High Redshift Massive Galaxies (BzKs & EIS-Deep3a and COSMOS Xu KONG collaborators ： E. Daddi, N. Arimoto, A. Renzini, K. Ohta ， T. Broadhurst ， A. Cimatti ， C. Ikuta ， L. Costa, L. Olsen, M. Onodera ， N. Tamura Kyoto

1. Introduction NIR Surveys –HDF (2x5.3 arcmin 2 ) UDF (5.76 arcmin 2 ) SDF (4.0 arcmin 2 ) –K20 (52.0 arcmin 2 ) SXDF (114.0 arcmin 2 ) GOODS (160.0arcmin 2 ) Limited: small sky area (high-z galaxy clustering) Step forward : ~1000 arcmin 2 NIR survey ~ COSMOS !!

2. EIS-Deep3a Fields –Deep3a-F: 320 arcmin 2 (Ks<20.0 mag) –Daddi-F : 600 arcmin 2 (Ks<18.8 mag); 450 arcmin 2 (Ks<19.2 mag) Observation ： Image ＋ Spectroscopy –Imaging ： optical ＋ NIR (Subaru +NTT) NAOJ 8.2m SUBARU telescope: B,R,I and z' 2003 ESO 3.5m NTT telescope : J and Ks 2001 BRIzJK and U877,U841,V843 –Spectroscopy ： optical ＋ NIR (VLT + Subaru) hundreds optical spectra, >10 NIR spectra

3. Photometric Catalog NIR : Ks band catalog, 10 4 objects  BzKs & EROs K-band number counts

4.1 High redshift galaxies Daddi et al. (2004, ApJ, 617,746) K20 Survey ： VLT Large Program –50. arcmin 2 –~ 500 spectra –SFGs BzK> -0.2 BzK=(z-K) AB -(B-z) AB BzK >-0.2 : sBzKs BzK 2.5 : pBzKs sBzKspBzKs a) BzKs at 1.4≤z≤2.5 b) EROs R-K>5.0

High-z Galaxies In Our fields Passive galaxies at z>1.0 (pBzKs) EROs: R-K>5.0 SFGs at z>1.4 (sBzKs) Galaxies at z<1.4 Stars Deep3a-F: 380 sBzKs 122 pBzKs 750 EROs Daddi-F: 120 sBzKs 40 pBzKs 350 EROs

High-z galaxy number counts K=20mag :sBzKs 1.20/arcmin 2 ; pBzKs 0.38/arcmin 2

5.1 Photometric Redshift VLT Spectroscopic z Photometric z

Redshift (photo_z) Distribution BzKs EROs z ~1.8 z ~1.0 BzK selection is a quite powerful way to separate galaxies at 1.4<z<2.5

BzKs are strong clustering! 5.2 Clustering Clustering of field galaxies Amplitudes ~ published values Clustering of EROs A ~ published values K fainter, A decrease Clustering of BzKs A is large K fainter, A decrease Landy & Szalay (1993)  (DD-2DR+RR)/RR ＝ A   

sBzKs are dusty galaxies : E(B-V) ~ 0.4 sBzKs have high SFRs : SFR ~ 190 M  /yr Most BzKs are massive galaxies : M ~ 1.0E11 M  SFRD at z~2 : M  /yr Mass densities : logρ * =7.7 M  Mpc -3 M*>1.0e11 : n(pBzKs) = n(pBzKs) = 0.5 n(E/S0) = 4.0*10 -4 Mpc E(B-V) SFR Mass

Conclusion BzK selection is a quite powerful way to separate galaxies at 1.4<z<2.5. BzKs are likely to be possible precursors of z ～ 1 EROs and z=0 elliptical galaxies. Massive, high-z, strong clustering, high SFR, and high metallicity. Kong, Daddi, Arimoto, Renzini, et al. 2005, submitted to ApJ.

Mobasher & Capak May05 (i<26) Sample selection: RA,DEC: 1.3x1.3 Ks<19.8 Mask=0 Non-saturated Subaru B Subaru z’ KPNO Ks mask

BzKs in COSMOS

sBzKs (K<19.8 in Vega) 10% low redshift BzKs (z<1.0) What are the reasons? More templates? J or H band catalog? mask?

Number and sky density Deep3aCOSMOS Ks sBzKs /arcmin^20.9/arcmin^2 pBzKs /arcmin^20.06/arcmin^2 ? Sky density of pBzKs in COSMOS is less than that of in Deep3a i<26 mag catalog be used  full catalog

Clustering of sBzKs

EROs in COSMOS (rp-Ks>3.5)

sBzKs EROs

We will do on COSMOS … BzKs : 1.4<z<2.5 High-z cluster candidates Morphology of BzKs Hubble sequence at z~2 LF from z=1.4 to 2.5 We are working on COSMOS … sBzKs/pBzKs/EROs sampling Number counts of BzKs/EROs Clustering for BzKs/EROs Cosmic variances of clustering E(B-V), SFR, stellar mass of sBzKs, SFRD at z~2