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?