (Durham, UK)K. Umetsu, W. KawasakiK. Umetsu, W. Kawasaki (Taipei), (Taipei), M. BaloghM. Balogh (Waterloo, Canada) (Waterloo, Canada)

Total Sample & Current Total Sample & Current StatusStatus

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<z<1.3

ACS(3.5’)

XMM1.14

SpitzerSpitzer

SpitzerSpitzer

SpitzerSpitzer

SpitzerSpitzer

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’(1% out of 34’x27’)

Courtesy: Ichi Tanaka

“A Chain Cluster”

Seeing ~ 0.5-0.6”

Optical (Galaxies) vs. X-ray Optical (Galaxies) vs. X-ray (Hot gas) (Hot gas)

RX J0152.7-1357 (z=0.83), 7 arcmin = 3.2 Mpc

Jones et al. (2003)

Kodama et al. (2004)

XMM-Newton

phot-z selected galaxies (Δz =－ 0.05~+0.03)

Panoramic Map of RXJ0153 Panoramic Map of RXJ0153 (z=0.83)(z=0.83)

Marked qualitative agreement with N-body simulations!

Central core dominated by red galaxies, and filaments coming out to variousdirections connecting groups of galaxies out to 10Mpc.

Moore et al. (1999)

Spectroscopic confirmation Spectroscopic confirmation of LSS of LSS

F1

F2F3

F4

F5

F7

F8

F6

We selected 8 groups in RXJ0153 for multi-slit spectroscopy with FOCAS/Subaru.

Spectroscopic confirmation Spectroscopic confirmation of LSS of LSS

0.835

0.842 0.837

0.835

0.843

0.7820.745

0.845

6 out of 8 groups are confirmed to locate at cluster redshifts! (~10 members per group)

Tanaka, Kodama, et al. (2005b)

⊿Vr <1000km/s

Spectroscopic confirmation Spectroscopic confirmation of LSS of LSS

They all show a distinct isolated peak in spec-z!

Tanaka, Kodama, et al. (2005b)

F1

F5

F4F3

F2

F6

F1F5

F2F3 F6

F4

σv = 200-400km/s

Panoramic Views of Cluster Panoramic Views 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

(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)

Truncation of SF in CL0939 Cluster Truncation of SF in CL0939 Cluster (z=0.41)(z=0.41)Suprime-Cam /

BVRIcritical density

Galaxies start to be truncated at relatively low density (groups) far from core, suggesting a non-cluster-specific mechanism for truncation.Kodama et al.

(2001)

75 %5025

Colour-Density RelationsColour-Density RelationsRXJ0153 (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. (2005)

bright

faint

50%

25%50%

25%

““Break Densities”Break Densities”

Tanaka, Kodama, et al. (2005)

slop

e o

f colo

ur

ch

an

ge

Star Formation vs. Star Formation vs. MorphologyMorphology

E+S0

S+I

Kodama, Balogh, et al. (2004)

Treu et al. (2003)

Morphologies seem to react later (or at inner region) than SF.

0.5Mpc

1.7Mpc

0.5Mpc

1.7Mpc

39 WFPC2 pointings across 25 arcmin!

CL0024 Cluster (z=0.4)

Suprime-Cam/Subaru

Galaxy evolution as a function Galaxy evolution as a function of massof 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), 1.2 deg^2

red+bright

blue+faint

red+bright

blue+faint

11 10 9 8log Mstar

U-V

=z’ (magnitude)

R-z

’ (c

olo

ur)

Down-sizing seen in the FP Down-sizing seen in the FP to z~1to z~1

Treu et al. (2005)

van der Wel et al. (2005)

GOODS (141 field early-types)CDFS/1252 (27 field early-types)

Less massive galaxies tend to have larger deviation in M/L ratiocompared to local FP, suggesting their younger ages.

Down-sizing seen in Down-sizing seen in Mg/Fe ratioMg/Fe ratio

Thomas (2001)Ap&SS, 277, 209

Lower Mg/Fe ratio towards smaller ellipticalssuggesting longer timescale of star formation.

ObsObs

ModelModel

““MorphologicalMorphological Down-sizing” Down-sizing”

＊ Early-types at massive-end and late-types at faint-end.

＊ Fraction of early-types at smallmass increases with decreasing redshift.

