Astronomy and Astrophysics, volume 620A, 51-51 (2018/12-1)
The WIRCam Ultra Deep Survey (WUDS). I. Survey overview and UV luminosity functions at z ∼ 5 and z ∼ 6.
PELLO R., HUDELOT P., LAPORTE N., MELLIER Y., McCRACKEN H.J., BALCELLS M., BOONE F., CARDIEL N., GALLEGO J., GARZON F., GUZMAN R., LE BORGNE J.F., PRIETO M., RICHARD J., SCHAERER D., TRESSE L., ARNOUTS S., CUBY J.G., DISSEAU K. and HAYES M.
Abstract (from CDS):
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-arcmin2. The typical depth of WUDS data reaches between ∼26.8 in Y and J, and ∼26 in H and Ks (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-arcmin2 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.