2006ApJ...641L..17F

We present measurements of the spatial clustering of galaxies with stellar masses ≳10¹¹ M_☉, infrared luminosities ≳10¹² L_☉, and star formation rates ≳200 M_☉/yr in two redshift intervals: 1.5<z<2.0 and 2<z<3. Both samples cluster moderately strongly, with spatial correlation lengths of r₀=6.14±0.84 h^–1 Mpc for the 2<z<3 sample and r₀=5.36±1.28 h^–1 Mpc for the 1.5<z<2.0 sample. These clustering amplitudes are consistent with both populations residing in dark matter halos with masses of ∼7x10¹² M_☉, which is comparable to that seen for optical QSOs at the same epochs. We infer 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 active galactic nuclei. Adopting plausible models for the growth of dark matter halos with redshift, the halos hosting the 2<z<3 sample will likely host poor to rich clusters of galaxies at z=0, whereas the halos hosting the 1.5<z<2.0 sample will likely host ≳L^* elliptical galaxies or poor clusters at z=0. We conclude that ultraluminous infrared galaxies (ULIRGs) at z∼2.5 likely signpost stellar buildup in galaxies that will reside in clusters at z=0 and that ULIRGs at z∼1.7 signpost stellar buildup in sources that will either become ≳L^* elliptical galaxies or reside in poor clusters at z=0.