The VIPERS Multi-Lambda Survey

I. UV and near-IR observations, multi-colour catalogues, and photometric redshifts^⋆,⋆⋆

¹ Aix Marseille Université, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, 38 rue F. Joliot-Curie, 13388 Marseille, France
e-mail: thibaud.moutard@lam.fr
² Astronomical Observatory of the University of Geneva, ch. d’Ecogia 16, 1290 Versoix, Switzerland
³ CNRS, UMR 7095 & UPMC, Institut d’Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
⁴ INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
⁵ INAF–Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate/via Brera 28, 20122 Milano, Italy
⁶ California Institute of Technology, Pasadena, CA 91125, USA
⁷ Institue for Astronomy, University of Hawaii, Honolulu, HI 96822, USA
⁸ Canada-France-Hawaii Telescope, 65-1238 Mamalahoa Highway, Kamuela, HI 96743, USA
⁹ Department of Astronomy, Columbia University, New York, NY 10027, USA
¹⁰ Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, V6T 1Z1, BC, Canada

Received: 10 December 2015
Accepted: 9 February 2016

Abstract

We present observations collected in the CFHTLS-VIPERS region in the ultraviolet with the GALEX satellite (far- and near-ultraviolet channels) and in the near-infrared with the CFHT/WIRCam camera (K_s band) over an area of 22 and 27 deg², respectively. The depth of the photometry was optimised to measure the physical properties (e.g., star formation rate, stellar masses) of all the galaxies in the VIPERS spectroscopic survey. The large volume explored by VIPERS will enable a unique investigation of the relationship between the galaxy properties and their environment (density field and cosmic web) at high redshift (0.5 ≤ z ≤ 1.2). In this paper, we present the observations, the data reductions, and the build-up of the multi-colour catalogues. The CFHTLS-T0007 (gri-χ²) images are used as reference to detect and measure the K_s-band photometry, while the T0007 u^∗-selected sources are used as priors to perform the GALEX photometry based on a dedicated software (EMphot). Our final sample reaches NUV_AB ~ 25 (at 5σ) and K_AB ~ 22 (at 3σ). The large spectroscopic sample (~51 000 spectroscopic redshifts) allows us to highlight the robustness of our star/galaxy separation and the reliability of our photometric redshifts with a typical accuracy of σ_z ≤ 0.04 and a fraction of catastrophic failures η ≤ 2% down to i ~ 23. We present various tests on the K_s-band completeness and photometric redshift accuracy by comparing our results with existing overlapping deep photometric catalogues. Finally, we discuss the BzK sample of passive and active galaxies at high redshift and the evolution of galaxy morphology in the (NUV−r) vs. (r−K_s) diagram at low redshift (z ≤ 0.25) based on the high image quality of the CFHTLS.