We use the BzK color selection proposed by Daddi et al .
( 13 ) 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 \lesssim z \lesssim 2.5 down to K _ { AB } = 23.2 , which roughly corresponds to a stellar-mass limit of \simeq 1 \times 10 ^ { 10 } M _ { \odot } .
We measure the angular correlation function ( ACF ) of these sBzKs to be w ( \theta ) = ( 0.58 \pm 0.13 ) \times \theta [ \arcsec ] ^ { -0.8 } and translate the amplitude into the correlation length assuming a reasonable redshift distribution .
The resulting value , r _ { 0 } = 3.2 ^ { +0.6 } _ { -0.7 } h ^ { -1 } Mpc , suggests that our sBzKs reside in haloes with a typical mass of 2.8 \times 10 ^ { 11 } M _ { \odot } .
Combining this halo mass estimate with those for brighter samples of Kong et al .
( 26 ) , we find that the mass of dark haloes largely increases with K brightness , a measure of the stellar mass ; the dark halo mass increases by as much as 10 ^ { 2 - 3 } as K brightness increases by only a factor of \simeq 10 .
We also find that the halo occupation number , the number of galaxies hosted in a dark halo , is higher for brighter sBzKs .
Comparison with other galaxy populations suggests that faint sBzKs ( K _ { AB } < 23.2 ) and Lyman Break Galaxies at z \sim 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 .