artefacts, following the same method as described in @Delorme.2008b. Since brown dwarfs are point sources, this morphological rejection of all non-point-source-like objects effectively removes many non-stellar contaminants.

This automated selection produces an average of 6 candidates per square degree. Each of these is visually examined to remove remaining contaminants. In addition to inspecting both the $z'$-band and the $J$-band images, we examine the $i'$-band image (available from the CFBDS), to reject some variable contaminants, as well as possible contamination by atypical broad absorption line quasars, none of which is known to be very red in both $z'-J$ and $i'-z'$ [P.Hall, private communication and @Hall.2002]. Since the 5$\sigma$ detection limits of the CFBDS $i'$ images (between 24.5 and 25.5) are significantly deeper than the $z'$ images, broad absorption line quasars with $z'-J>3.5$ should be visible on the $i'$ image. We identified one such object, CFBDSIR232451-045852, with $z'-J=$4.7 and $i'-z'$=0.9.

Very high-redshift (z$>$6), star-forming galaxies and evolved galaxies with strong Balmer/4000Å breaks at z$\sim$2, shown in Fig. \[wilkins\], are other possible contaminants. While the surface density of J$\sim$20 high-redshift, star-forming galaxies is unknown (the brightest of these objects discovered so far have J$_{vega}\sim$25 [@Ouchi.2009], five magnitudes fainter than our detection limit), the 