%0 Journal Article
%A Pelló, R.
%A Hudelot, P.
%A Laporte, N.
%A Mellier, Y.
%A McCraken, H.J.
%A Balcells, M.
%A Boone, F.
%A Cardiel López, Nicolás
%A Gallego Maestro, Jesús
%A Garzón, F.
%A Guzmán, R.G.
%A Le Borgne, J.F.
%A Prieto, M.
%A Richard, J.
%A Schaerer, D.
%A Tresse, L.
%A Arnouts, S.
%A Cuby, J.G.
%A Disseau, K.
%A Hayes, M.
%T The WIRCam Ultra Deep Survey (WUDS) I. Survey overview and UV luminosity functions at z similar to 5 and z similar to 6
%D 2018
%@ 1432-0746
%U https://hdl.handle.net/20.500.14352/13064
%X The aim of this paper is to introduce the WIRCam Ultra Deep Survey (WUDS), a near-IR photometric survey carried out at the CFH Telescope in the field of the CFHTLS-D3 field (Groth Strip). WUDS includes four near-IR bands (Y, J, H and Ks) over a field of view of ∼400 arcmin^(2) . The typical depth of WUDS data reaches between ∼26.8 in Y and J, and ∼26 in H and K_(s) (AB, 3σ in 1.3´´ aperture), whereas the corresponding depth of the CFHTLS-D3 images in this region ranges between 28.6 and 29 in ugr, 28.2 in i and 27.1 in z (same S/N and aperture). The area and depth of this survey were specifically tailored to set strong constraints on the cosmic star formation rate and the luminosity function brighter or around L* in the z ∼ 6−10 redshift domain, although these data are also useful for a variety of extragalactic projects. This first paper is intended to present the properties of the public WUDS survey in details: catalog building, completeness and depth, number counts, photometric redshifts, and global properties of the galaxy population. We have also concentrated on the selection and characterization of galaxy samples at z ∼ [4.5−7] in this field. For these purposes, we include an adjacent shallower area of ∼1260 arcmin^(2) in this region, extracted from the WIRCam Deep Survey (WIRDS), and observed in J, H and Ks bands. UV luminosity functions were derived at z ∼ 5 and z ∼ 6 taking advantage from the fact that WUDS covers a particularly interesting regime at intermediate luminosities, which allows a combined determination of M* and Φ* with increased accuracy. Our results on the luminosity function are consistent with a small evolution of both M* and Φ* between z = 5 and z = 6, irrespective of the method used to derive them, either photometric redshifts applied to blindly-selected dropout samples or the classical Lyman Break Galaxy color-preselected samples. Our results lend support to higher Φ* determinations at z = 6 than usually reported. The selection and combined analysis of different galaxy samples at z ≥ 7 will be presented in a forthcoming paper, as well as the evolution of the UV luminosity function between z ∼ 4.5 and 9. WUDS is intended to provide a robust database in the near-IR for the selection of targets for detailed spectroscopic studies, in particular for the EMIR/GTC GOYA Survey.
%~