We present measurements of the clustering properties of bright ( L > L _ { * } ) z \sim 4 Lyman Break Galaxies ( LBGs ) selected from the Oxford-Dartmouth Thirty Degree Survey ( ODT ) .
We describe techniques used to select and evaluate our candidates and calculate the angular correlation function which we find best fitted by a power law , \omega ( \theta ) = A _ { w } \theta ^ { - \beta } with A _ { w } = 15.4 ( with \theta in arcseconds ) , using a constrained slope of \beta = 0.8 .
Using a redshift distribution consistent with photometric models , we deproject this correlation function and find a comoving r _ { 0 } = 11.4 _ { -1.9 } ^ { +1.7 } h _ { 100 } ^ { -1 } Mpc in a \Omega _ { m } = 0.3 flat \Lambda cosmology for i _ { AB } \leq 24.5 .
This corresponds to a linear bias value of b = 8.1 _ { -2.6 } ^ { +2.0 } ( assuming \sigma _ { 8 } = 0.9 ) .
These data show a significantly larger r _ { 0 } and b than previous studies at z \sim 4 .
We interpret this as evidence that the brightest LBGs have a larger bias than fainter ones , indicating a strong luminosity dependence for the measured bias of an LBG sample .
Comparing this against recent results in the literature at fainter ( sub- L _ { * } ) limiting magnitudes , and with simple models describing the relationship between LBGs and dark matter haloes , we discuss the implications on the implied environments and nature of LBGs .
It seems that the brightest LBGs ( in contrast with the majority sub- L _ { * } population ) , have clustering properties , and host dark matter halo masses , that are consistent with them being progenitors of the most massive galaxies today .