The XMM-BCS galaxy cluster survey

Šuhada, R.; Song, J.; Böhringer, H.; Mohr, J. J.; Chon, G.; Finoguenov, A.; Fassbender, R.; Desai, S.; Armstrong, R.; Zenteno, A.; Barkhouse, W. A.; Bertin, E.; Buckley-Geer, E.; Hansen, S. M.; High, F. W.; Lin, Huan; Mühlegger, M.; Ngeow, Chow-Choong; Pierini, D.; Pratt, G. W.; Verdugo, M.; Tucker, D. L.

doi:10.1051/0004-6361/201117214

Cited by 49 publications

(24 citation statements)

References 76 publications

(110 reference statements)

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“…The XXL-100-GC 1 sample is a flux-limited sample based on 100 clusters ranked brightest in flux. It is described in detail by Pacaud et al (2016, Paper II, hereafter), some of these clusters have previously been described in the XMM-LSS and XMM-BCS studies (Clerc et al 2014;Šuhada et al 2012). We note that five systems (XLSSC 113,114,115,550,and 551) were observed in bad pointings that are contaminated by flaring.…”

Section: Survey and Sample Definitionsupporting

confidence: 62%

The XXL Survey

Lieu

Smith

Giles

et al. 2016

A&A

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Context. The XXL Survey is the largest survey carried out by XMM-Newton. Covering an area of 50 deg 2 , the survey contains ∼450 galaxy clusters out to a redshift ∼2 and to an X-ray flux limit of ∼5 × 10 −15 erg s −1 cm −2 . This paper is part of the first release of XXL results focussed on the bright cluster sample. Aims. We investigate the scaling relation between weak-lensing mass and X-ray temperature for the brightest clusters in XXL. The scaling relation discussed in this article is used to estimate the mass of all 100 clusters in XXL-100-GC. Methods. Based on a subsample of 38 objects that lie within the intersection of the northern XXL field and the publicly available CFHTLenS shear catalog, we derive the weak-lensing mass of each system with careful considerations of the systematics. The clusters lie at 0.1 < z < 0.6 and span a temperature range of T 1−5 keV. We combine our sample with an additional 58 clusters from the literature, increasing the range to T 1−10 keV. To date, this is the largest sample of clusters with weak-lensing mass measurements that has been used to study the mass-temperature relation. Results. The mass-temperature relation fit (M ∝ T b ) to the XXL clusters returns a slope b = 1.78−0.32 and intrinsic scatter σ ln M|T 0.53; the scatter is dominated by disturbed clusters. The fit to the combined sample of 96 clusters is in tension with selfsimilarity, b = 1.67 ± 0.12 and σ ln M|T 0.41. Conclusions. Overall our results demonstrate the feasibility of ground-based weak-lensing scaling relation studies down to cool systems of ∼1 keV temperature and highlight that the current data and samples are a limit to our statistical precision. As such we are unable to determine whether the validity of hydrostatic equilibrium is a function of halo mass. An enlarged sample of cool systems, deeper weak-lensing data, and robust modelling of the selection function will help to explore these issues further.Key words. gravitational lensing: weak -X-rays: galaxies: clusters -galaxies: groups: general -galaxies: clusters: general The Master catalogue is available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via

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Section: Survey and Sample Definitionsupporting

confidence: 62%

The XXL Survey

Lieu

Smith

Giles

et al. 2016

A&A

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“…Some of these clusters were previously studied as part of the XMM-LSS and XMM-BCS surveys (Clerc et al 2014;Šuhada et al 2012) and span a wide redshift range (0.05 < ∼ z < ∼ 1.07). All systems within the XXL-100-GC sample are characterised as either C1 or C2 classification.…”

