The DAFT/FADA survey

Guennou, L.; Adami, C.; Ulmer, M. P.; Lebrun, V.; Durret, F.; Johnston, David; Ilbert, O.; Clowe, Douglas; Gavazzi, R.; Murphy, Kellen; Schrabback, T.; Allam, S.; Annis, J.; Basa, S.; Benoist, Christophe; Biviano, A.; Cappi, A.; Kubo, Jeffrey M.; Marshall, Phil; Mazure, A.; Rostagni, F.; Russeil, D.; Slezak, E.

doi:10.1051/0004-6361/201015174

Cited by 25 publications

(37 citation statements)

References 33 publications

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“…Second, late-type galaxies in luminous and moderately luminous clusters (as well as in C0 clusters) also exhibit higher uncertainties than early-type galaxies, by a factor of 2 in luminous clusters and by 50% in moderately luminous and C0 clusters. This behavior was already detected in Guennou et al (2010).…”

Section: A1 General Agreement Between Spectroscopic and Photometricsupporting

confidence: 59%

The XMM-LSS survey: optical assessment and properties of different X-ray selected cluster classes

Adami

Mazure

Pierre

et al. 2010

A&A

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Context. XMM and Chandra opened a new area for the study of clusters of galaxies not only for cluster physics, but also for the detection of faint and distant clusters that were inaccessible with previous missions. Aims. This article presents 66 spectroscopically confirmed clusters (0.05 ≤ z ≤ 1.5) within an area of 6 deg 2 enclosed in the XMM-LSS survey. Almost two thirds have been confirmed with dedicated spectroscopy only and 10% have been confirmed with dedicated spectroscopy supplemented by literature redshifts. Methods. Sub-samples, or classes, of extended-sources are defined in a two-dimensional X-ray parameter space allowing for various degrees of completeness and contamination. We describe the procedure developed to assess the reality of these cluster candidates using the CFHTLS photometric data and spectroscopic information from our own follow-up campaigns. Results. Most of these objects are low-mass clusters, hence constituting a still poorly studied population. In a second step, we quantify the correlations between the optical properties such as richness or velocity dispersion and the cluster X-ray luminosities. We examine the relation of the clusters to the cosmic web. Finally, we review peculiar compact structures in the surveyed area such as very distant clusters and fossil groups.

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Section: A1 General Agreement Between Spectroscopic and Photometricsupporting

confidence: 59%

The XMM-LSS survey: optical assessment and properties of different X-ray selected cluster classes

Adami

Mazure

Pierre

et al. 2010

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“…Furthermore, it is reasonable to conclude 10 This suggests that the COSMOS galaxy templates are less adequate to represent the characteristics of the galaxy populations of XMMU J0338.7+0030. An analogous point was made by Guennou et al (2010), who discussed photometric redshifts along lines of sight to 10 clusters at spectroscopic redshifts between 0.48 and 0.79 obtained with the same COSMOS galaxy templates and photo-z code used here. 11 Colours redder than I − K = 4 Vega mag statistically select EROs at z ∼ 1−2 (Pozzetti & Mannucci 2000, and references therein; see also Pierini et al 2004aPierini et al , 2005.…”

Section: The Photometric-redshift Distribution Functionsupporting

confidence: 55%

First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND

Pierini

Šuhada

Fassbender

et al. 2012

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Context. The XMM-Newton Distant Cluster Project is a serendipitous survey for clusters of galaxies at redshifts z ≥ 0.8 based on deep archival XMM-Newton observations. X-ray sources identified as extended are screened against existing optical all-sky surveys for galaxies, in case of candidate high-z clusters followed up with imaging at 4 m-class telescopes and, ultimately, multi-object spectroscopy at 8 m-class telescopes. Low-significance candidate high-z clusters are followed up with the seven-channel imager GROND (Gamma-Ray Burst Optical and Near-Infrared Detector) that is mounted at a 2 m-class telescope. Its unique capability of simultaneous imaging in the g , r , i , z , J, H, Ks bands enables the use of the photometric redshift technique. Aims. Observing strategy, data reduction and analysis, depth and accuracy of the simultaneous multi-wavelength photometry are discussed with the goal of establishing GROND as a useful instrument to confirm X-ray selected (high-z) clusters. Methods. The test case is XMMU J0338.7+0030, suggested to be at z ∼ 1.45 ± 0.15 (1σ) from the analysis of the z − H vs. H colour−magnitude diagram obtained from the follow-up imaging. Later VLT-FORS2 spectroscopy enabled us to identify four members, which set this cluster at z = 1.097 ± 0.002 (1σ). To reach a better knowledge of its galaxy population, we observed XMMU J0338.7+0030 with GROND for about 6 h. The publicly available photo-z code le Phare was used. Results. The Ks-band number counts of the non-stellar sources out of the 832 detected down to z ∼ 26 AB mag (1σ) in the 3.9×4.3 arcmin 2 region of XMMU J0338.7+0030 imaged at all GROND bands clearly exceed those computed in deep fields/survey areas at ∼20.5-22.5 AB mag. The photo-z's of the three imaged spectroscopic members yield z = 1.12 ± 0.09 (1σ). The spatial distribution and the properties of the GROND sources with a photo-z in the range 1.01-1.23 confirm the correspondence of the X-ray source with a galaxy over-density at a significance of at least 4.3σ. Candidate members that are spectro-photometrically classified as elliptical galaxies define a red locus in the i −z vs. z colour−magnitude diagram that is consistent with the red sequence of the cluster RDCS J0910+5422 at z = 1.106. XMMU J0338.7+0030 hosts also a population of bluer late-type spirals and irregulars. The starbursts among the photometric members populate both loci, consistently with previous results. Conclusions. The analysis of the available data set indicates that XMMU J0338.7+0030 is a low-mass cluster (M 200 ∼ 10 14 M ) at z = 1.1. With the photometric accuracy yielded by the present unoptimized multi-band observations with GROND, we not only confirm the spectroscopic redshift of this cluster but also show that it hosts a galaxy population that can still undergo significant bursts of star-formation activity.

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“…This cluster is part of the DAFT/FADA survey (Guennou et al 2010) and the analysis presented here is proof of concept for similar analyses to be performed on other clusters of the DAFT/FADA sample.…”

Section: Introductionmentioning

confidence: 58%

“…We refer to Guennou et al (2010) for a complete description of the optical and infrared imaging data and for the evaluation of photometric redshifts, z p . These photometric redshifts are characterized by typical uncertainties lower than 0.1 up to z ∼1.5 for galaxies brighter than F814W = 22.5, or up to z ∼1 for galaxies brighter than F814W = 24.…”

Section: Optical and Near-infrared Imagingmentioning

confidence: 99%

Mass profile and dynamical status of thez~ 0.8 galaxy cluster LCDCS 0504

Guennou¹,

Biviano²,

Adami³

et al. 2014

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Context. Constraints on the mass distribution in high-redshift clusters of galaxies are currently not very strong. Aims. We aim to constrain the mass profile, M(r), and dynamical status of the z ∼ 0.8 LCDCS 0504 cluster of galaxies that is characterized by prominent giant gravitational arcs near its center. Methods. Our analysis is based on deep X-ray, optical, and infrared imaging as well as optical spectroscopy, collected with various instruments, which we complemented with archival data. We modeled the mass distribution of the cluster with three different mass density profiles, whose parameters were constrained by the strong lensing features of the inner cluster region, by the X-ray emission from the intracluster medium, and by the kinematics of 71 cluster members. Results. We obtain consistent M(r) determinations from three methods based on kinematics (dispersion-kurtosis, caustics, and MAMPOSSt), out to the cluster virial radius, 1.3 Mpc and beyond. The mass profile inferred by the strong lensing analysis in the central cluster region is slightly higher than, but still consistent with, the kinematics estimate. On the other hand, the X-ray based M(r) is significantly lower than the kinematics and strong lensing estimates. Theoretical predictions from ΛCDM cosmology for the concentration-mass relation agree with our observational results, when taking into account the uncertainties in the observational and theoretical estimates. There appears to be a central deficit in the intracluster gas mass fraction compared with nearby clusters. Conclusions. Despite the relaxed appearance of this cluster, the determinations of its mass profile by different probes show substantial discrepancies, the origin of which remains to be determined. The extension of a dynamical analysis similar to that of other clusters of the DAFT/FADA survey with multiwavelength data of sufficient quality will allow shedding light on the possible systematics that affect the determination of mass profiles of high-z clusters, which is possibly related to our incomplete understanding of intracluster baryon physics.

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The DAFT/FADA survey

Cited by 25 publications

References 33 publications

The XMM-LSS survey: optical assessment and properties of different X-ray selected cluster classes

The XMM-LSS survey: optical assessment and properties of different X-ray selected cluster classes

First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND

Mass profile and dynamical status of thez~ 0.8 galaxy cluster LCDCS 0504

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