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Figure 25: Distribution of the median seeing over the Wide tiles. The seeing is the FWHM= √ a b derived with PSFEX, from the fitting of a 2-dimension Moffat model of the PSF. The mean seeing value over the MegaCam field of each stack is available at http://terapix.iap.fr/cplt/T0007/table_syn_T0007.html. is observed, the median seeing of each stack appears randomly distributed over the four Wide fields. Figure 27 shows the seeing fluctuations on MegaCam. The seeing is averaged over a CCD field of view and compared to the mean seeing over the whole MegaCam field. The statistics is based on 6378 input images used for the CFHTLS Wide T0007 release. For CCDs at the edges of the detector, the differences are important but never exceed 0.065", and the maximum peak-to-peak amplitude is less than 0.1" . This upper limit is acceptable. It still preserves the mean seeing over the whole MegaCam field of view below one arcsecond for all input images that will be combined into stacks. The legend of Figure 27 elaborates on the extreme corners of the MegaCam field of view which exhibit a rapid image quality degradation, but represent an area limited to just 3% of each image. 38
Figure 26: Maps of seeing (FWHM) in the CFHTLS Wide. Each small square represents a median seeing value over a 1 o × 1 o tile (or a stack) of the Wide survey. The panels show, from left to right: W1, W2, W3 and W4; from top to bottom: the u ∗ , g, r, i/y and z CFHTLS stacks. 39
Page 1: T0007 : The Final CFHTLS Release Pa
Page 4 and 5: patches are provided. Sources from
Page 6 and 7: Contents 1 CFHTLS-T0007 Executive S
Page 8 and 9: B.1 Rescaling factors applied to de
Page 10 and 11: 33 Galaxy counts for the four Wide
Page 12 and 13: 30 Description of parameters listed
Page 14 and 15: B A B A B A B A B A B A B A B A B A
Page 16 and 17: constraints. Two series of Deep sta
Page 18 and 19: evealed minor problems (such as unu
Page 20 and 21: een preferable because of the highe
Page 22 and 23: Figure 5: Outputs of the SCAMP cali
Page 24 and 25: Figure 7: CFHTLS T0007 absolute pho
Page 26 and 27: Figure 8: Seeing FWHM distribution
Page 28 and 29: Figure 10: Aperture correction (def
Page 30 and 31: Filter u g r i z - ApCorr - ApCorr
Page 32 and 33: Figure 14: Photometric calibration
Page 34 and 35: Figure 17: Photometric calibration
Page 36 and 37: Figure 18: Matching between one L99
Page 38 and 39: • four (u, g, r , i/y, z) Wide pa
Page 40 and 41: W1 W2 N N E E W3 W4 N N E E Figure
Page 42 and 43: CFHTLS Reference center Total Total
Page 44 and 45: Each tile is centered at a well-def
Page 46 and 47: Field Parameter u ∗ g r i y z W1
Page 48 and 49: Figure 23: Distribution of exposure
Page 52 and 53: All CFHTLS Wide images: (mean CCD s
Page 54 and 55: 50% completeness are given for poin
Page 56 and 57: 80% completeness limit (stars) 26.0
Page 58 and 59: 10 5 W1 W2 W3 10 5 W1 W2 W3 N gal 0
Page 60 and 61: Wide Field Magnitude range u ∗ g
Page 62 and 63: Wide Field Magnitude range u ∗ g
Page 64 and 65: 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
Page 114 and 115:
102
Page 116 and 117:
Figure 51: Upper panel: CFHTLS all-
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
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Page 126 and 127:
Page 128 and 129:
Page 130 and 131:
Page 132 and 133:
Page 134 and 135:
Page 136 and 137:
Page 138 and 139:
DISTORT_GROUPS 1,1 # Polynom group
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#--------------------------- 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
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#--------------------------- 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
Page 170 and 171:
References Astier, P., et al. 2006,
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