Galaxy colours in high-redshift, X-ray-selected clusters - I. Blue galaxy fractions in eight clusters

Fairley, B. W.; Jones, L. R.; Wake, David A.; Collins, Chris; Burke, Douglas; Nichol, R. C.; Romer, A. K.

doi:10.1046/j.1365-8711.2002.05121.x

Cited by 51 publications

(74 citation statements)

References 66 publications

(148 reference statements)

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“…These results support the general view that blue galaxies dominate the galaxy population in the outskirts of clusters in contrast to the central cluster region (e.g., Ellingson et al 2001;Fairley et al 2002;Dahlén et al 2004;Tran et al 2005). They also imply that field galaxies, which are generally bluer than cluster galaxies (see, for example, Lewis et al 2002;McIntosh et al 2004), fall into the cluster environment, turn red (possibly via some process that truncates star formation), and that blue dwarf galaxies get preferentially disrupted or transformed into red dwarfs at small clustercentric radii.…”

Section: Discussionsupporting

confidence: 88%

“…Transforming the magnitude limit utilized by Aguerri et al to our filter and distance scale (M R c ∼ −21), we find an 80% probability of a correlation. Our results are in agreement with Fairley et al (2002) and Wake et al (2005), who found no significant correlation between f b and L X .…”

Section: Blue Galaxy Fractionsupporting

confidence: 93%

“…As a caveat we note that our results based on Figures 4 and 5 demonstrate that the counting aperture and magnitude range has a direct impact on the value of f b , and thus one must be cautious when comparing blue fractions for clusters with disparate masses from a variety of sources (see also, Ellingson et al 2001;Fairley et al 2002;De Propris et al 2004;Popesso et al 2007). …”

Section: Radial and Magnitude Dependence Of F Bmentioning

confidence: 84%

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The Galaxy Population of Low-Redshift Abell Clusters

Barkhouse

Yee

López-Cruz

2009

ApJ

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We present a study of the luminosity and color properties of galaxies selected from a sample of 57 low-redshift Abell clusters. We utilize the non-parametric dwarf-to-giant ratio (DGR) and the blue galaxy fraction (f b ) to investigate the clustercentric radial-dependent changes in the cluster galaxy population. Composite cluster samples are combined by scaling the counting radius by r 200 to minimize radius selection bias. The separation of galaxies into a red and blue population was achieved by selecting galaxies relative to the cluster color-magnitude relation. The DGR of the red and blue galaxies is found to be independent of cluster richness (B gc ), although the DGR is larger for the blue population at all measured radii. A decrease in the DGR for the red and red+blue galaxies is detected in the cluster core region, while the blue galaxy DGR is nearly independent of radius. The f b is found not to correlate with B gc ; however, a steady decline toward the inner-cluster region is observed for the giant galaxies. The dwarf galaxy f b is approximately constant with clustercentric radius except for the innercluster core region where f b decreases. The clustercentric radial dependence of the DGR and the galaxy blue fraction indicates that it is unlikely that a simple scenario based on either pure disruption or pure fading/reddening can describe the evolution of infalling dwarf galaxies; both outcomes are produced by the cluster environment.

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Section: Discussionsupporting

confidence: 88%

Section: Blue Galaxy Fractionsupporting

confidence: 93%

Section: Radial and Magnitude Dependence Of F Bmentioning

confidence: 84%

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The Galaxy Population of Low-Redshift Abell Clusters

Barkhouse

Yee

López-Cruz

2009

ApJ

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“…3.3.1) is a consequence of our choice to define red and blue galaxies (see Fairley et al 2002 for an opposite result when using the red-sequence to split red and blue galaxies).…”

Section: Blue/red Definitionmentioning

confidence: 99%

Galaxy mass, cluster-centric distance and secular evolution: their role in the evolution of galaxies in clusters in the last 10 Gyr

