Luminosity‐Dependent Clustering of Star‐formingBzKGalaxies at Redshift 2

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Abstract
We use the BzK color selection proposed by Daddi et al. (2004) to obtain a sample of 1092 faint star-forming galaxies (hereafter sBzKs) from 180 arcmin^2 in the Subaru Deep Field. This sample represents star-forming galaxies at 1.4 < z < 2.5 down to K(AB)=23.2, which roughly corresponds to a stellar-mass limit of ~ 1 x 10^{10} Msun. We measure the angular correlation function (ACF) of these sBzKs to be w(theta) = (0.58 +- 0.13) x theta["]^{-0.8} and translate the amplitude into the correlation length assuming a reasonable redshift distribution. The resulting value, r0 = 3.2^{+0.6}_{-0.7} h^{-1} Mpc, suggests that our sBzKs reside in haloes with a typical mass of 2.8 x 10^{11} Msun. Combining this halo mass estimate with those for brighter samples of Kong et al. (2006), we find that the mass of dark haloes largely increases with K brightness, a measure of the stellar mass. Comparison with other galaxy populations suggests that faint sBzKs (K(AB)<23.2) and Lyman Break Galaxies at z ~ 2 are similar populations hosted by relatively low-mass haloes, while bright sBzKs (K(AB)<21) reside in haloes comparable to or more massive than those of Distant Red Galaxies and Extremely Red Objects. Using the extended Press-Schechter formalism, we predict that present-day descendants of haloes hosting sBzKs span a wide mass range depending on K brightness, from lower than that of the Milky Way up to those of richest clusters.
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