Lecture140504

Galaxy Evolution and Environment (Malaysia, 03/04/2009)Build-up of the red sequence of galaxies through cosmic time and across environmentTaddy Kodama (NAOJ), Yusei Koyama (Univ. of Tokyo), Masao Hayashi (Univ. of Tokyo) Masayuki Tanaka (ESO), and the PISCES/HzRG team

Inside-out propagation of star forming activity in clusters 1

OutlineLarge scale structures in and around clusters at all redshifts (0.4 1011 Lsun)Deep imaging (67Jy) at 15m

IR satellite, D=69cm, 1.7 1.5 M/yrH[OIII][OII]15

Ha emitter with > 2 Msun/year:Spatial Distribution of H emitters

MOIRCS FoVNone! H emitters are avoiding the central region ( Rc < 230kpc ) and preferentially found in the surrounding regions.None !distance from the x-ray centreSpatial distributions of H emitters and 15m sources are similar (but direct overlaps are only 8).16H emitters on the red sequence!

EW > 50 A EW < 50 AMost of them are located in the outer region ( Rc>500kpc ). H emitters 17

What are the red H emitters?

red H emittersStrong dust extinction even for H? (or dusty AGN?)RzJA similar method that are used to separate between passive/dusty EROs with IJKthat measures the sharpness of the 4000/Balmer break feature. 15m sources blue H emitters(Pozzetti+2000)Koyama, TK, et al. (2009)There may be a large amount of hidden star formation in IR which is not seen even with H??18instrumentsSuprime-CamMOIRCSpassbandsBzNB912JKsdates2008. 07.30-312008. 06.30-07.01pointings14FoV32 x 236.1 x 5.83 mags27.5925.8125.7523.84-24.5723.07-23.65seeing1.091.09

z NB912 [OII] @ z=1.46

(Stanford+06 )XMMXCS J2215.9-1738NB912 filter(lc=9139A, Dl=134A)A narrow-band [OII] imaging with Suprime-Cam/Subaru (XCS2215@z=1.457) Hayashi et al. (2009), in prep.19

NB912 emitters[OII] emitters (44)3s5s3s[OII] @ z=1.46Ha @ z=0.4 [OIII] @ z=0.84Selection of [OII] emitters associated to the XCS2215 cluster (z=1.46)SFR ([OII]) > 2.6 M/yrHayashi et al. (2009), in prep.Spectroscopically confirmedmembers (Hilton et al. 2007)Spatial Distribution of the [OII] emittersHayashi et al. (2009), in prep.

High star formation activity to the very center of the cluster!(AGN contamination?)21

Hayashi et al. (2009), in prep.

fractionto field corrected phot-z membersHigh star formation activity to the very center of the cluster!(AGN contamination?)Spatial Distribution of the [OII] emitters22

Star forming activity in the cluster coresInside-out propagation of star forming activity in cluster cores !?H emitters at z=0.81 (RXJ1716)[OII] emitters at z=1.46 (XCS2215)Koyama, TK, et al. (2009)Hayashi, TK, et al. (2009)phot-z members23

(Kodama+04)H @ z=0.4[OII] @ z=1.51001010.60.40.2[OII] fractionDensity [Galaxies/Mpc2]

H @ z=0.8

(Koyama+09)(Hayashi+09)Poggianti+081000[OII] @ z=0.4-0.8PAH @ z=0.8(Koyama+08)Density [Galaxies/Mpc2]highlow(Cooper +08)[OII] @ z=1Densitylog Can we eventually see a reversal of the SFR-Rc / SFR-density relations?highlowRadius [Mpc]Radius [arcmin]Radius [arcmin]see also Elbaz et al. (2007)

Poggianti+08SSFR24Emergence of the red-sequence at z~2 in proto-clusters?

DRG(J-K>2.3)RG

r-JHK b-JHKKodama et al. (2007)The red sequence seems to be emerging between z=3 and 2 ( 2 < Tuniv[Gyr] < 3).z~2 (PKS1138)z~3 (USS0943)25SummaryStarbursts/truncation of galaxies in groups/ outskirts of clusters at z1.5-2 Intrinsic effects (Nature) (galaxy formation bias?)Inside-out propagation/truncation of star formation in clusters?