  We present an analysis of the clustering of galaxies from z ~ 2 to the
present day using the WIRCam Deep Survey (WIRDS). WIRDS combines deep
near-infrared data with the deep optical data from the CFHTLS Deep fields,
providing a photometric data-set over an effective area of 2.4 sq. deg., from
which accurate photometric redshifts and stellar masses can be estimated. We
use the data to calculate the angular correlation function for galaxy samples
split by star-formation activity, stellar mass and redshift. We estimate the
real-space clustering for each sample, determining clustering lengths and
power-law slopes. For galaxies selected by constant mass, we find that the
clustering scale shows no evolution up to z ~ 2. Splitting the galaxy sample by
mass, we see that higher mass galaxies have larger clustering scales at all
redshifts. We use our results to test the GALFORM semi-analytical galaxy
formation model and find the two are consistent. We split the galaxy population
into passive and star-forming populations and find that the passive galaxy
population shows a significantly larger clustering scale at all redshifts than
the star-forming population below masses of ~$10^{11}M_\odot/h$, showing that
even at z ~ 2 passive galaxies exist in denser environments than the bulk of
the star-forming galaxy population. For star-forming galaxies with stellar
masses $>10^{11}M_\odot/h$, we find a clustering strength of ~8Mpc/h across all
redshifts, comparable to the measurements for the passive population. Also, for
star-forming galaxies we see that clustering strength increases for higher
stellar mass systems, however there is little sign of a mass dependence in
passive galaxies. Finally, we investigate the connection between galaxy stellar
mass and dark matter halo mass, showing a clear correlation between the two in
both the WIRDS data and the GALFORM predictions.
