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J/A+A/613/A67  Candidate clusters in 4 CFHTLS T0007 Wide fields  (Sarron+, 2018)

Evolution of the cluster optical galaxy luminosity function in the CFHTLS: breaking the degeneracy between mass and redshift. Sarron F., Martinet N., Durret F., Adami C. <Astron. Astrophys. 613, A67 (2018)> =2018A&A...613A..67S (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Redshifts Keywords: galaxies: clusters: general - galaxies: evolution - galaxies: luminosity function, mass function Abstract: Obtaining large samples of galaxy clusters is important for cosmology: cluster counts as a function of redshift and mass can constrain the parameters of our Universe. They are also useful in order to understand the formation and evolution of clusters. We develop an improved version of the Adami & MAzure Cluster FInder (AMACFI), now the Adami, MAzure & Sarron Cluster FInder (AMASCFI), and apply it to the 154deg2 of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) to obtain a large catalogue of 1371 cluster candidates with mass M200>1014M{sun} and redshift z≤0.7. We derive the selection function of the algorithm from the Millennium simulation, and cluster masses from a richness-mass scaling relation built from matching our candidates with X-ray detections. We study the evolution of these clusters with mass and redshift by computing the i'-band galaxy luminosity functions (GLFs) for the early-type (ETGs) and late-type galaxies (LTGs). This sample is 90% pure and 70% complete, and therefore our results are representative of a large fraction of the cluster population in these redshift and mass ranges. We find an increase in both the ETG and LTG faint populations with decreasing redshift (with Schechter slopes σETG=-0.65±0.03 and σLTG=-0.95±0.04 at z=0.6, and σETG=-0.79±0.02 and σLTG=-1.26±0.03 at z=0.2) and also a decrease in the LTG (but not the ETG) bright end. Our large sample allows us to break the degeneracy between mass and redshift, finding that the redshift evolution is more pronounced in high-mass clusters, but that there is no significant dependence of the faint end on mass for a given redshift. These results show that the cluster red sequence is mainly formed at redshift z>0.7, and that faint ETGs continue to enrich the red sequence through quenching of brighter LTGs at z≤0.7. The efficiency of this quenching is higher in large-mass clusters, while the accretion rate of faint LTGs is lower as the more massive clusters have already emptied most of their environment at higher redshifts. Description: We have updated the Adami & MAzure Cluster FInder (AMACFI, Mazure et al., 2007A&A...467...49M) and applied it to the CFHTLS final data release T0007 photometric redshift (hereafter photo-z, symbol zphot) catalogues. The original AMACFI algorithm was already applied to the CFHTLS in previous studies: Mazure et al. (2007A&A...467...49M) for the Deep1 field, Adami et al. (2010, Cat. J/A+A/509/A81) for the T0004 data release, and Durret et al. (2011, Cat. J/A+A/535/A65) for the Wide fields of the T0006 data release. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file catalog.dat 101 7100 *Candidate clusters detected using the AMASCFI algorithm in the 4 Wide fields of CFHTLS T0007 catalog.fits 2880 130 Fits version of the catalog
Note on catalog.dat: All clusters with S/N>3 and 0.15<z<1.1 are included (7100 clusters). Only clusters with S/N>4 and z<0.7 have a richness and M200 estimate (2710 clusters).
See also: J/A+A/509/A81 : Candidate clusters detected in six CFHTLS fields (Adami+, 2010) J/A+A/535/A65 : Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011) Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 7 A7 --- IdClus Cluster Identification in the catalog 10- 20 F11.7 deg RAdeg Cluster right ascension (J2000) 23- 34 F12.8 deg DEdeg Cluster declination (J2000) 37- 40 F4.2 --- zclus Cluster redshift 42- 45 F4.1 --- S/N Cluster signal-to-noise ratio 47- 51 F5.2 --- R-AMASCFI ?=- Cluster richness (as computed by AMASCFI, see paper for details) 53- 56 F4.2 --- e_R-AMASCFI ?=- Error on cluster richness (as computed by AMASCFI) 58- 71 E14.9 --- M200 ?=- Median M200, mass contained in a radius r200, inside which the density is 200 times the critical density of the Universe (1) 73- 86 E14.9 --- e_M200 ?=- 68% lower confidence limit on M200 (1) 88-101 E14.9 --- E_M200 ?=- 68% upper confidence limit on M200 (1)
Note (1): obtained from a mass-richness scaling relation, using X-ray detected clusters. See paper for details.
Acknowledgements: Florian Sarron, sarron(at)
(End) Patricia Vannier [CDS] 01-Jun-2018
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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