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

Adami, C.; Mazure, A.; Pierre, M.; Sprimont, Pierre-Guillaume; Libbrecht, C.; Pacaud, F.; Clerc, N.; Sadibekova, T.; Surdej, Jean; Altiéri, B.; Duc, Pierre–Alain; Galaz, Gaspar; Gueguen, A.; Guennou, L.; Hertling, G.; Ilbert, O.; Fèvre, J. P. Le; Quintana, H.; Valtchanov, I.; Willis, Jon; Akiyama, Masayuki; Aussel, H.; Chiappetti, L.; Detal, Alain; Garilli, B.; Lebrun, V.; LeFèvre, O.; Maccagni, D.; Melin, J.-B.; Ponman, T. J.; Ricci, Davide; Tresse, L.

doi:10.1051/0004-6361/201015182

Cited by 64 publications

(91 citation statements)

References 59 publications

(123 reference statements)

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“…One of the main results of G10 was that the precision of our photometric redshifts was sometimes degraded by a factor of two when considering cluster galaxies (see also Adami et al 2011). This is probably due to a lack of galaxy templates typical of high density regions.…”

Section: Extinction and Photometric Redshiftsmentioning

confidence: 96%

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The evolution of the cluster optical galaxy luminosity function betweenz= 0.4 and 0.9 in the DAFT/FADA survey

Martinet

Durret

Guennou

et al. 2015

A&A

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Context. There is some disagreement about the abundance of faint galaxies in high-redshift clusters, with contradictory results in the literature arising from studies of the optical galaxy luminosity function (GLF) for small cluster samples. Aims. We compute GLFs for one of the largest medium-to-high-redshift (0.4 ≤ z < 0.9) cluster samples to date in order to probe the abundance of faint galaxies in clusters. We also study how the GLF depends on cluster redshift, mass, and substructure and compare the GLFs of clusters with those of the field. We separately investigate the GLFs of blue and red-sequence (RS) galaxies to understand the evolution of different cluster populations. Methods. We calculated the GLFs for 31 clusters taken from the DAFT/FADA survey in the B, V, R, and I rest-frame bands. We used photometric redshifts computed from BVRIZ J images to constrain galaxy cluster membership. We carried out a detailed estimate of the completeness of our data. We distinguished the red-sequence and blue galaxies using a V − I versus I colour−magnitude diagram. We studied the evolution of these two populations with redshift. We fitted Schechter functions to our stacked GLFs to determine average cluster characteristics. Results. We find that the shapes of our GLFs are similar for the B, V, R, and I bands with a drop at the red GLF faint ends that is more pronounced at high redshift: α red ∼ −0.5 at 0.40 ≤ z < 0.65 and α red > 0.1 at 0.65 ≤ z < 0.90. The blue GLFs have a steeper faint end (α blue ∼ −1.6) than the red GLFs, which appears to be independent of redshift. For the full cluster sample, blue and red GLFs meet at M V = −20, M R = −20.5, and M I = −20.3. A study of how galaxy types evolve with redshift shows that late-type galaxies appear to become early types between z ∼ 0.9 and today. Finally, the faint ends of the red GLFs of more massive clusters appear to be richer than less massive clusters, which is more typical of the lower redshift behaviour. Conclusions. Our results indicate that these clusters form at redshifts higher than z = 0.9 from galaxy structures that already have an established red sequence. Late-type galaxies then appear to evolve into early types, enriching the red sequence between this redshift and today. This effect is consistent with the evolution of the faint-end slope of the red sequence and the galaxy type evolution that we find. Finally, faint galaxies accreted from the field environment at all redshifts might have replaced the blue late-type galaxies that converted into early types, explaining the lack of evolution in the faint-end slopes of the blue GLFs.

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Section: Extinction and Photometric Redshiftsmentioning

confidence: 96%

“…To do so, we select cluster galaxies in the XXM-LSS survey (e.g. Adami et al 2011) with spectroscopic redshifts and check their corresponding photo-zs in the CFHTLS. We then calculate the photo-z uncertainties for this sample (I < 22.5 and z < 1.05) using LePhare and plot them in Fig.…”

Section: Photometric Redshift Qualitymentioning

confidence: 99%

The evolution of the cluster optical galaxy luminosity function betweenz= 0.4 and 0.9 in the DAFT/FADA survey

Martinet

Durret

Guennou

et al. 2015

A&A

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“…We have examined each of the non-matches by splitting the sample according to the X-CLASS distance estimates. Following the criteria defined for the XMM-LSS cluster confirmation, we declare that a cluster is confirmed either when at least three galaxies with concordant redshifts are available within a radius of 500 kpc around the X-ray centroid or when the cD has a spectroscopic redshift (Adami et al 2011). We note that z min−redMaPPer is the lowest possible redshift value of the redMaPPer clusters: z min−redMaPPer = 0.054.…”

