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In the theory of structure formation, galaxies are biased tracers of theunderlying matter density field. The statistical relation between galaxy andmatter density field is commonly referred as galaxy bias. In this paper, wetest the linear bias model with weak-lensing and galaxy clustering measurementsin the 2 square degrees COSMOS field (Scoville et al. 2007). We estimate thebias of galaxies between redshifts z=0.2 and z=1, and over correlation scalesbetween R=0.2 h^-1 Mpc and R=15 h^-1 Mpc. We focus on three galaxy samples,selected in flux (simultaneous cuts I_814W < 26.5 and K_s < 24), and instellar-mass (10^9 < M_* < 10^10 h^-2 Msun and 10^10 < M^*< 10^11 h^-2 Msun).At scales R > 2 h^-1 Mpc, our measurements support a model of bias increasingwith redshift. The Tinker et al. (2010) fitting function provides a good fit tothe data. We find the best fit mass of the galaxy halos to be log(M_200 h^-1Msun) = 11.7^+0.6_-1.3 and log(M_200 h^-1 Msun) = 12.4^+0.2_-2.9 respectivelyfor the low and high stellar-mass samples. In the halo model framework, bias isscale-dependent with a change of slope at the transition scale between the oneand the two halo terms. We detect a scale-dependence of bias with a turn-downat scale R=2.3\pm1.5 h^-1 Mpc, in agreement with previous galaxy clusteringstudies. We find no significant amount of stochasticity, suggesting that alinear bias model is sufficient to describe our data. We use N-body simulationsto quantify both the amount of cosmic variance and systematic errors in themeasurement.

COSMOS: Stochastic bias from measurements of weak lensing and galaxy clustering