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 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 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 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:
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FileName Lrecl Records Explanations
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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
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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).
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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
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Bytes Format Units Label Explanations
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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)
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Note (1): obtained from a mass-richness scaling relation, using X-ray detected
clusters. See paper for details.
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Acknowledgements:
Florian Sarron, sarron(at)iap.fr
(End) Patricia Vannier [CDS] 01-Jun-2018