with the areas covered by each survey. The similar table 1 in @Delorme.2008b incorrectly uses the maximal magnitude limit for the CFHTLS-WIDE, instead of the average one. The value of 23.3 stated in Table \[maglim\] here corrects this error. The 335 square degrees CFBDSIR probes about 2.8 times more volume for late T-dwarfs than the $\sim$900 square degree CFBDS, and even more for redder (and thus likely cooler) objects. Figure \[cfbdsir\_map\] shows the sky coverage of CFBDSIR as of March 2010. The optical data is public and available on the CFHT archive, while the NIR data becomes public after the standard one-year CFHT proprietary period.\

![Map of observed CFBDSIR fields as of March 2010. Dashed lines are +/-20 degrees of galactic latitude. \[cfbdsir\_map\]](14277fg1.ps){width="8cm"}

[|X|X|X|X|X|X|]{} Survey Name& $z'_{AB}$ $10\sigma$ ($5\sigma$) detection limit& mid-L maximal detection (pc) & mid-T maximal detection (pc) & T9 maximal detection (pc) & Final coverage (sq deg)\
CFBDS:RCS-2 & 22.5 (23.25) & 185 & 80 &16 & 600\
CFBDS:CFHTLS-Very Wide & 22.8 (23.55) & 215 & 90 & 18 & 150\
CFBDS:CFHTLS-Wide & 23.3 (24.05) & 270 & 115 & 22 & 170\
Survey Name& $J_{vega}$ $10\sigma$ detection limit & mid-L maximal detection (pc) & mid-T maximal 