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W Cartesian CFHTLS Special filter VIPERS-DDT images Comments Ident name Ident name W1(+4 + 1) 023319-060400 g-band W1(+4 + 2) 023319-050800 y-band observations g-band W1(+4 + 3) 023319-041200 i-band : CCD#03 missing W2(−1 + 3) 085011-012700 g-band : CCD#03 missing W2(+1 + 1) 085749-031900 y-band observations W2(+3 + 1) 090526-031900 g-band : CCD#03 missing W2(+3 + 2) 090526-022300 g-band : CCD#03 missing W2(+3 + 3) 090526-012700 g-band : CCD#03 missing W2(+2 + 2) 090137-022300 y-band observations W3(−3 + 1) 135846+552631 y-band observations W3(−2 − 0) 140525+543031 u ∗ , g, r, i, z contamination: Messier 101 galaxy on the 4 th (bottom right) MegaCam quadrant W3(−2 − 1) 140540+533431 y-band observations W3(−2 + 1) 140509+552631 y-band observations W3(−2 + 3) 140433+571831 y-band observations W3(−1 + 3) 141113+571831 y-band observations y-band radial astrometric offset 0.077" W3(−0 − 1) 141754+533431 g-band seeing anomaly: 1.045" W3(+3 − 1) 143615+533431 y-band observations W3(+3 + 2) 143728+562231 y-band observations W4(+1 − 1) 221706+002300 W4(−1 − 1) 220930+002300 y-band observations W4(−1 + 1) 220930+021500 y-band observations W4(−1 + 2) 220930+031100 y-band observations W4(−1 + 3) 220930+040700 y-band observations W4(−2 + 2) 220542+031100 y-band observations W4(−2 + 3) 220542+040700 y-band observations W4(−3 + 3) 220154+040700 y-band observations Table 16: CFHTLS Wide stacks with exceptions or anomalies (cont’d). 68
Field name Reference center Comment RA DEC (J2000) (J2000) D1 02:25:59.00 −04:29:40 D2 10:00:28.00 +02:12:30 COSMOS u ∗ data included D3 14:19:27.00 +52:40:56 D4 22:15:31.00 −17:43:56 Table 17: Location of the CFHTLS Deep fields. All fields cover 1 deg 2 and are taken in all six filters. 5 Description of the CFHTLS T0007 Deep survey 5.1 Overview The CFHTLS Deep survey is composed of four independent MegaCam pointings in the D1, D2, D3 and D4 fields, whose sky location is shown in Figure 1, observed in all six MegaCam filters. It is composed of 96 u ∗ , g, r, i, y and z stacks and 16 chi2 images (that is 112 images including the weight-maps). There are two types of stacks per Deep field: the “85%” best seeing images (hereafter the Dk-85 sample, k = 1 − 4) and the “25%” best seeing images (Dk-25). The two Dk series of stacks have exactly the same center positions. The image selection criteria applied to the 10632 CFHTLS images for the production of the CFHTLS Deep survey has already been described in Section 3.4. Note that in addition to the CFHTLS images taken between May 26, 2003 and February 02, 2009 on the D2-u∗ field contains MegaCam images taken by the COSMOS consortium (Capak et al., 2007). The T0007 CFHTLS Deep survey contains in total 8916 images. After proper selection, the remaining 8638 images were combined into stacks as follows: 634 u ∗ , 1457 g, 1932 r, 1990 i, 691 y and 1934 z. All stacks have the same pixel scale and cover exactly 1×1 deg 2 (19354×19354 pixels of 0.1860"). For all fields with the exception of D2-u ∗ the stacks are only composed of images that are part of a CFHTLS Deep observing sequence and that are within a radius of 3 arc-minutes with respect to the CFHTLS Deep center fields. For the D2-u ∗ , we included all u ∗ -COSMOS images that passed the selection, without restriction on the radial distance. The Deep stacks combine sets of images obtained during sequences of medium exposures (few hundreds of seconds). Each exposure is followed by a small shift of the telescope to fill the physical gaps between CCDs. The shifts are within a box of 4 ′ in DEC and 3 arcminutes in RA. The D2-u ∗ stacks COSMOS data are shifted by 30 arcminutes in both RA and DEC directions in order to pave the 1.4×1.4 deg 2 of the COSMOS survey. These images are combined with CFHTLS D2-u ∗ observations and cut to provide the 1×1 deg 2 centered on the CFHTLS D2. The center position of each stack is predefined. The coordinates of a stack center position are given in Table 17, and are exactly the same for all filters. D1, D2, D3 and D4 are therefore composed of a complete set of u ∗ , g, r, i, y and z images of 1 deg 2 each. Tables 18 and 19 summarize the properties of Deep median-combined stacks; the characteristics of the sigma-combined stacks are given in Tables20 and 21. (Note that the exposure time u ∗ -band does not 69
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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
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 50 and 51: Figure 25: Distribution of the medi
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 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 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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Table 32 - Continued from previous
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DISTORT_GROUPS 1,1 # Polynom group
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#--------------------------- Photom
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#--------------------------- Photom
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#--------------------------- Photom
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#--------------------------- Backgr
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#--------------------------- Backgr
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#------------------------- Star/Gal
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#--------------------------- Star/G
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B.2 CFHTLS T0007 Deep configuration
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SCAMP astrometric run using interna
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SCAMP photometric run (D1,D2,D3,D4)
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B.2.2 SWarp stack configuration fil
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B.2.3 SWarp chi2-image configuratio
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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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