Raichoor

Andreon

2012

A&A

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Context. Galaxy mass and environment are known to play a key role in galaxy evolution: studying galaxy colors as a function of redshift, galaxy mass, and environment offers a powerful diagnosis to disentangle the role of each. Aims. We study the simultaneous dependence of the fraction of blue galaxies f blue on secular evolution, environment, and galaxy mass with a well-controlled cluster sample. We are thus able to study the evolution and respective role of the cessation of star formation history (SFH) in clusters caused by galaxy mass ("mass quenching") or by environment ("environmental quenching"). Methods. We defined an homogenous X-ray selected cluster sample (25 clusters with 0 < z < 1 and one cluster at z ∼ 2.2), having similar masses and well-defined sizes. Using multicolor photometry and a large spectroscopic sample to calibrate photometric redshifts, we carefully estimated f blue for each cluster at different galaxy mass and cluster-centric distance bins. We then fitted the dependence of f blue on redshift (z), environment (r/r 200 ) and galaxy mass (M) with a simple model. Results. f blue increases with cluster-centric distance with a slope α = 1.2 +0.4 −0.3 , decreases with galaxy mass with a slope β = −3.8 +0.6 −0.5 , and increases with redshift with a slope γ = 3.3 +0.7 −0.6 . The data also require for the first time a differential evolution with galaxy mass of f blue with redshift, with lower mass galaxies evolving slower by a factor ζ = −3.9 +0.9 −1.1 . Conclusions. Our study shows that the processes responsible for the cessation of star formation in clusters are effective at all epochs (z < ∼ 2.2), and more effective in denser environments and for more massive galaxies. We found that the mass and environmental quenchings are separable, that environmental quenching does not change with epoch, and that mass quenching is a dynamical process, i.e. its evolutionary rate is mass-dependent. Our study extends the downsizing-like scenario, where the most massive galaxies have their properties set at a very high redshift, to the cluster environment and all galaxies. It illustrates the need to disentangle galaxy mass and cluster-centric distance to properly estimate the behavior of f blue in clusters.

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“…However, observations of the near-infrared luminosity function show that any change with environment is likely to be small [68,69,70]. On the other hand, the strong redshift evolution observed in the colors of galaxies in both clusters [71,72,73] and the field [74,75] suggests that some galaxies transform from one population to another. In particular, Bell et al [18] noted a build up of stellar mass on the red sequence by a factor of about two between z ∼ 1 and 0, averaged over all environments.…”

Section: Transformation Modelingmentioning

confidence: 99%

Color bimodality: Implications for galaxy evolution

Baldry¹

2004

AIP Conference Proceedings

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Abstract. We use a sample of 69726 galaxies from the SDSS to study the variation of the bimodal color-magnitude (CM) distribution with environment. Dividing the galaxy population by environment (Σ 5 ) and luminosity (−23 < M r < −17), the u − r color functions are modeled using double-Gaussian functions. This enables a deconvolution of the CM distributions into two populations: red and blue sequences. The changes with increasing environmental density can be separated into two effects: a large increase in the fraction of galaxies in the red distribution, and a small color shift in the CM relations of each distribution. The average color shifts are 0.05 ± 0.01 and 0.11 ± 0.02 for the red and blue distributions, respectively, over a factor of 100 in projected neighbor density. The red fraction varies between about 0% and 70% for low-luminosity galaxies and between about 50% and 90% for high-luminosity galaxies. This difference is also shown by the variation of the luminosity functions with environment. We demonstrate that the effects of environment and luminosity can be unified. A combined quantity,, predicts the fraction of red galaxies, which may be related to the probability of transformation events. Our results are consistent with major interactions (mergers and/or harassment) causing galaxies to transform from the blue to the red distribution. We discuss this and other implications for galaxy evolution from earlier results and model the effect of slow transformations on the color functions. 1

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Galaxy colours in high-redshift, X-ray-selected clusters - I. Blue galaxy fractions in eight clusters

Cited by 51 publications

References 66 publications

The Galaxy Population of Low-Redshift Abell Clusters

The Galaxy Population of Low-Redshift Abell Clusters

Galaxy mass, cluster-centric distance and secular evolution: their role in the evolution of galaxies in clusters in the last 10 Gyr

Color bimodality: Implications for galaxy evolution

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