The spatial clustering of ultraluminous infrared galaxies over 1.5 < z < 3

We present measurements of the spatial clustering of galaxies with stellar masses greater than or similar to 10(11) M-circle dot, infrared luminosities greater than or similar to 10(12) L-circle dot, and star formation rates greater than or similar to 200 M-circle dot yr(-1) in two redshift intervals: 1.5 < z < 2.0 and 2 < z < 3. Both samples cluster moderately strongly, with spatial correlation lengths of r(0) = 6.14 +/- 0.84 h(-1) Mpc for the 2 < z < 3 sample and r(0) = 5.36 +/- 1.28 h(-1) Mpc for the sample. These clustering amplitudes are consistent with both populations residing in dark matter halos with masses of similar to 7 x 10(12) M-circle dot, 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, whereas the halos hosting the 1.5 < z < 2.0 sample will likely host greater than or similar to L-* elliptical galaxies or poor clusters at z = 0. We conclude that ultraluminous infrared galaxies (ULIRGs) at z similar to 2.5 likely signpost stellar buildup in galaxies that will reside in clusters at z = 0 and that ULIRGs at z similar to 1.7 signpost stellar buildup in sources that will either become greater than or similar to L-* elliptical galaxies or reside in poor clusters at z = 0.