The spatial clustering of ultraluminous infrared galaxies over 1.5<z<3
Abstract
We present measurements of the spatial clustering of galaxies with stellar masses >1011Msun, infrared luminosities >1012 Lsun, and star formation rates >200Msun per year in two redshift intervals; 1.5<z<2.0 and 2<z<3. Both samples cluster very strongly, with spatial correlation lengths of r0=14.40+/-1.99 h-1Mpc for the 2<z<3 sample, and r0=9.40+/-2.24 h-1Mpc for the 1.5<z<2.0 sample. These clustering amplitudes are consistent with both populations residing in dark matter haloes with masses of ~6x1013Msun, making them among the most biased galaxies at these epochs. We infer, from this and previous results, that a minimum dark matter halo mass is an important factor for all forms of luminous, obscured activity in galaxies at z>1, both starbursts and AGN. Adopting plausible models for the growth of DM haloes with redshift, then the haloes hosting the 2<z<3 sample will likely host the richest clusters of galaxies at z=0, whereas the haloes hosting the 1.5<z<2.0 sample will likely host poor to rich clusters at z=0. We conclude that ULIRGs at z>1 signpost stellar buildup in galaxies that will reside in clusters at z=0, with ULIRGs at increasing redshifts signposting the buildup of stars in galaxies that will reside in increasingly rich clusters.
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