A Wide Area Survey for High-Redshift Massive BzK Galaxies X.Kong, M.Onodera, C.Ikuta (NAOJ), K.Ohta (Kyoto), N.Tamura (Durham), A.Renzini, E.Daddi, L. Da Costa (ES O), A.Cimatti (Arcetri), T.Broadhurst (Tel’Aviv), L.F.Ols en (Cote d’Azur) N. ARIMOTO (NAOJ) Kong et al. (2006) ApJ 638, 72
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A Wide Area Survey for High- Redshift Massive BzK Galaxies X.Kong, M.Onodera, C.Ikuta (NAOJ), K.Ohta (Kyoto), N.Tamura (Durham), A.Renzini, E.Daddi, L.
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A Wide Area Survey for High-Redshift Massive BzK Galaxies
X.Kong, M.Onodera, C.Ikuta (NAOJ), K.Ohta (Kyoto),N.Tamura (Durham), A.Renzini, E.Daddi, L. Da Costa (ESO),
We have undertaken a fairly deep, wide-field imaging with the Subaru/Suprime-Cam of two fields of 900 arcmin2 each for part of which near-IR data are available from ESO
NTT observations.
EIS3a-F (Subaru/NTT, Ks=20.8) 320 arcmin2
Daddi-F (Subaru/NTT, Ks=19.0) 600 arcmin2
The prime aim of this survey is to understandhow and when the present-day massive
galaxies formed. To this end, the imaging observations have been optimized for the use of optical/near-infrared multi-colour selectioncriteria to identify both star forming (sBzKs)
and passive galaxies (pBzKs).
Kong et al. (2006) ApJ 638, 72
Subaru/Sup-Cam Observation
Daddi FieldRA=14:49:29, DEC=09:00:00 (J2000.0)
Subaru/Suprime-Cam BIz’: 2003/03/02-04WHT R : 1998/03/19-21NTT/SOFI K : 1999/03/27-30 BRIz’ (940 arcmin2) 3σ in 2”(AB) B(AB)=26.59 R(AB)=25.64 I(AB)=25.62 z’(AB)=25.31
K (600 arcmin2) 3σ in 2”(AB) Ks(AB)=20.91
940arcmin2
600arcmin2
Subaru/Sup-Cam Observation
ESO Imaging Survey (EIS Deep 3a) FieldRA=11:24:50, DEC=-21:42:00 (J2000.0)
Subaru/Suprime-Cam BRIz’: 2003/03/02-04NTT/SOFI JK : 2002/03/28-31 BRIz’ (940 arcmin2) 3σ in 2”(AB) B(AB)=27.46 R(AB)=26.87 I(AB)=26.56 z’(AB)=26.07
JK (320 arcmin2) 3σ in 2”(AB) J(AB)=23.40, Ks(AB)=22.70
940arcmin2
320arcmin2
High-z galaxies Deep 3a field
Star-forming galaxies at z>1.4 (sBzKs)
Old galaxies at z>1.4: (pBzKs)
stars
BzK=(z-K)-(B-z)>-0.2
(z-K)>2.5
Daddi et al. (2004) ApJ 617, 746
SEDs of sBzKs and pBzKs
star-formingpassive
low-z
high-z
Photometric Redshift
Spectroscopic Redshifts (VLT)
Daddi et al. (2006)
pBzK(ERO) sBzK sBzK sBzK
ERO ERO ERO ERO
Star/Galaxy Separation
(z-K)AB-0.3(B-z)AB<-0.5
387 sBzK 121 pBzK
108 sBzK 48 pBzK
513 ERO
337 EROs
Photometric Redshift (EROs)
Photometric Redshift (sBzKs)
Photometric Redshift (pBzKs)
Number Counts of sBzKs, pBzKs, and EROs
EROs
galaxies
sBzKs
pBzKs
Two Point Correlation Functions w(Θ)
Daddi-F Deep 3a-F
Landy & Szalay (1993)
Angular Clustering Amplitude
Physical Properties of sBzKs and pBzKs
• Supposing <z> ~ 2 for sBzKs, we have derived their physical properties, such as the reddening, star formation rate, and the stellar mass.
(While errors by a factor of 2 or more may affect individual estimates, the average quantities should be relatively robust.)