Galaxy cluster searches based on photometric redshifts in the four CFHTLS Wide fields

Abstract

Context. Cosmological parameters can be constrained by counting clusters of galaxies as a function of mass and redshift and by considering regions of the sky sampled as deeply and as homogeneously as possible. Aims. Several methods for detecting clusters in large imaging surveys have been developed, among which the one used here, which is based on detecting structures. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007, A&A, 467, 49), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, A&A, 509, A81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we use the same method to analyse the full CFHTLS Wide survey, based on the T0006 data release. Methods. Our method is based on the photometric redshifts computed with Le Phare for all the galaxies detected in the Wide fields, limited to magnitudes z ≤ 22.5. We constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique, detected structures with SExtractor at various detection levels, and built cluster catalogues by applying a minimal spanning tree algorithm. Results. In a total area of 154 deg 2 , we have detected 4061 candidate clusters at 3σ or above (6802 at 2σ and above), in the redshift range 0.1 ≤ z ≤ 1.15, with estimated mean masses between 1.3 × 10 14 and 12.6 × 10 14 M . This catalogue of candidate clusters will be available at the CDS. 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 the one obtained for other cluster surveys and analyse large-scale filamentary galaxy distributions. Conclusions. 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 if they are located at the intersection of filaments by which they are fed.

The NuSTAR Extragalactic Surveys: Source Catalog and the Compton-thick Fraction in the UDS Field

“…located in a part of the mosaic where only XMM-Newton coverage is available, but it is not matched to any SXDS source. At its position, Sloan Digital Sky Survey maps show the presence of a group of galaxies, which is indeed detected as a galaxy cluster in the CFHTLS 4 Wide Fields Galaxy Clusters catalog (Durret et al 2011) at z phot ∼0.45. Moreover, two galaxies of the group are detected by WISE (Wright et al 2010) and are 4 7 and 11 5 away from the NuSTAR position.…”

The XXL Survey

“…Based on a cluster search using photometric redshifts in the CFHTLS wide fields, Durret et al (2011) identified one potential cluster at z phot = 0.48 located at RA = 32.7603, Dec = −6.1936, and ∼6.55 away from our XLSSC 085 cluster; this corresponds approximately to the position of the BCG of XLSSC 084.…”

Diffuse light in the young cluster of galaxies CL J1449+0856 atz= 2.07

“…Even with the most favourable cluster-cluster angular correlation functions (e.g. Durret et al 2011), the probability of finding three groups hotter than 2 keV (Romer et al 2001) in a 10 × 10 arcsec 2 area to explain S1, S2, and S3 is completely negligible (≤10 −14 ). We can therefore conclude quite securely that the best possibility to have detected three such low surface-brightness objects in such a small area is to have detected diffuse light sources related to the CL J1449+0856 cluster.…”