The Clustering and Halo Masses of Star Forming Galaxies at z<1
  We present clustering measurements and halo masses of star forming galaxies
at 0.2 < z < 1.0. After excluding AGN, we construct a sample of 22553 24 {\mu}m
sources selected from 8.42 deg^2 of the Spitzer MIPS AGN and Galaxy Evolution
Survey of Bo\"otes. Mid-infrared imaging allows us to observe galaxies with the
highest star formation rates (SFRs), less biased by dust obscuration afflicting
the optical bands. We find that the galaxies with the highest SFRs have optical
colors which are redder than typical blue cloud galaxies, with many residing
within the green valley. At z > 0.4 our sample is dominated by luminous
infrared galaxies (LIRGs, L_TIR > 10^11 Lsun) and is comprised entirely of
LIRGs and ultra-luminous infrared galaxies (ULIRGs, L_TIR > 10^12 Lsun) at z >
0.6. We observe weak clustering of r_0 = 3-6 Mpc/h for almost all of our star
forming samples. We find that the clustering and halo mass depend on L_TIR at
all redshifts, where galaxies with higher L_TIR (hence higher SFRs) have
stronger clustering. Galaxies with the highest SFRs at each redshift typically
reside within dark matter halos of M_halo ~ 10^12.9 Msun/h. This is consistent
with a transitional halo mass, above which star formation is largely truncated,
although we cannot exclude that ULIRGs reside within higher mass halos. By
modeling the clustering evolution of halos, we connect our star forming galaxy
samples to their local descendants. Most star forming galaxies at z < 1.0 are
the progenitors of L < 2.5L* blue galaxies in the local universe, but star
forming galaxies with the highest SFRs (L_TIR >10^11.7 Lsun) at 0.6<z<1.0 are
the progenitors of early-type galaxies in denser group environments.
