Environmental effects on the galaxy luminosity function   in the cluster of galaxies Abell 496

Durret, F.; Adami, C.; Lobo, C.

doi:10.1051/0004-6361:20021077

Cited by 19 publications

(18 citation statements)

References 24 publications

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“…Durret et al (2002) find a slope of −1.79 ± 0.01 in I, whereas we find here a slope of −1.52 ± 0.05. Given our analysis of cosmic variance, we estimate the error from cosmic variance on the slope of Durret et al (2002) to be roughly 0.08. If this error estimate is correct, then the difference in faint-end slopes would be statistically significant.…”

Section: Comparison With Previous Analyses Of Abell 496contrasting

confidence: 95%

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The galaxy luminosity function of the Abell 496 cluster and its spatial variations

Boué¹,

Adami²,

Durret

et al. 2007

A&A

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Context. The faint end slopes of galaxy luminosity functions (LFs) in clusters of galaxies have been observed in some cases to vary with clustercentric distance and should be influenced by the physical processes (mergers, tides) affecting cluster galaxies. However, there is a wide disagreement on the values of the faint end LF slopes, ranging from −1 to −2.3 in the magnitude range −18 < M r < −14. Aims. We investigate the LF in the very relaxed cluster Abell 496. Methods. Our analysis is based on deep images obtained at CFHT with MegaPrime/MegaCam in four bands (u * g r i ) covering a 1 × 1 deg 2 region, which is centred on the cluster Abell 496 and extends to near its virial radius. The LFs are estimated by statistically subtracting a reference field taken as the mean of the 4 Deep fields of the CFHTLS survey. Background contamination is minimised by cutting out galaxies redder than the observed Red Sequence in the g − i versus i colour-magnitude diagram. Results. In Abell 496, the global LFs show a faint end slope of −1.55 ± 0.06 and vary little with observing band. Without colour cuts, the LFs are much noisier but not significantly steeper. The faint end slopes show a statistically significant steepening from α = −1.4 ± 0.1 in the central region (extending to half a virial radius) to −1.8 ± 0.1 in the Southern envelope of the cluster. Cosmic variance and uncertain star-galaxy separation are our main limiting factors in measuring the faint end of the LFs. The large-scale environment of Abell 496, probed with the fairly complete 6dFGS catalogue, shows a statistically significant 36 Mpc long filament at PA = 137• . Conclusions. Our LFs do not display the large number of dwarf galaxies (α ≈ −2) inferred by several authors, whose analyses may suffer from field contamination caused by non-existent or inadequate colour cuts. Alternatively, different clusters may have different faint end slopes, but this is hard to reconcile with the wide range of slopes found for given clusters and for wide sets of clusters.

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Section: Comparison With Previous Analyses Of Abell 496contrasting

confidence: 95%

“…This problem has already been highlighted (e.g. Oemler 1974;Durret et al 2002). We improve our analysis by removing those objects whose colour imply that they are background objects.…”

Section: Improvement Using Colour Magnitude Relationsmentioning

confidence: 99%

The galaxy luminosity function of the Abell 496 cluster and its spatial variations

Boué¹,

Adami²,

Durret

et al. 2007

A&A

Self Cite

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“…Moreover, we observed that the cluster to cluster variations of the LF found in the literature are due to choice of a fixed metric apertures for all the systems. This is due to the fact that fraction of dwarf galaxies in clusters is an increasing function of the clustercentric distance (see also Durret et al 2002). To keep under control also the possible dependence between the shape of the LF and the cluster mass, we divided our cluster sample (with mass ranges from the statistics and study the average luminosity distribution of the galaxies in each mass bin, we have used the SDSS photometric data to compute a composite luminosity function (LF) by stacking the individual cluster LFs calculated within r 200 .…”