Section: What Are the X-class Clusters Not Having A Redmapper Countermentioning

confidence: 99%

The X-CLASS−redMaPPer galaxy cluster comparison

Sadibekova

Pierre

Clerc

et al. 2014

A&A

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Context. This paper is the first in a series undertaking a comprehensive correlation analysis between optically selected and X-rayselected cluster catalogues. The rationale of the project is to develop a holistic picture of galaxy clusters utilising optical and X-raycluster-selected catalogues with well-understood selection functions. Aims. Unlike most of the X-ray/optical cluster correlations to date, the present paper focuses on the non-matching objects in either waveband. We investigate how the differences observed between the optical and X-ray catalogues may stem from (1) a shortcoming of the detection algorithms; (2) dispersion in the X-ray/optical scaling relations; or (3) substantial intrinsic differences between the cluster populations probed in the X-ray and optical bands. The aim is to inventory and elucidate these effects in order to account for selection biases in the further determination of X-ray/optical cluster scaling relations. Methods. We correlated the X-CLASS serendipitous cluster catalogue extracted from the XMM archive with the redMaPPer optical cluster catalogue derived from the Sloan Digital Sky Survey (DR8). We performed a detailed and, in large part, interactive analysis of the matching output from the correlation. The overlap between the two catalogues has been accurately determined and possible cluster positional errors were manually recovered. The final samples comprise 270 and 355 redMaPPer and X-CLASS clusters, respectively. X-ray cluster matching rates were analysed as a function of optical richness. In the second step, the redMaPPer clusters were correlated with the entire X-ray catalogue, containing point and uncharacterised sources (down to a few 10 −15 erg s −1 cm −2 in the [0.5−2] keV band). A stacking analysis was performed for the remaining undetected optical clusters. Results. We find that all rich (λ ≥ 80) clusters are detected in X-rays out to z = 0.6. Below this redshift, the richness threshold for X-ray detection steadily decreases with redshift. Likewise, all X-ray bright clusters are detected by redMaPPer. After correcting for obvious pipeline shortcomings (about 10% of the cases both in optical and X-ray), ∼50% of the redMaPPer (down to a richness of 20) are found to coincide with an X-CLASS cluster; when considering X-ray sources of any type, this fraction increases to ∼80%; for the remaining objects, the stacking analysis finds a weak signal within 0.5 Mpc around the cluster optical centres. The fraction of clusters totally dominated by AGN-type emission appears to be a few percent. Conversely, ∼40% of the X-CLASS clusters are identified with a redMaPPer (down to a richness of 20) − part of the non-matches being due to the X-CLASS sample extending further out than redMaPPer (z < 1.5 vs. z < 0.6), but extending the correlation down to a richness of 5 raises the matching rate to ∼65%. Conclusions. This state-of-the-art study involving two well-validated cluster catalogues has shown itself to be complex, and it points to a number of issues inherent to blind c...

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“…In contrast, as the largest nonlinear objects in the present Universe, galaxy clusters are much rarer (current cluster samples have a density of about ten per deg 2 at most, e.g. Adami et al 2011), but their relationship with dark matter halo mass is controlled better. This means that their abundance is very sensitive to cosmological parameters (especially Ω m and σ 8 , Evrard 1989;Oukbir & Blanchard 1992), and has already been used to derive constraints on cosmology, but their clustering has not yet provided much cosmological information (because of low statistics).…”

Section: Introductionmentioning

confidence: 96%

Covariance matrices for halo number counts and correlation functions

Valageas

Clerc

Pacaud

et al. 2011

A&A

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Aims. We study the mean number counts and two-point correlation functions, along with their covariance matrices, of cosmological surveys such as for clusters. In particular, we consider correlation functions averaged over finite redshift intervals, which are well suited to cluster surveys or populations of rare objects, where one needs to integrate over nonzero redshift bins to accumulate enough statistics. Methods. We develop an analytical formalism to obtain explicit expressions of all contributions to these means and covariance matrices, taking into account both shot-noise and sample-variance effects. We compute low-order as well as high-order (including non-Gaussian) terms. Results. We derive expressions for the number counts per redshift bins both for the general case and for the small window approximation. We estimate the range of validity of Limber's approximation and the amount of correlation between different redshift bins. We also obtain explicit expressions for the integrated 3D correlation function and the 2D angular correlation. We compare the relative importance of shot-noise and sample-variance contributions, and of low-order and high-order terms. We check the validity of our analytical results through a comparison with the Horizon full-sky numerical simulations, and we obtain forecasts for several future cluster surveys.

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

Cited by 64 publications

References 59 publications

The evolution of the cluster optical galaxy luminosity function betweenz= 0.4 and 0.9 in the DAFT/FADA survey

The evolution of the cluster optical galaxy luminosity function betweenz= 0.4 and 0.9 in the DAFT/FADA survey

The X-CLASS−redMaPPer galaxy cluster comparison

Covariance matrices for halo number counts and correlation functions

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