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 0:4 our sample is dominated by luminous infrared galaxies (LIRGs, LTIR > 10 11 L ) and is comprised entirely of LIRGs and ultra-luminous infrared galaxies (ULIRGs, LTIR> 10 12 L ) at z> 0:6. We observe weak clustering of r0 3- 6 h -1 Mpc for almost all of our star forming samples. We find that the clustering and halo mass depend on LTIR at all redshifts, where galaxies with higher LTIR (hence higher SFRs) have stronger clustering. Galaxies with the highest SFRs at each redshift typically reside within dark matter halos of Mhalo 10 12:9 h -1 M . 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 (LTIR & 10 11:7 L ) at 0:6

Keywords:

• Dark matter
• Luminous infrared galaxy
• Star formation
• Star cluster
• Halo
• Astrophysics
• Stars
• Physics
• Galaxy
• Redshift

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