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J/A+A/535/A65     Galaxy clusters in the 4 CFHTLS Wide fields    (Durret+, 2011)

Galaxy cluster searches based on photometric redshifts in the four CFHTLS Wide fields. Durret F., Adami C., Cappi A., Maurogordato S., Marquez I., Ilbert O., Coupon J., Arnouts S., Benoist C., Blaizot J., Edorh T.M., Garilli B., Guennou L., Le Brun V., Le Fevre O., Mazure A., McCracken H.J., Mellier Y., Mezrag C., Slezak E., Tresse L., Ulmer M.P. <Astron. Astrophys. 535, A65 (2011)> =2011A&A...535A..65D
ADC_Keywords: Clusters, galaxy ; Redshifts Keywords: large-scale structure of Universe - galaxies: clusters: general - surveys Abstract: We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg2, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1≤z≤1.15, with estimated mean masses between 1.3x1014 and 12.6x1014M. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file wide1.dat 32 3247 Cluster positions and magnitudes in Wide 1 wide2.dat 32 919 Cluster positions and magnitudes in Wide 2 wide3.dat 32 1819 Cluster positions and magnitudes in Wide 3 wide4.dat 32 817 Cluster positions and magnitudes in Wide 4
See also: J/A+A/509/A81 : Candidate clusters detected in six CFHTLS fields (Adami+, 2010) Byte-by-byte Description of file: wide1.dat wide2.dat wide3.dat wide4.dat
Bytes Format Units Label Explanations
1- 2 A2 --- Field [W1234] Field name (W1-W4) 3 A1 --- --- [-] 4- 7 I4 --- Seq Running number within the field 9- 16 F8.4 deg RAdeg Right ascension in decimal degrees (J2000.0) 18- 25 F8.4 deg DEdeg Declination in decimal degrees (J2000.0) 27- 30 F4.2 --- zphot Photometric redshift 32 I1 --- S/N Signal to noise or significance level
Acknowledgements: Florence Durret, durret(at)
(End) Patricia Vannier [CDS] 13-Sep-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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