The VIRMOS deep imaging survey: II: CFH12K BVRI optical data for the 0226-04 deep field

By H. McCracken, Mario Radovich, E. Bertin, Y. Mellier, M. Dantel-Fort, O. Fèvre, J. Cuillandre, S. Gwyn, S. Foucaud, G. Zamorani. 2003

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In this paper we describe in detail the reduction, preparation and reliability of the photometric catalogues which comprise the CFH12K-VIRMOS deep field. This region, consisting of four contiguous pointings of the CFH12K wide-field mosaic camera, covers a total area of 1: 2d eg 2 . The survey reaches a limiting magnitude of BAB 26:5, VAB 26:2, RAB 25:9 and IAB 25:0 (corresponding to the point at which our recovery rate for simulated point-like sources sources falls below 50%). In total the survey contains 90 729 extended sources in the magnitude range 18:0< IAB< 24:0. We demonstrate our catalogues are free from systematic biases and are complete and reliable down these limits. By comparing our galaxy number counts to previous wide-field CCD surveys, we estimate that the upper limit on bin-to-bin systematic photometric errors for the I lim- ited sample is10% in this magnitude range. We estimate that 68% of the catalogues sources have absolute per co-ordinate astrometric uncertainties less than j j0:38 00 andj j0:32 00 . Our internal (filter-to-filter) per co-ordinate astrometric uncertainties arej j0:08 00 andj j0:08 00 . We quantify the completeness of our survey in the joint space defined by object total magnitude and peak surface brightness. We also demonstrate that no significant positional incompleteness eects are present in our catalogues to IAB< 24:0. Finally, we present numerous comparisons between our catalogues and published literature data: galaxy and star counts, galaxy and stellar colours, and the clustering of both point-like and extended populations. In all cases our measurements are in excellent agreement with literature data to IAB< 24:0. This combination of depth and areal coverage makes this multi-colour catalogue a solid foundation to select galaxies for follow-up spectroscopy with VIMOS on the ESO-VLT and a unique database to study the formation and evolution of the faint galaxy population to z 1 and beyond.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7660db695175035ad6ce2777fbc5164714ca2952

