Advanced Camera for Surveys Photometry of the Cluster RDCS 1252.9-2927: The Color-Magnitude Relation at
                    <i>z</i>
                    = 1.24

Aims. The aim of the present paper is to identify and study the properties and galactic content of groups and clusters in the GOODSSouth field up to z ∼ 2.5, and to analyse the physical properties of galaxies as a continuous function of environmental density up to high redshift. Methods. We used the deep (z 850 ∼ 26), multi-wavelength GOODS-MUSIC catalogue, which has a 15% of spectroscopic redshifts and accurate photometric redshifts for the remaining fraction. On these data, we applied a (2+1)D algorithm, previously developed by our group, that provides an adaptive estimate of the 3D density field. We supported our analysis with simulations to evaluate the purity and the completeness of the cluster catalogue produced by our algorithm. Results. We find several high-density peaks embedded in larger structures in the redshift range 0.4-2.5. From the analysis of their physical properties (mass profile, M 200 , σ v , L X , U − B vs. B diagram), we find that most of them are groups of galaxies, while two are poor clusters with masses a few times 10 14 M . For these two clusters we find from the Chandra 2Ms data an X-ray emission significantly lower than expected from their optical properties, suggesting that the two clusters are either not virialised or are gas poor. We find that the slope of the colour magnitude relation, for these groups and clusters, is constant at least up to z ∼ 1. We also analyse the dependence on environment of galaxy colours, luminosities, stellar masses, ages, and star formations. We find that galaxies in high-density regions are, on average, more luminous and massive than field galaxies up to z ∼ 2. The fraction of red galaxies increases with luminosity and with density up to z ∼ 1.2. At higher z this dependence on density disappears. The variation of galaxy properties as a function of redshift and density suggests that a significant change occurs at z ∼ 1.5-2.

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“…Blakeslee et al 2003;Homeier et al 2006;Trevese et al 2007). We confirm that the observations indicate no evolution up to redshift ∼1.…”

Section: Colour-magnitude Diagramssupporting

confidence: 86%

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Salimbeni

Castellano

Pentericci

et al. 2009

A&A

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“…Earlier studies concentrated on nearby galaxies, but with the recent advent of large telescopes, environment studies at z ∼ 1 became possible. Interestingly, the environmental dependence of galaxy properties observed at z ∼ 1 is already strong; clusters at z ∼ 1 are dominated by red earlytype galaxies (e.g., Blakeslee et al 2003;Nakata et al 2005;Postman et al 2005;Lidman et al 2008;Mei et al 2009, but see also Cucciati et al 2006). Also, the formation epoch of cluster galaxies measured at z ∼ 1 is consistent with that observed locally (Gobat et al 2008) .…”

Section: Introductionsupporting

confidence: 67%

The environmental dependence of galaxy properties atz = 2

Tanaka¹,

Breuck²,

Venemans³

et al. 2010

A&A

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We report on the environmental dependence of galaxy properties at z = 2.15. We construct multi-band photometric data sets in the (proto-)cluster PKS1138-26 field and in the GOODS field. We then fit spectral energy distributions of the galaxies with model templates generated with the latest stellar population synthesis code and derive physical properties of galaxies from the fits. To quantify the environmental dependence of galaxy properties, a special care is taken of systematic errors -we use data sets that have almost the same wavelength samplings, use the same code to fit SEDs with the same set of templates, and compare relative differences between the two samples. We find that the PKS1138 galaxies have similar ages, shorter star formation time scales, lower star formation rates, and weaker dust extinction compared to the GOODS galaxies at z ∼ 2. This trend is similar to that observed locally, suggesting that the environmental dependence of galaxy properties is already partly in place as early as z = 2.15. We show that the PKS1138 galaxies assemble the bulk of their masses ∼1 Gyr earlier than field galaxies, i.e., the galaxy formation depends on environment. Galaxy mergers should frequently occur during the first collapse of clusters and they might play an important role in driving the observed environmental dependence of galaxy properties at z = 2.15.

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“…Our analysis supports the evidence of a constant C-M slope up to z = 1, meaning a correspondingly constant mass-metallicity relation. We stress that most of the highest redshift clusters detected so far were selected in the X-ray band, in particular those at z = 1.24 (Blakeslee et al 2003;Rosati et al 2004) and z = 1.4 (Mullis et al 2005). However, both these clusters have a velocity dispersion of about 800 km s −1 and intracluster gas temperature kT ∼ 6 keV, typical of rich clusters (Bahcall 1988;Arnaud et al 2005).…”

Section: Discussionmentioning

confidence: 85%

“…Our results show that the slope of the red sequence is consistent with being the same in local clusters and in the two main overdensities (z ∼ 0.7 and z ∼ 1.0). Blakeslee et al (2003) found little or no evidence of evolution of this slope, out to z = 1.2. Our results (Fig.…”

Section: Cosmological Evolution Of the Red Sequencementioning

confidence: 81%

“…Following Bell et al (2004) we assume a constant slope ∂(U − V) rest /∂M V rest = −0.08 which is derived from a sample of nearby clusters (Bower et al 1992). This assumption is justified by the analysis of Blakeslee et al (2003) who find a constant slope for different galaxy clusters up to z = 1.2 (see the next paragraph). At higher redshifts Giallongo et al (2005) find a decrease of the red sequence slope ∂(U −V) rest /∂M B rest from −0.098 to −0.062, in the two wide redshift bins 0.4-1 and 1.3-3.5 respectively.…”

Section: Cosmological Evolution Of the Red Sequencementioning

confidence: 93%

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A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

Trèvese

Castellano

Fontana

et al. 2006

A&A

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Aims. We study galaxy clustering and explore the dependence of galaxy properties on the the environment up to a redshift z ∼ 1, on the basis of a deep multi-band survey in the Chandra Deep Field South. Methods. We have developed a new method which combines galaxy angular positions and photometric redshifts to estimate the local galaxy number-density. This allows both the detection of overdensities in the galaxy distribution and the study of the properties of the galaxy population as a function of the environmental density. Results. We detect two moderate overdensities at z ∼ 0.7 and z ∼ 1 previously identified spectroscopically. We find that the fraction of red galaxies within each structure increases with volume density, extending to z ∼ 1 previous results. We measure "red sequence" slopes consistent with the values found in X-ray selected clusters, supporting the notion that the mass-metallicity relation hold constant up to z ∼ 1. Conclusions. Our method based on photometric redshifts allows to extend structure detection and density estimates up to the limits of photometric surveys, i.e. considerably deeper than spectroscopic surveys. Since X-ray cluster detection at high redshift is presently limited to massive relaxed structures, galaxy volume density based on photometric redshift appears as a valuable tool in the study of galaxy evolution.

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Advanced Camera for Surveys Photometry of the Cluster RDCS 1252.9-2927: The Color-Magnitude Relation at z = 1.24

Cited by 214 publications

References 22 publications

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

The environmental dependence of galaxy properties atz = 2

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

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