Matthieu BETHERMIN
(CEA Saclay)
We studied the link between the physical properties of galaxies and the mass of their host halo at z∼2 trough clustering measurements and halo occupation distribution modeling. Our sample of galaxy is selected using a BzK criterion in the COSMOS field. We split our sample into three sub-samples: passive, "main-sequence" (i.e. galaxies following a narrow correlation between stellar mass and star-formation rate) and starburst (defined here has having an excess of specific star formation rate of a factor 3 or more compared to the "main-sequence") galaxies. The properties of passive and "main-sequence" galaxies are determined using optical/near-infrared data. The starburst galaxies are in general very dust-obscured and \textit{Herschel}/PACS data are necessary to derive accurately their star formation rate. We found that the stellar-to-halo mass relation of both passive and star-forming galaxies ("main- sequence" and starburst) agree with the estimates based on abundance matching, showing an halo mass increasing with stellar mass. We also measured that halo mass increase with star formation rate for "main-sequence" galaxies. On the contrary, we detected no evolution of the halo mass as a function of the specific star formation rate for a mass-selected sample. However, we found an excess of clustering at small scale (few tens of arcsec) for passive and starburst galaxies which could be linked to environmental effects and/or mergers.