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

Trèvese, D.; Castellano, M.; Fontana, A.; Giallongo, E.

doi:10.1051/0004-6361:20065384

Cited by 32 publications

(68 citation statements)

References 45 publications

(97 reference statements)

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“…Scoville et al (2007), Mazure et al (2007), Eisenhardt et al (2008), andvan Breukelen et al (2006) have estimated the surface density in redshift slices, each with different methods: the first two use adaptive smoothing of galaxy counts, Eisenhardt et al (2008) analyse a density map convolved with a wavelet kernel, while the last author adopts FoF and Voronoi tessellation (Marinoni et al 2002). At variance with these, we preferred to adopt an adaptive 3D density estimate to consider, automatically, distances in all directions and the relevant positional accuracies at the same time.…”

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%

“…The algorithm is described in detail in Trevese et al (2007). Here we outline its main features and, in the next section, we present the simulations used to estimate its reliability.…”

Section: The (2+1)d Algorithm For the Density Estimationmentioning

confidence: 99%

“…While this is a rather simplistic representation of a survey, it allows us to evaluate some basic features of our algorithm, without the use of N-body simulations. We expanded the previous simulations presented in Trevese et al (2007), using a larger number of mock catalogues and adopting a more consistent treatment of the survey completeness. For each redshift, we calculated the limiting absolute B magnitude for the two populations of "red" and "blue" galaxies, defined from the minima in the U − V vs. B distribution in Salimbeni et al (2008), using the average type−dependent K− and evolutionary corrections calculated from the best-fit SED of the objects in the real catalogue.…”

Section: Simulationsmentioning

confidence: 99%

“…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). This method combines galaxy angular positions and precise photometric redshifts to estimate the galaxy number density and to detect galaxy over-densities in three dimensions also at z > 1, as described in Sect.…”

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%

“…The algorithm is described in detail in Trevese et al (2007). Here we outline its main features and, in the next section, we present the simulations used to estimate its reliability.…”

Section: The (2+1)d Algorithm For the Density Estimationmentioning

confidence: 99%

Section: Simulationsmentioning

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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The Large-scale Structure in the Chandra Deep Field South

et al. 2010

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Abstract. We have studied the large scale distribution of matter in the Chandra Deep Field South on the basis of photometric redshifts and we have identified several over-densities between redshift 0.6 and 2.3. We analyse two of these structures using the deepest X-ray observations ever obtained: 4 Ms with the Chandra satellite and 2.5 Ms with XMM-Newton. We set a very faint upper limit on the X-ray luminosity of a structure at redshift 1.6, and we find an extended X-ray emission from a structure at redshift 0.96 of which we can estimate the gas temperature and make a comparison with the scaling relations between the X-ray luminosity and mass or temperature of high redshift galaxy clusters.

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GMASS ultradeep spectroscopy of galaxies at z ~ 2

Kurk

Cimatti

Zamorani

et al. 2009

A&A

108

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Context. Clusters of galaxies represent important laboratories for studying galaxy evolution and formation. Well established and relaxed clusters are known below z < 1.4, as well as, clusters in formation found close to radio galaxies at z > 2, but the in-between redshift range, during which clusters are expected to undergo significant changes, is almost unexplored. Aims. By studying a galaxy overdensity in redshift and angular distribution at z = 1.6, uncovered in the Galaxy Mass Assembly ultra-deep Spectroscopic Survey (GMASS), we provide insight into the evolution of cluster galaxies at high redshift. Methods. We present a study of the significance of the galaxy overdensity at z = 1.6, Cl 0332-2742, its velocity dispersion, and X-ray emission. We identify the colour bimodality of the cluster members and compare the properties of members of Cl 0332-2742 with galaxies outside the overdensity. Results. From the redshifts of the 42 overdensity members, we measure a velocity dispersion of 500 km s −1 . We conservatively estimate the overdensity in redshift space for the spike at z = 1.6 in the GMASS field to be 8.3 ± 1.5. A map of the surface density of galaxies at z = 1.6 in the GMASS field shows that its structure is irregular with several filaments and local overdensities. The differences in the physical properties of Cl 0332-2742 member and field galaxies agree with the latest hierarchical galaxy formation models: for overdensity members, the star formation rate (SFR), and specific SFR, is approximately 50% lower than for the field galaxies; overdensity galaxies are twice the age, on average, of field galaxies; and there is a higher proportion of both massive (M > 10 10.7 M ), and early-type galaxies, inside Cl 0332-2742 than in the field. Among the 42 members, seven have spectra consistent with being passively evolving, massive galaxies. These are all located within an area where the surface density of z = 1.6 galaxies is highest. In a z − J colour-magnitude diagram, the photometric data of these early-type galaxies are in close agreement with a theoretical red sequence of a galaxy cluster at redshift z = 1.6, which formed most of its stars in a short burst of star formation at z ∼ 3. Conclusions. We conclude that the redshift spike at z = 1.6 in the GMASS field represents a sheet-like structure in the cosmic web, and that the area with the highest surface density within this structure, containing already seven passively evolving galaxies, will evolve into a cluster of galaxies at a later time.

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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

Cited by 32 publications

References 45 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 Large-scale Structure in the Chandra Deep Field South

GMASS ultradeep spectroscopy of galaxies at z ~ 2

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