The XXL Survey

Lieu, M.; Smith, Graham P.; Giles, Paul; Ziparo, F.; Maughan, B. J.; Démoclès, J.; Pacaud, F.; Pierre, M.; Adami, C.; Bahé, Yannick M.; Clerc, N.; Chiappetti, L.; Eckert, D.; Ettori, S.; Lavoie, S.; Fèvre, J. P. Le; McCarthy, Ian G.; Kilbinger, M.; Ponman, T. J.; Sadibekova, T.; Willis, Jon

doi:10.1051/0004-6361/201526883

Cited by 79 publications

(110 citation statements)

References 66 publications

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“…The cluster is referred to as XXL091 in the XXL survey (Eckert et al 2016), and has Mgas = 5.00 is derived from a scaling relation between WL mass and X-ray temperature (Lieu et al 2016). We find that our measurement Mgas = 5.10 70 M⊙ within the same radius is in good agreement with Eckert et al (2016 …”

Section: Mcxcj02317-0451supporting

confidence: 70%

Multiwavelength study of X-ray luminous clusters in the Hyper Suprime-Cam Subaru Strategic Program S16A field

Miyaoka¹,

Okabe²,

Kitaguchi³

et al. 2017

Publications of the Astronomical Society of Japan

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We present a joint X-ray, optical and weak-lensing analysis for X-ray luminous galaxy clusters selected from the MCXC (Meta-Catalog of X-Ray Detected Clusters of Galaxies) cluster catalog in the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) survey field with S16A data, As a pilot study of our planned series papers, we measure hydrostatic equilibrium (H.E.) masses using XMM-Newton data for four clusters in the current coverage area out of a sample of 22 MCXC clusters. We additionally analyze a non-MCXC cluster associated with one MCXC cluster. We show that H.E. masses for the MCXC clusters are correlated with cluster richness from the CAMIRA catalog , while that for the non-MCXC cluster deviates from the scaling relation. The mass normalization of the relationship between the cluster richness and H.E. mass is compatible with one inferred by matching CAMIRA cluster abundance with a theoretical halo mass function. The mean gas mass fraction based on H.E. masses for the MCXC clusters is f gas = 0.125 ± 0.012 at spherical overdensity ∆ = 500, which is ∼ 80 − 90 percent of the cosmic mean baryon fraction, Ω b /Ω m , measured by cosmic microwave background experiments. We find that the mean baryon fraction estimated from X-ray and HSC-SSP optical data is comparable to Ω b /Ω m . A weak-lensing shear catalog of background galaxies, combined with photometric redshifts, is currently available only for three clusters in our sample. Hydrostatic equilibrium masses roughly agree with weak-lensing masses, albeit with large uncertainty. This study demonstrates that further multiwavelength study for a large sample of clusters using X-ray, HSC-SSP optical and weak lensing data will enable us to understand cluster physics and utilize cluster-based cosmology.

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Section: Mcxcj02317-0451supporting

confidence: 70%

Multiwavelength study of X-ray luminous clusters in the Hyper Suprime-Cam Subaru Strategic Program S16A field

Miyaoka¹,

Okabe²,

Kitaguchi³

et al. 2017

Publications of the Astronomical Society of Japan

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“…The observed gas fraction is generally found to increase with radius because of non-gravitational energy input (Allen et al 2004;Vikhlinin et al 2006;Eckert et al 2013) and it converges toward the value of ∼13% at r 500 . The stellar content of cluster galaxies and intracluster light generally represents 10−20% of the total baryonic mass (Lin & Mohr 2004;Gonzalez et al 2007;Andreon 2010Andreon , 2015Mulroy et al 2014). The overall baryon content of galaxy clusters is therefore found to be close to the Universal value (Lin et al 2003;Giodini et al 2009;Laganá et al 2013).…”

Section: Introductionmentioning

confidence: 79%

“…Temperatures and luminosities within a fixed radius of 300 kpc were measured from the survey data and presented in Paper III. Halo masses were measured directly through weak lensing for 38 z < 0.6 clusters coinciding with the CFHTLS survey (Lieu et al 2016, hereafter Paper IV; see Sect. 4.1), which allowed us to directly calibrate the relation between weak-lensing mass and X-ray temperature using a subset of the XXL-100-GC.…”

Section: Cluster Samplementioning

confidence: 99%

The XXL Survey

Eckert

Ettori

Coupon

et al. 2016

A&A

Self Cite

115

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Traditionally, galaxy clusters have been expected to retain all the material accreted since their formation epoch. For this reason, their matter content should be representative of the Universe as a whole, and thus their baryon fraction should be close to the Universal baryon fraction Ω b /Ω m . We make use of the sample of the 100 brightest galaxy clusters discovered in the XXL Survey to investigate the fraction of baryons in the form of hot gas and stars in the cluster population. Since it spans a wide range of mass (10 13 −10 15 M ) and redshift (0.05−1.1) and benefits from a large set of multiwavelength data, the XXL-100-GC sample is ideal for measuring the global baryon budget of massive halos. We measure the gas masses of the detected halos and use a mass-temperature relation directly calibrated using weak-lensing measurements for a subset of XXL clusters to estimate the halo mass. We find that the weak-lensing calibrated gas fraction of XXL-100-GC clusters is substantially lower than was found in previous studies using hydrostatic masses. Our best-fit relation between gas fraction and mass reads f gas,500 = 0.055 +0.007 −0.006 M 500 /10 14 M 0.21 +0.11 −0.10 . The baryon budget of galaxy clusters therefore falls short of the Universal baryon fraction by about a factor of two at r 500,MT . Our measurements require a hydrostatic bias 1 − b = M X /M WL = 0.72 +0.08 −0.07 to match the gas fraction obtained using lensing and hydrostatic equilibrium, which holds independently of the instrument considered. Comparing our gas fraction measurements with the expectations from numerical simulations, we find that our results favour an extreme feedback scheme in which a significant fraction of the baryons are expelled from the cores of halos. This model is, however, in contrast with the thermodynamical properties of observed halos, which might suggest that weak-lensing masses are overestimated. In light of these results, we note that a mass bias 1 − b = 0.58 as required to reconcile Planck cosmic microwave background and cluster counts should translate into an even lower baryon fraction, which poses a major challenge to our current understanding of galaxy clusters.

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“…seeing, depth). The production of the weight maps was possible via the WeightWatcher software (Marmo & Bertin 2008), while astrometric and photometric calibration was performed using SCAMP (Bertin 2006) with the Two Micron All Sky Survey (2MASS) taken as the astrometric reference catalogue.…”

Section: Optical and Near-infrared Imagingmentioning

confidence: 99%

The XXL Survey

Ziparo

Smith

Mulroy

et al. 2016

A&A

Self Cite

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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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The XXL Survey

Cited by 79 publications

References 66 publications

Multiwavelength study of X-ray luminous clusters in the Hyper Suprime-Cam Subaru Strategic Program S16A field

Multiwavelength study of X-ray luminous clusters in the Hyper Suprime-Cam Subaru Strategic Program S16A field

The XXL Survey

The XXL Survey

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