TY - JOUR
T1 - Clustering of dust-obscured galaxies at z ∼ 2
AU - Brodwin, Mark
AU - Dey, Arjun
AU - Brown, Michael J.I.
AU - Pope, Alexandra
AU - Armus, Lee
AU - Bussmann, Shane
AU - Desai, Vandana
AU - Jannuzi, Buell T.
AU - Le Floc'h, Emeric
PY - 2008/11/10
Y1 - 2008/11/10
N2 - We present the angular autocorrelation function of 2603 dust-obscured galaxies (DOGs) in the Boötes field of the NOAO Deep Wide-Field Survey. DOGs are red, obscured galaxies, defined as having R - [24] ≥ 14 (F 24/FR ≥ 1000). Spectroscopy indicates that they are located at 1.5 ≲ z ≲ 2.5. We find strong clustering, with r 0 = 7.40-0.84+1.27 h-1 Mpc for the full F24 > 0.3 mJy sample. The clustering and space density of the DOGs are consistent with those of submillimeter galaxies, suggestive of a connection between these populations. We find evidence for luminosity-dependent clustering, with the correlation length increasing to r0 = 12.97-2.64+4.26 h-1 Mpc for brighter (F24 < 0.6 mJy) DOGs. Bright DOGs also reside in richer environments than fainter ones, suggesting these subsamples may not be drawn from the same parent population. The clustering amplitudes imply average halo masses of log M = 12.2-0.2+0.3 M⊙ for the full DOG sample, rising to log M = 13.0-0.3+0.4 M ⊙ for brighter DOGs. In a biased structure formation scenario, the full DOG sample will, on average, evolve into ∼3L, present-day galaxies, whereas the most luminous DOGs may evolve into brightest cluster galaxies.
AB - We present the angular autocorrelation function of 2603 dust-obscured galaxies (DOGs) in the Boötes field of the NOAO Deep Wide-Field Survey. DOGs are red, obscured galaxies, defined as having R - [24] ≥ 14 (F 24/FR ≥ 1000). Spectroscopy indicates that they are located at 1.5 ≲ z ≲ 2.5. We find strong clustering, with r 0 = 7.40-0.84+1.27 h-1 Mpc for the full F24 > 0.3 mJy sample. The clustering and space density of the DOGs are consistent with those of submillimeter galaxies, suggestive of a connection between these populations. We find evidence for luminosity-dependent clustering, with the correlation length increasing to r0 = 12.97-2.64+4.26 h-1 Mpc for brighter (F24 < 0.6 mJy) DOGs. Bright DOGs also reside in richer environments than fainter ones, suggesting these subsamples may not be drawn from the same parent population. The clustering amplitudes imply average halo masses of log M = 12.2-0.2+0.3 M⊙ for the full DOG sample, rising to log M = 13.0-0.3+0.4 M ⊙ for brighter DOGs. In a biased structure formation scenario, the full DOG sample will, on average, evolve into ∼3L, present-day galaxies, whereas the most luminous DOGs may evolve into brightest cluster galaxies.
KW - Evolution-galaxies
KW - Formation-galaxies
KW - Galaxies
KW - High-redshift-galaxies
KW - Statistics-large-scale structure of universe
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U2 - 10.1086/593327
DO - 10.1086/593327
M3 - Article
AN - SCOPUS:58149107120
SN - 0004-637X
VL - 687
SP - L65-L68
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -