EDisCS – the ESO distant cluster survey

White, Simon D. M.; Clowe, Douglas; Simard, Luc; Rudnick, Gregory; Lucia, G. De; Aragón-Salamanca, Alfonso; Bender, Ralf; Best, P. N.; Bremer, M. N.; Charlot, S.; Dalcanton, Julianne J.; Dantel, M.; Desai, Vandana; Fort, B.; Halliday, C.; Jablonka, P.; Kauffmann, Guinevere; Mellier, Y.; Milvang-Jensen, B.; Pelló, R.; Poggianti, Bianca M.; Poirier, Sylvie; Röttgering, H. J. A.; Saglia, R. P.; Schneider, Peter; Zaritsky, Dennis

doi:10.1051/0004-6361:20042068

Cited by 130 publications

(219 citation statements)

References 64 publications

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“…A similar comparison (Kriek et al 2008), based however on real spectroscopic and J − K measurements, displays Δz ∼ 0.08 systematic errors. At much lower redshift EDiSCs clusters have photo-z systematics of Δz ∼ 0.1 (White et al 2005), similar to RCS clusters prior to photometric redshift recalibration (Gilbank et al 2007). …”

Section: Cluster Redshiftmentioning

confidence: 80%

JKCS 041: a colour-detected galaxy cluster at $z_{\mathrm{phot}}$ ~ 1.9 with deep potential well as confirmed by X-ray data

Andreon¹,

Maughan

Trinchieri³

et al. 2009

A&A

121

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We report the discovery of JKCS 041, a massive near-infrared selected cluster of galaxies at z phot ∼ 1.9. The cluster was originally discovered using a modified red-sequence method and also detected in follow-up Chandra data as an extended X-ray source. Optical and near-infrared imaging data alone allow us to show that the detection of JKCS 041 is secure, even in the absence of the X-ray data. We investigate the possibility that JKCS 041 is not a galaxy cluster at z ∼ 1.9, and find other explanations unlikely. The X-ray detection and statistical arguments rule out the hypothesis that JKCS 041 is actually a blend of groups along the line of sight, and we find that the X-ray emitting gas is too hot and dense to be a filament projected along the line of sight. The absence of a central radio source and the extent and morphology of the X-ray emission argue against the possibility that the X-ray emission comes from inverse Compton scattering of CMB photons by a radio plasma. The cluster has an X-ray core radius of 36.6 +8.3 −7.6 arcsec (about 300 kpc), an X-ray temperature of 7.4 +5.3 −3.3 keV, a bolometric X-ray luminosity within R 500 of (7.6 ± 0.5) × 10 44 erg s −1 , and an estimated mass of M 500 = 2.9 +3.8 −2.4 × 10 14 M , the last derived under the usual (and strong) assumptions. The cluster is composed of 16.4 ± 6.3 galaxies within 1.5 arcmin (750 kpc) brighter than K ∼ 20.7 mag. The high redshift of JKCS 041 is determined from the detection colour, from the detection of the cluster in a galaxy sample formed by z phot > 1.6 galaxies and from a photometric redshift based on 11-band spectral energy distribution fitting. By means of the latter we find the cluster redshift to be 1.84 < z < 2.12 at 68% confidence. Therefore, JKCS 041 is a cluster of galaxies at z phot ∼ 1.9 with a deep potential well, making it the most distant cluster with extended X-ray emission known.

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Section: Cluster Redshiftmentioning

confidence: 80%

JKCS 041: a colour-detected galaxy cluster at $z_{\mathrm{phot}}$ ~ 1.9 with deep potential well as confirmed by X-ray data

Andreon¹,

Maughan

Trinchieri³

et al. 2009

A&A

121

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“…The EDisCS multiwavelength photometric and spectroscopic survey of galaxies (White et al 2005) was developed to characterise both the clusters themselves and the galaxies within them. It observed 20 fields containing galaxy clusters at 0.4 < z < 1.…”

Section: Ediscsmentioning

confidence: 99%

The galaxy stellar mass function and its evolution with time show no dependence on global environment

Vulcani

Poggianti

Oemler

et al. 2013

A&A

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We present an analysis of the galaxy stellar mass function in different environments at intermediate redshift (0.3 ≤ z ≤ 0.8) for two mass-limited galaxy samples. We use the IMACS Cluster Building Survey (ICBS; M * ≥ 10 10.5 M ) to study cluster, group and field galaxies at z = 0.3-0.45, and the ESO Distant Cluster Survey (EDisCS; M * ≥ 10 10.2 M ) to investigate cluster and group galaxies at z = 0.4-0.8. Our analysis thus includes galaxies with masses reaching just below that of the Milky Way. Excluding the brightest cluster galaxies, we show that the shape of the mass distribution does not seem to depend on global environment, Our two main results are: (1) Galaxies in the virialised regions of clusters, in groups, and in the field follow similar mass distributions. (2) Comparing the ICBS and EDisCS mass functions to mass functions in the local universe, we detect evolution from z ∼ 0.4-0.6 to z ∼ 0.07 in the sense that the population of low-mass galaxies has grown with time with respect to the population of massive galaxies. This evolution is independent of environment, i.e., the same for clusters and the field. Furthermore, considering only cluster galaxies, we find that no differences can be detected in their mass functions either within the virialised regions, or when we compare galaxies inside and outside the virial radius. Finally, we find that red and blue galaxies have different mass functions. However, the shapes of the mass functions of blue and red galaxies do not seem to depend on their environment (clusters groups and the field).

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“…For all systems, we have assembled three-band optical VLT deep photometry, deep NTT/SOFI near-infrared imaging, and optical VLT/FORS2 spectroscopy (White et al 2005). We also acquired HST/ACS images in the F814W filter for 10 fields containing the most distant clusters studied by EDisCS.…”

Section: Sample Selection From Ediscsmentioning

confidence: 99%

“…Galaxies are considered to be cluster/group members if the integrated photometric redshift probability to be within z ± 0.1 of the cluster redshift is greater than a specific limit. These limits are based on our spectroscopy and range from 0.1 to 0.35 depending on the filter set available for each particular field (White et al 2005;Pelló et al 2008). Cluster/group membership for objects with spectroscopic observations is defined as being within ±3σ cl of z cl (Halliday et al 2004;Milvang-Jensen et al 2008).…”

Section: Sample Selection From Ediscsmentioning

confidence: 99%

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Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

Barazza¹,

Jablonka

Desai

et al. 2009

A&A

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We present a study of large-scale bars in field and cluster environments out to redshifts of ∼0.8 using a final sample of 945 moderately inclined disk galaxies drawn from the EDisCS project. We characterize bars and their host galaxies and look for relations between the presence of a bar and the properties of the underlying disk. We investigate whether the fraction and properties of bars in clusters are different from their counterparts in the field. The properties of bars and disks are determined by ellipse fits to the surface brightness distribution of the galaxies using HST/ACS images in the F814W filter. The bar identification is based on quantitative criteria after highly inclined (>60 • ) systems have been excluded. The total optical bar fraction in the redshift range z = 0.4−0.8 (median z = 0.60), averaged over the entire sample, is 25% (20% for strong bars). For the cluster and field subsamples, we measure bar fractions of 24% and 29%, respectively. We find that bars in clusters are on average longer than in the field and preferentially found close to the cluster center, where the bar fraction is somewhat higher (∼31%) than at larger distances (∼18%). These findings however rely on a relatively small subsample and might be affected by small number statistics. In agreement with local studies, we find that disk-dominated galaxies have a higher optical bar fraction (∼45%) than bulge-dominated galaxies (∼15%). This result is based on Hubble types and effective radii and does not change with redshift. The latter finding implies that bar formation or dissolution is strongly connected to the emergence of the morphological structure of a disk and is typically accompanied by a transition in the Hubble type. The question whether internal or external factors are more important for bar formation and evolution cannot be answered definitely. On the one hand, the bar fraction and properties of cluster and field samples of disk galaxies are quite similar, indicating that internal processes are crucial for bar formation. On the other hand, we find evidence that cluster centers are favorable locations for bars, which suggests that the internal processes responsible for bar growth are supported by the typical interactions taking place in such environments.

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EDisCS – the ESO distant cluster survey

Cited by 130 publications

References 64 publications

JKCS 041: a colour-detected galaxy cluster at $z_{\mathrm{phot}}$ ~ 1.9 with deep potential well as confirmed by X-ray data

JKCS 041: a colour-detected galaxy cluster at $z_{\mathrm{phot}}$ ~ 1.9 with deep potential well as confirmed by X-ray data

The galaxy stellar mass function and its evolution with time show no dependence on global environment

Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

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