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Figure 51: Upper panel: CFHTLS all-sky previews available via Aladin server. Lower Panel: From the whole sky view to M101: an example of CFHTLS Wide u-band multi-resolution all-sky preview. 104
7 Acknowledgements We thank Emmanuel Bertin for practical advice on the use of the AstrOmatic software suite; the CFHT staff, in particular the QSO team; the SNLS team, in particular Pierre Astier, Ray Carlberg, Julien Guy, Chris Pritchet, Raynald Pain; CADC, in particular JJ Kavelaars and John Ouelette; the CDS in Strasbourg; the CFHTLS Data Operation Group and the CFHTLS Steering Group. Terapix is funded by the French national research agency (CNRS/INSU), the Programme National Cosmologie et Galaxies (PNCG), the Service d’Astrophysique of the Commissariat à l’Energie Atomique (CEA/SAp), the Institut d’Astrophysique de Paris (IAP), the Agence National de la Recherche (ANR) grants ECOSSTAT, DESIR and TG_REGALDIS, and the European FP5 RTD contracts “Astrowise” and “AVO” (Astrophysical Virtual Observatory). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This survey makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. 105
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T0007 : The Final CFHTLS Release Pa
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patches are provided. Sources from
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Contents 1 CFHTLS-T0007 Executive S
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B.1 Rescaling factors applied to de
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33 Galaxy counts for the four Wide
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30 Description of parameters listed
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B A B A B A B A B A B A B A B A B A
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constraints. Two series of Deep sta
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evealed minor problems (such as unu
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een preferable because of the highe
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Figure 5: Outputs of the SCAMP cali
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Figure 7: CFHTLS T0007 absolute pho
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Figure 8: Seeing FWHM distribution
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Figure 10: Aperture correction (def
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Filter u g r i z - ApCorr - ApCorr
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Figure 14: Photometric calibration
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Figure 17: Photometric calibration
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Figure 18: Matching between one L99
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• four (u, g, r , i/y, z) Wide pa
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W1 W2 N N E E W3 W4 N N E E Figure
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CFHTLS Reference center Total Total
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Each tile is centered at a well-def
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Field Parameter u ∗ g r i y z W1
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Figure 23: Distribution of exposure
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Figure 25: Distribution of the medi
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All CFHTLS Wide images: (mean CCD s
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50% completeness are given for poin
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80% completeness limit (stars) 26.0
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10 5 W1 W2 W3 10 5 W1 W2 W3 N gal 0
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Wide Field Magnitude range u ∗ g
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Wide Field Magnitude range u ∗ g
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paths. From the joint effort betwee
Page 66 and 67: Wide field External magnitude offse
Page 68 and 69: Wide field External rms errors with
Page 70 and 71: Figure 38: Comparison of one CFHTLS
Page 72 and 73: 4.5.2 Absolute astrometric accuracy
Page 74 and 75: 4.6 Outliers, stacks with exception
Page 76 and 77: Figure 40: Mean RA-DEC offsets betw
Page 78 and 79: Figure 42: Mean RA-DEC offsets betw
Page 80 and 81: W Cartesian CFHTLS Special filter V
Page 82 and 83: accurately reflect the integration
Page 84 and 85: Field Parameter u ∗ g r i y z D1-
Page 86 and 87: Field Parameter u ∗ g r i y z D1-
Page 88 and 89: 76 Figure 43: Comparison of the (u
Page 90 and 91: Figure 44: Estimation of the intern
Page 92 and 93: 5.4 Depth and completeness limits T
Page 94 and 95: D2 u−band (25% best−seeing imag
Page 96 and 97: log Ngal 0.5 mag −1 deg −2 5 4
Page 98 and 99: - there is one chi2 image per Wide
Page 100 and 101: File name Content Data Size Number
Page 102 and 103: File name Content Data Size Number
Page 104 and 105: 6.3 Content of CFHTLS source catalo
Page 106 and 107: stacks made with the y-(i.MP9702) f
Page 108 and 109: Id Parameter Description Units Comm
Page 110 and 111: 6.4 The QualityFITS input and outpu
Page 112 and 113: Figure 48: QFITS-out page of the W4
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Page 118 and 119: A CFHTLS T0007 Wide supplementary i
Page 120 and 121: Table 31 - Continued from previous
Page 122 and 123: A.2 List of images in each Wide sta
Page 138 and 139: DISTORT_GROUPS 1,1 # Polynom group
Page 140 and 141: #--------------------------- Photom
Page 142 and 143: #--------------------------- Photom
Page 144 and 145: #--------------------------- Photom
Page 146 and 147: #--------------------------- Backgr
Page 148 and 149: #--------------------------- Backgr
Page 150 and 151: #------------------------- Star/Gal
Page 152 and 153: #--------------------------- Star/G
Page 154 and 155: B.2 CFHTLS T0007 Deep configuration
Page 156 and 157: SCAMP astrometric run using interna
Page 158 and 159: SCAMP photometric run (D1,D2,D3,D4)
Page 160 and 161: B.2.2 SWarp stack configuration fil
Page 162 and 163: B.2.3 SWarp chi2-image configuratio
Page 164 and 165: B.2.4 SExtractor .ldac catalogue co
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B.2.5 SExtractor DUAL MODE .cat cat
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Acronyms & Abbreviations ASCII CADC
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References Astier, P., et al. 2006,
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