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 ] \geq 14 ( F _ { 24 } / F _ { R } \gtrsim 1000 ) .
Spectroscopy indicates that they are located at 1.5 \lesssim z \lesssim 2.5 .
We find strong clustering , with r _ { 0 } = 7.40 ^ { +1.27 } _ { -0.84 } h ^ { -1 } Mpc for the full F _ { 24 } > 0.3 mJy sample .
The clustering and space density of the DOGs are consistent with those of sub-mm galaxies , suggestive of a connection between these populations .
We find evidence for luminosity-dependent clustering , with the correlation length increasing to r _ { 0 } = 12.97 ^ { +4.26 } _ { -2.64 } h ^ { -1 } Mpc for brighter ( F _ { 24 } > 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 ^ { +0.3 } _ { -0.2 } M _ { \odot } for the full DOG sample , rising to \log { M } = 13.0 ^ { +0.4 } _ { -0.3 } M _ { \odot } for brighter DOGs .
In a biased structure formation scenario , the full DOG sample will , on average , evolve into \sim 3 L _ { * } present-day galaxies , whereas the most luminous DOGs may evolve into brightest cluster galaxies .