Distant galaxy clusters in the COSMOS field found by HIROCS

Zatloukal, M.; Röser, H.-J.; Wolf, Christian; Hippelein, H.; Falter, S.

doi:10.1051/0004-6361:20078063

Cited by 17 publications

(26 citation statements)

References 17 publications

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“…However, a more detailed comparison is beyond the scope of the present work, since it would require extensive simulations and/or the application of the different methods to the same datasets. A similar three-dimensional approach has been proposed by Zatloukal et al (2007). They select cluster candidates detecting excess density in the 3D galaxy distribution reconstructed from the photometric redshift probability distributions p(z) of each object.…”

Section: Comparison With Other Methods Based On Photometric Redshiftsmentioning

confidence: 99%

“…Mazure et al (2007), while Scoville et al (2007), van Breukelen et al (2006), Zatloukal et al (2007), and Eisenhardt et al (2008) consider the full probability distribution function (PDF) to take redshift uncertainties into account. As discussed by Scoville et al (2007), this last method could tend to detect structures formed by early type galaxies, since they have smaller photometric redshift uncertainty, thanks to their stronger Balmer break, when this feature is well-sampled in the observed bands.…”

Section: Comparison With Other Methods Based On Photometric Redshiftsmentioning

confidence: 99%

“…In the past few years, several authors (e.g. Botzler et al 2004;van Breukelen et al 2006;Scoville et al 2007;Zatloukal et al 2007;Mazure et al 2007;Eisenhardt et al 2008) have developed or extended known algorithms to take the greater redshift uncertainties into account. We have developed a new algorithm that uses an adaptive estimate of the 3D density field, as described in detail in Trevese et al (2007).…”

Section: Introductionmentioning

confidence: 99%

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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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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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Section: Comparison With Other Methods Based On Photometric Redshiftsmentioning

confidence: 99%

Section: Comparison With Other Methods Based On Photometric Redshiftsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…This will then allow a detailed discussion of the results. Derivation of the selection function for the 5-filter HIROCS data sets will follow the lines described by Zatloukal et al (2009), who derived the selection function for the cluster search in the COSMOS field based on the analysis of 10 filters (Zatloukal et al 2007). …”

Section: Introductionmentioning

confidence: 99%

“…As part of HIROCS, we have supplemented the public COSMOS data with H-band observations at Calar Alto and isolated 11 clusters with z > 1 (Zatloukal et al 2007). …”

Section: Introductionmentioning

confidence: 99%

The Heidelberg InfraRed Optical Cluster Survey (HIROCS)

Röser¹,

Hippelein²,

Wolf

et al. 2010

A&A

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Aims. We describe a survey for distant clusters of galaxies that identified clusters as local overdensities in the 3D galaxy distribution. Methods. Optical and near-IR imaging in B, R, i, z, and H are used to derive photometric redshifts for objects as faint as m* + 1 at a redshift of 1.5. We outline the astrometric and photometric data reduction. The 3D cluster search, based on the photometric redshifts, is described. Results. On the basis of the first fully reduced 1 square degree of data, we demonstrate that the objectives of HIROCS have been achieved. Four representative clusters from the list of candidates are presented.

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