Extending the Butcher-Oemler effect up to<i>z</i>∼ 0.7

Andreon, S.; Lobo, C.; Iovino, A.

doi:10.1111/j.1365-2966.2004.07554.x

Cited by 42 publications

(59 citation statements)

References 57 publications

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“…It may be related to environmental effects (e.g. Dressler et al 1997), but has also been proposed to be consistent with the overall ageing of all galaxies, irrespective of their environment (Andreon et al 2004a(Andreon et al , 2006. According to our criteria, a galaxy is "blue" if it has a colour U − B ≤ 1.…”

Section: The U -B Colour Of Group Galaxiesmentioning

confidence: 86%

The VIMOS-VLT deep survey: the group catalogue

Cucciati

Marinoni

Iovino³

et al. 2010

A&A

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Aims. We present a homogeneous and complete catalogue of optical galaxy groups identified in the purely flux-limited (17.5 ≤ I AB ≤ 24.0) VIMOS-VLT deep redshift Survey (VVDS). Methods. We use mock catalogues extracted from the Millennium Simulation, to correct for potential systematics that might affect the overall distribution as well as the individual properties of the identified systems. Simulated samples allow us to forecast the number and properties of groups that can be potentially found in a survey with VVDS-like selection functions. We use them to correct for the expected incompleteness and, to asses in addition, how well galaxy redshifts trace the line-of-sight velocity dispersion of the underlying mass overdensity. In particular, on these mock catalogues we train the adopted group-finding technique i.e., the Voronoi-Delaunay Method (VDM). The goal is to fine-tune its free parameters, recover in a robust and unbiased way the redshift and velocity dispersion distributions of groups (n(z) and n(σ), respectively), and maximize, at the same time, the level of completeness and purity of the group catalogue. Results. We identify 318 VVDS groups with at least 2 members in the range 0.2 ≤ z ≤ 1.0, among which 144 (/30) with at least 3 (/5) members. The sample has an overall completeness of ∼60% and a purity of ∼50%. Nearly 45% of the groups with at least 3 members are still recovered if we run the algorithm with a particular parameter set that maximizes the purity (∼75%) of the resulting catalogue. We use the group sample to explore the redshift evolution of the fraction f b of blue galaxies (U − B ≤ 1) in the redshift range 0.2 ≤ z ≤ 1. We find that the fraction of blue galaxies is significantly lower in groups than in the global population (i.e. in the whole ensemble of galaxies irrespective of their environment). Both of these quantities increase with redshift, the fraction of blue galaxies in groups exhibiting a marginally significant steeper increase. We also investigate the dependence of f b on group richness: not only we confirm that, at any redshift, the blue fraction decreases in systems with increasing richness, but we find that this result continues to hold towards fainter luminosities.

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Section: The U -B Colour Of Group Galaxiesmentioning

confidence: 86%

The VIMOS-VLT deep survey: the group catalogue

Cucciati

Marinoni

Iovino³

et al. 2010

A&A

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“…We define a galaxy as blue if it is bluer than a CB07 model with τ = 3.7 Gyr, as in Andreon et al (2004Andreon et al ( , 2006Andreon et al ( , 2008, Loh et al (2008), and Raichoor & Andreon (2012). This galaxy will be bluer by 0.2 mag in B − V than red-sequence galaxies at z = 0 (which would be a blue galaxy by the original definition of Butcher & Oemler 1984).…”

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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“…(Dressler & Gunn 1982, 1992Lavery & Henry 1986, 1988Fabricant et al 1991;Poggianti et al 1999Poggianti et al , 2006Ellingson et al 2001), has been extended to groups (Allington-Smith et al 1993;Wilman et al 2005a;Gerke et al 2007;Cucciati et al 2009b), and critically discussed in the context of selection biases (Andreon & Ettori 1999;Andreon et al 2004Andreon et al , 2006.…”

Section: Introductionmentioning

confidence: 99%

The zCOSMOS redshift survey: how group environment alters global downsizing trends

Iovino¹,

Cucciati

Scodeggio

et al. 2009

A&A

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Context. Groups of galaxies are a common environment, bridging the gap between starforming field galaxies and quiescent cluster galaxies. Within groups secular processes could be at play, contributing to the observed strong decrease of star formation with cosmic time in the global galaxy population. Aims. We took advantage of the wealth of information provided by the first ∼10 000 galaxies of the zCOSMOS-bright survey and its group catalogue to study in detail the complex interplay between group environment and galaxy properties. Methods. The classical indicator F blue , i.e., the fraction of blue galaxies, proved to be a simple but powerful diagnostic tool. We studied its variation for different luminosity and mass selected galaxy samples, divided as to define groups/field/isolated galaxy subsamples. Results. Using rest-frame evolving B-band volume-limited samples, the groups galaxy population exhibits significant blueing as redshift increases, but maintains a systematic difference (a lower F blue ) with respect to the global galaxy population, and an even larger difference with respect to the isolated galaxy population. However moving to mass selected samples it becomes apparent that such differences are largely due to the biased view imposed by the B-band luminosity selection, being driven by the population of lower mass, bright blue galaxies for which we miss the redder, equally low mass, counterparts. By carefully focusing the analysis on narrow mass bins such that mass segregation becomes negligible we find that only for the lowest mass bin explored, i.e., log(M * /M ) ≤ 10.6, does a significant residual difference in color remain as a function of environment, while this difference becomes negligible toward higher masses. Conclusions. Our results indicate that red galaxies of mass log(M * /M ) ≥ 10.8 are already in place at z ∼ 1 and do not exhibit any strong environmental dependence, possibly originating from so-called nature or internal mechanisms. In contrast, for lower galaxy masses and redshifts lower than z ∼ 1, we observe the emergence in groups of a population of nurture red galaxies: slightly deviating from the trend of the downsizing scenario followed by the global galaxy population, and more so with cosmic time. These galaxies exhibit signatures of group-related secular physical mechanisms directly influencing galaxy evolution. Our analysis implies that these mechanisms begin to significantly influence galaxy evolution after z ∼ 1, a redshift corresponding to the emergence of structures in which these mechanisms take place.

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Extending the Butcher-Oemler effect up toz∼ 0.7

Cited by 42 publications

References 57 publications

The VIMOS-VLT deep survey: the group catalogue

The VIMOS-VLT deep survey: the group catalogue

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

The zCOSMOS redshift survey: how group environment alters global downsizing trends

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