Section: Luminosity Function Shape and Cluster Massmentioning

confidence: 99%

RASS-SDSS galaxy cluster survey

Popesso¹,

Biviano

Böhringer

et al. 2006

A&A

135

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Aims. We explore the mass-to-light ratio in galaxy clusters and its relation to the cluster mass. Methods. We study the relations among the optical luminosity (L op ), the cluster mass (M 200 ) and the number of cluster galaxies within r 200 (N gal ) in a sample of 217 galaxy clusters with confirmed 3D overdensity. We correct for projection effect, by determining the galaxy surface number density profile in our cluster sample. This is best fitted by a cored King profile in low and intermediate mass systems. The core radius decreases with cluster mass, and, for the highest mass clusters, the profile is better represented by a generalized King profile or a cuspy Navarro, Frenk & White profile. Results. We find a very tight proportionality between L op and N gal , which, in turn, links the cluster mass-to-light ratio to the Halo Occupation Distribution N gal vs. M 200 . After correcting for projection effects, the slope of the L op −M 200 and N gal −M 200 relations is found to be 0.92 ± 0.03, close, but still significantly less than unity. We show that the non-linearity of these relations cannot be explained by variations of the galaxy luminosity distributions and of the galaxy M/L with the cluster mass. Conclusions. We suggest that the nonlinear relation between number of galaxies and cluster mass reflects an underlying nonlinear relation between number of subhaloes and halo mass.

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“…In particular, ground-based wide-field instruments like CFHT-12K, AAT-WFI, MPG/ESO-WFI, and INT-WFC are providing large databases for morphological and evolutionary studies of galaxies at low and intermediate redshifts (McMahon et al 2001;Andreon & Cuillandre 2002;Durret et al 2002;Pracy et al 2003;Fasano et al 2003;Hudson et al 2003;Pimbblet & Drinkwater 2004), while highresolution, very deep HST(WFPC2/ACS) observations of distant galaxies are giving us a glimpse at their early evolutionary phases (Blakeslee et al 2004;Ravindranath et al 2004;Thompson 2004;Rix et al 2004;Cimatti et al 2004;Cassata et al 2005). This kind of data is invaluable for the huge information it contains.…”

Section: Introductionmentioning

confidence: 99%

GASPHOT: a tool for Galaxy Automatic Surface PHOTometry

Pignatelli¹,

Fasano²,

Cassata

2006

A&A

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In this paper we present a new tool for automatic, blind surface photometry of galaxies in deep and/or wide fields. The tool (GASPHOT) favors the robustness of results with respect to the details of galaxy modeling. To this aim, a single Sersic-law for the models and a hybrid 1D/2D approach for the best-fitting algorithm were adopted. GASPHOT is heavily based on SExtractor and provides luminosity, position angle and ellipticity profiles of galaxies extracted from CCD frames, as well as total magnitudes, half-light radii, and Sersic indices. These global parameters were obtained by simultaneously fitting the major and minor axis light growth curves of galaxies with a 2D flattened Sersiclaw, convolved by the appropriate, space-varying PSF, which was previously evaluated by the tool itself. We tested GASPHOT on more than 15 000 simulated and real galaxies, obtaining robust upper limits for the errors of the global parameters of galaxies, even for non-Sersic profiles and blended objects. The GASPHOT performance was also compared with those of two popular alternative tools for a single component, Sersic law: GALFIT (Peng et al. 2002) and GIM2D (Marleau &Simard 1998). When dealing with ideal, isolated, and adeguately large galaxies, the three packages were all found to provide satisfactory results, apart from a definite bias in the GIM2D magnitudes. On the other hand, GASPHOT proved to be more robust than GALFIT and GIM2D for simulated, blended objects and for real galaxies. Moreover, at variance with GASPHOT and GALFIT, the quality (bias and scatter) of the fits provided by GIM2D rapidly declines as the galaxy size decreases.

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Environmental effects on the galaxy luminosity function in the cluster of galaxies Abell 496

Cited by 19 publications

References 24 publications

The galaxy luminosity function of the Abell 496 cluster and its spatial variations

The galaxy luminosity function of the Abell 496 cluster and its spatial variations

RASS-SDSS galaxy cluster survey

GASPHOT: a tool for Galaxy Automatic Surface PHOTometry

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