SIMBAD references

We present a new near-infrared imaging survey in the four CFHTLS deep fields: the WIRCam Deep Survey or ``WIRDS''. WIRDS comprises extremely deep, high quality (FWHM∼0.6") J, H, and K<sub>s</sub> imaging covering a total effective area of 2.1°2 and reaching AB 50% completeness limits of ≃24.5. We combine our images with the CFHTLS to create a unique eight-band ugrizJHK<sub>S</sub> photometric catalogues in the four CFHTLS deep fields; these four separate fields allow us to make a robust estimate of the effect of cosmic variance for all our measurements. We use these catalogues in combination with ≃9800 spectroscopic redshifts to estimate precise photometric redshifts (σ<sub>Δz/(1+z)</sub>≲0.03 at i<25), galaxy types, star-formation rates and stellar masses for a unique sample of ≃1.8 million galaxies. Our JHK<sub>s</sub> number counts are consistent with previous studies. We apply the ``BzK'' selection to our gzK filter set and find that the star forming BzK selection successfully selects 76% of star-forming galaxies in the redshift range 1.4<z<2.5 in our photometric catalogue, based on our photometric redshift measurement. Similarly the passive BzK selection returns 52% of the passive 1.4<z<2.5 population identified in the photometric catalogue. We present the mass functions of the total galaxy population as a function of redshift up to z=2 and present fits using double Schechter functions. A mass-dependent evolution of the mass function is seen with the numbers of galaxies with masses of M≲10^10.75 still evolving at z≲1, but galaxies of higher mass reaching their present day numbers by z∼0.8-1. This is consistent with the present picture of downsizing in galaxy evolution. We compare our results with the predictions of the GALFORM semi-analytical galaxy formation model and find that the simulations provide a relatively successful fit to the observed mass functions at intermediate masses (i.e. 10≲log(M/M_☉)≲11). However, as is common with semi-analytical predictions of the mass function, the GALFORM results under-predict the mass function at low masses (i.e. log(M/M_☉)≲10), whilst the fit as a whole degrades beyond redshifts of z∼1.2. All photometric catalogues and images are made publicly available from TERAPIX and CADC.