Section: Sample and Datamentioning

confidence: 99%

The XXL Survey

Ziparo

Smith

Mulroy

et al. 2016

A&A

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Galaxy clusters and groups are important cosmological probes and giant cosmic laboratories for studying galaxy evolution. Much effort has been devoted to understanding how and when baryonic matter cools at the centre of potential wells. However, a clear picture of the efficiency with which baryons are converted into stars is still missing. We present the K-band luminosity-halo mass relation, L K,500 − M 500,WL , for a subsample of 20 of the 100 brightest clusters in the XXL Survey observed with WIRCam at the Canada-France-Hawaii Telescope (CFHT). For the first time, we have measured this relation via weak-lensing analysis down to M 500,WL = 3.5 × 10 13 M . This allows us to investigate whether the slope of the L K − M relation is different for groups and clusters, as seen in other works. The clusters in our sample span a wide range in mass, M 500,WL = 0.35−12.10 × 10 14 M , at 0 < z < 0.6. The K-band luminosity scales as log 10 (L K,500 /10 12 L ) ∝ β log 10 (M 500,WL /10 14 M ) with β = 0.85 +0.35 −0.27 and an intrinsic scatter of σ ln L K |M = 0.37 +0.19 −0.17 . Combining our sample with some clusters in the Local Cluster Substructure Survey (LoCuSS) present in the literature, we obtain a slope of 1.05 +0.16 −0.14 and an intrinsic scatter of 0.14 +0.09 −0.07 . The flattening in the L K − M seen in previous works is not seen here and might be a result of a bias in the mass measurement due to assumptions on the dynamical state of the systems. We also study the richness-mass relation and find that group-sized halos have more galaxies per unit halo mass than massive clusters. However, the brightest cluster galaxy (BCG) in low-mass systems contributes a greater fraction to the total cluster light than BCGs do in massive clusters; the luminosity gap between the two brightest galaxies is more prominent for group-sized halos. This result is a natural outcome of the hierarchical growth of structures, where massive galaxies form and gain mass within low-mass groups and are ultimately accreted into more massive clusters to become either part of the BCG or one of the brighter galaxies.

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“…Finoguenov et al 2007Finoguenov et al , 2010Šuhada et al 2012;Clerc et al 2014;Pierre et al 2016), in addition to serendipitous cluster surveys in the archival observations that provide a relatively large area of a few hundred square degrees (e.g. Barkhouse et al 2006; Kolokotronis et al 2006;Lamer et al 2008;Fassbender et al 2011;Takey et al 2011Takey et al , 2013Mehrtens et al 2012;Clerc et al 2012;Tundo et al 2012;de Hoon et al 2013;Takey et al 2014).…”

Section: Introductionmentioning

confidence: 99%

The 3XMM/SDSS Stripe 82 Galaxy Cluster Survey

Takey

Durret

Mahmoud

et al. 2016

A&A

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We present a galaxy cluster survey based on XMM-Newton observations that are located in Stripe 82 of the Sloan Digital Sky Survey (SDSS). The survey covers an area of 11.25 deg 2 . The X-ray cluster candidates were selected as serendipitously extended detected sources from the third XMM-Newton serendipitous source catalogue (3XMM-DR5). A cross-correlation of the candidate list that comprises 94 objects with recently published X-ray and optically selected cluster catalogues provided optical confirmations and redshift estimates for about half of the candidate sample. We present a catalogue of X-ray cluster candidates previously known in X-ray and/or optical bands from the matched catalogues or NED. The catalogue consists of 54 systems with redshift measurements in the range of 0.05-1.19 with a median of 0.36. Of these, 45 clusters have spectroscopic confirmations as stated in the matched catalogues. We spectroscopically confirmed another 6 clusters from the available spectroscopic redshifts in the SDSS-DR12. The cluster catalogue includes 17 newly X-ray discovered clusters, while the remainder were detected in previous XMM-Newton and/or ROSAT cluster surveys. Based on the available redshifts and fluxes given in the 3XMM-DR5 catalogue, we estimated the X-ray luminosities and masses for the cluster sample. We also present the list of the remaining X-ray cluster candidates (40 objects) that have no redshift information yet in the literature. Of these candidates, 25 sources are considered as distant cluster candidates beyond a redshift of 0.6. We also searched for galaxy cluster mergers in our cluster sample and found two strong candidates for newly discovered cluster mergers at redshifts of 0.11 and 0.26. The X-ray and optical properties of these systems are presented.

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The XMM-BCS galaxy cluster survey

Cited by 49 publications

References 76 publications

The XXL Survey

The XXL Survey

The XXL Survey

The 3XMM/SDSS Stripe 82 Galaxy Cluster Survey

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