Bundy, Ellis, Conselice (2005) astro-ph/0502204 on GOODS fields (300 sq. arcmin)

AllE

P

AllE

P

AllE

PS

S

S

Classification of galaxy Classification of galaxy environmentsenvironments

fieldcluster

group

field

groupcluster

controlfield

controlfield

controlfield

Σ2Mpc

Field, Group, and Cluster

Tanaka, Kodama, et al. (2005)

Colour-Magnitude Colour-Magnitude DiagramsDiagrams

as a function of as a function of environmentenvironment

Tanaka, Kodama et al. (2005, astro-ph/0506713)

Luminosity Functions as a function of Luminosity Functions as a function of environmentenvironmentRXJ0153 (z=0.83) CL0016 (z=0.55) SDSS (z~0)

Tanaka, Kodama et al. (2005)

red

blue blueblueredred

Environmental Dependence of Environmental Dependence of Down-SizingDown-Sizing

Deficit of Red+Faint Galaxies is Stronger in Lower Density Regions. Environment = Evolutionary Stage

Tanaka, Kodama, et al. (2005)

R(Giant/Dwarf) for red galaxies (><4ｘ 10 Mo)

Degree of theDeficit of RedFaint Galaxies

＝

10

Build-up of Build-up of thethe colour- colour-magnitude relationmagnitude relation

z=1

z=0.5

z=0 Coma

fading vector

From Distant Clusters to From Distant Clusters to Nearby ClustersNearby Clusters

z=0.43 0.33 0.23 0.0

Assembly

Evolution

fading vector

Kodama & Bower (2001)

Once the SF is truncated, difference inlum. weighted age as a function of luminosity will be diminished quickly.

Luminosity weighted age at z=0

Flow of galaxies on the CMDs

Δ(U

-V)

MV

Formation of massive Formation of massive galaxies: late assembly?galaxies: late assembly?

Baugh et al. (2002)

z=3

1 0

Stellar mass function is expected to dramatically change with time in the hierarchical galaxy formation models

Mstars

semi-analytic model

Bekki & Chiba (2001)

2

Assembly of massive galaxies Assembly of massive galaxies in the Fieldin the Field

Pozzetti et al. (2003)

Saracco et al. (2004)

K20 (52 arcmin^2)

GDDS (120 arcmin^2)

No evolution out to z~1.5

10 M◎11

No evol. to z~1.7

Glazebrook et al. (2004)

No evol. to z~1.6

L>2L*

L>3L*

MUNICS (160

arcmin^2)

Also in the field environment, mass assembly is largely completed by z~1.5.

Distant Red Galaxies (DRG) at Distant Red Galaxies (DRG) at 2<z<32<z<3

by the FIRES (near-infrared by the FIRES (near-infrared survey)survey)Franx + (2003), van Dokkum + (2003; 2004), Forster Schreiber + (2004)

DRGs significantly contribute to stellar mass density at 2<z<3: 2×LBG！

DRG

LBG

10 Mo11

SummarySummary Assembly of clusters of galaxiesAssembly of clusters of galaxies * Large scale filamentary structures (>10Mpc) are * Large scale filamentary structures (>10Mpc) are

seen in all clusters, providing good evidence for seen in all clusters, providing good evidence for cluster scale assembly.cluster scale assembly.

Origins of morph-density/sfr-density relationsOrigins of morph-density/sfr-density relations * Truncation of SF is sharply seen in groups far out * Truncation of SF is sharply seen in groups far out

from cluster cores.from cluster cores. * Truncation of SF and transformation of * Truncation of SF and transformation of

morphologies are driven by different physical morphologies are driven by different physical processes (at least partly).processes (at least partly).

Down-sizing in galaxy formation/evolution.Down-sizing in galaxy formation/evolution. * Massive galaxies form early while less massive * Massive galaxies form early while less massive

galaxies (in final) form later or have more extended galaxies (in final) form later or have more extended star formation.star formation.

* Down-sizing is a function of environment * Down-sizing is a function of environment (=evolutionary stage). (=evolutionary stage).

high-density/high-mass high-density/high-mass low-density/low- low-density/low-massmass

Key QuestionsKey Questions

What’s happening in groups to stop star formation?What’s happening in groups to stop star formation? Is it intrinsic or external effect?Is it intrinsic or external effect? Search for interaction and/or E+A in groups.Search for interaction and/or E+A in groups.

What’s the connection between “down-sizing” and What’s the connection between “down-sizing” and the hierarchical galaxy formation (“bottom-up”)?the hierarchical galaxy formation (“bottom-up”)?

--- strong galaxy formation bias --- --- strong galaxy formation bias --- Very efficient SF and assembly for massive Very efficient SF and assembly for massive

galaxies?galaxies? Suppression of early SF in dwarfs (UVB, gas Suppression of early SF in dwarfs (UVB, gas

fallback)?fallback)?

Thank you, Alvio!Thank you, Alvio!

Prost !18/06/05