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Citations in the corpus

The VIMOS VLT Deep Survey. Evolution of the luminosity functions by galaxy type up to z = 1.5 from first epoch data (2005, unknown): “Multicolour photometry is available for each field (Le Fèvre et al. 2004a): in particular, the B, V , R, I photometry for the 0226-04 deep field is described in detail in McCracken et al. (2003).”
CARS: the CFHTLS-Archive-Research Survey - II. Weighing dark matter halos of Lyman-break galaxies at z = 3–5 (2009, methodology): “Astrometric calibration of the i-band images with the Astrometrix (Radovich 2002; McCracken et al. 2003) software and the USNO-B1 astrometric catalogue (Monet et al. 2003) as a reference.”
The VIMOS VLT Deep Survey final data release: a spectroscopic sample of 35 016 galaxies and AGN out to z ~ 6.7 selected with 17.5 ≤ iAB ≤ 24.75 (2013, methodology): “The VVDS-Wide fields were observed with the CFH12K camera at CFHT (Le Fèvre et al. 2004a), reaching depths of IAB = 24 (3σ) (McCracken et al. 2003).”
The VIMOS VLT deep survey - First epoch VVDS-deep survey: 11 564 spectra with 17.5 $\leq$ I$_\textit{\textbf{\small AB}}$ $\leq$ 24, and the redshift distribution over 0 $\leq$ z $\leq$ 5 (2004, unknown): “In addition to the U, BVRI, JK surveys conducted by the VVDS team (Le Fèvre et al. 2004a; McCracken et al. 2003; Radovich et al. 2003; Iovino et al. 2005, respectively), multiwavelength surveys are carried out by the VVDS team or under data exchange agreements with other teams.”
The VIMOS VLT deep survey: the assembly history of the stellar mass in galaxies: from the young to the old universe (2007, unknown): “In particular, B, V , R, I photometry for the 0226-04 deep field, covering ∼1 deg2, has been obtained at CFHT and is described in detail in McCracken et al. (2003).”
The First Release COSMOS Optical and Near-IR Data and Catalog (2007, methodology): “…1995, ApJ, 455, 50 Lilly et al., 1996, ApJ, 460, L1+ Magnier, E. A. & Cuillandre, J.-C. 2004, PASP, 116, 449 McCracken et al., 2007, astro-ph/0704.2545 McCracken et al., 2003, A&A, 410, 17 Metcalfe et al., 2001, MNRAS, 323, 795 Monet et al., 1998, VizieR Online Data Catalog, 1252, 0 Monet et al.,…”
Evolution and Color Dependence of the Galaxy Angular Correlation Function: 350,000 Galaxies in 5 Square Degrees (2004, result): “The Large-Scale Structure of the Universe, (Princeton, N.J., Princeton Univ. Press) Postman, M., Lauer, T. R., Szapudi, I., & Oegerle, W. 1998, ApJ, 506, 33 Roche, N., & Eales, S. A. 1999, MNRAS, 307, 703 Roche, N., Shanks, T., Metcalfe, N., & Fong, R. 1993, MNRAS, 263, 360 Shepherd, C. W., et al. 2”
Spectral Energy Distributions of Hard X-Ray Selected Active Galactic Nuclei in the XMM-Newton Medium Deep Survey (2007, unknown): “The VVDS data set includes broadband photometric data in the B, V, R, and I filters, to an AB limiting magnitude (50% completeness for point sources) of 26.5, 26.2, 25.9, and 25.0, respectively (McCracken et al. 2003).”
Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelength Spitzer observations up to z ~ 2.5 (2009, methodology): “Photometric redshifts computed by Arnouts et al. (2007) are also available through the VVDS database (see also McCracken et al. 2003, Radovich et al. 2004, Iovino et al. 2005).”
THE LAST OF FIRST: THE FINAL CATALOG AND SOURCE IDENTIFICATIONS (2015, methodology): “23 shows the resolution required as a function of magnitude using therband galaxy counts from the CFHTLS-D1 1 deg2 survey (McCracken et al. 2003).”
CARS: the CFHTLS-Archive-Research Survey. I. Five-band multi-colour data from 37 sq. deg. CFHTLS-wid (2008, methodology): “Hence, we generate our object catalogues based on this colour rather than on a combination of all available colours such as aχ2 image (see e.g. McCracken et al. 2003).”
Integral field spectroscopy with SINFONI of VVDS galaxies I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6 (2009, methodology): “We have used CFHT legacy survey images with best seeing (<0.65′′) for VVDS-02h field galaxies (Figures A.1 to A.4) and CFH12K/CFHT (McCracken et al. 2003) images for VVDS-22h field galaxies (Figures A.5 to A.9).”
Photometric redshifts in the SWIRE Survey (2008, methodology): “In addition within XMM we have 10-band photometry (ugrizUBVRI) from the VVDS programme of McCracken et al (2003), Le Févre et al (2004) (0.79 sq deg), and very deep 5-band photometry (BVRi’z’) in 1.12 sq deg of the Subaru XMM Deep Survey (SXDS, Sekiguchi et al 2005, Furusawa et al 2008).”
Very weak lensing in the CFHTLS Wide: Cosmology from cosmic shear in the linear regime (2007, methodology): “The image re-centering, resampling and stacking are produced by SWarp6 (Bertin 2005b), using the same configuration and image processing parameters as those discussed by McCracken et al. (2003).”
Accurate photometric redshifts for the CFHT legacy survey calibrated using the VIMOS VLT deep survey (2006, methodology): “McCracken et al. (2003) describe in detail the photometry and the astrometry of the VVDS-0226-04 field.”
Post-starburst galaxies: more than just an interesting curiosity (2008, methodology): “V) = 0.027 (McCracken et al. 2003), moved to the galaxy rest frame and interpolated on to a common wavelength grid.”
Cosmological constraints from the 100-deg2 weak-lensing survey (2007, methodology): “Technical details of the data set are given in Van Waerbeke et al. (2001) and McCracken et al. (2003), while an overview of the VIRMOS-DESCART survey is given in Le Fèvre et al. (2004).”