LoCuSS: Testing hydrostatic equilibrium in galaxy clusters

Smith, Graham P.; Mazzotta, P.; Okabe, Nobuhiko; Ziparo, F.; Mulroy, Sarah L.; Babul, Arif; Finoguenov, A.; McCarthy, Ian G.; Lieu, M.; Bahé, Yannick M.; Bourdin, H.; Evrard, A. E.; Futamase, Toshifumi; Haines, C. P.; Jauzac, Mathilde; Marrone, Daniel P.; Martino, R.; May, Paul Edward; Taylor, James E.; Umetsu, Keiichi

doi:10.1093/mnrasl/slv175

Cited by 114 publications

(124 citation statements)

References 40 publications

Supporting

Mentioning

111

Contrasting

Order By: Relevance

“…) than both the Smith et al (2016) lensing determination and the Rines et al (2016) determination, also based on velocity dispersions; both determinations favor little or no mass bias. However, we agree within 1σ with the results from WtG (von der Linden et al 2014), the CCCP (Hoekstra et al 2015), 13 There is some confusion in the nature of these corrections.…”

Section: Discussionmentioning

confidence: 90%

“…13 Smith et al (2016) use three sets of independent mass measurements to study the departures from hydrostatic equilibrium in the Local Cluster Substructure Survey (LoCuSS) sample of 50 clusters at z 0.15 0.3 < <…”

Section: Discussionmentioning

confidence: 99%

“…Several recent WL calibrations of the Planck cluster scale have found results in the range of b 0 30 < < %, at the 10% precision level (von der Linden et al 2014;Hoekstra et al 2015;Simet et al 2017a;Smith et al 2016). Melin & Bartlett (2015) propose a new technique to measure cluster masses through lensing of CMB temperature anisotropies.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Calibrating the Planck Cluster Mass Scale with Cluster Velocity Dispersions

Amodeo

Mei

Stanford

et al. 2017

ApJ

View full text Add to dashboard Cite

We measure the Planck cluster mass bias using dynamical mass measurements based on velocity dispersions of a subsample of 17 Planck-detected clusters. The velocity dispersions were calculated using redshifts determined from spectra that were obtained at the Gemini observatory with the GMOS multi-object spectrograph. We correct our estimates for effects due to finite aperture, Eddington bias, and correlated scatter between velocity dispersion and the Planck mass proxy. The result for the mass bias parameter, , an error of 17% on the mass bias measurement with 17 clusters. This mass bias value is consistent with most previous weak-lensing determinations. It lies within 1s of the value that is needed to reconcile the Planck cluster counts with the Planck primary cosmic microwave background constraints. We emphasize that uncertainty in the velocity bias severely hampers the precision of the measurements of the mass bias using velocity dispersions. On the other hand, when we fix the Planck mass bias using the constraints from PennaLima et al., based on weak-lensing measurements, we obtain a positive velocity bias of b 0.9 v  at 3s.

show abstract

Section: Discussionmentioning

confidence: 90%

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Calibrating the Planck Cluster Mass Scale with Cluster Velocity Dispersions

Amodeo

Mei

Stanford

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…Okabe & Smith (2015) presented weak-lensing mass measurements for the LoCuSS sample and found results ∼10% lower than WtG, but in good agreement with CCCP and CLASH (Donahue et al 2014). While WtG and CCCP indicate a bias of the order of 20−30% in the mass calibration adopted by the Planck team (Planck Collaboration XI 2011), Smith et al (2016) showed that the LoCuSS data are consistent with no bias, depending on the method adopted to compute the sample average. No consensus has thus been reached on the true value of the hydrostatic bias (see also Sereno & Ettori 2015;Applegate et al 2016).…”

Section: Comparison With Previous Measurementsmentioning

confidence: 98%

The XXL Survey

Eckert

Ettori

Coupon

et al. 2016

A&A

Self Cite

115

View full text Add to dashboard Cite

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.

show abstract

“…The hydrostatic bias necessary to reconcile the Planck data sets is a factor of two larger than the expectation from simulations. Recently there has been a significant effort to characterize the bias using other observables that are insensitive to the hydrodynamical state of the ICM, primarily gravitational weak lensing (von der Linden et al 2014;Hoekstra et al 2015;Smith et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the Mass, Concentration, and Nonthermal Pressure Support of Six CLASH Clusters from a Joint Analysis of X-Ray, SZ, and Lensing Data

Siegel

Sayers

Mahdavi

et al. 2018

ApJ

View full text Add to dashboard Cite

We present a joint analysis of Chandra X-ray observations, Bolocam thermal Sunyaev-Zel'dovich (SZ) effect observations, Hubble Space Telescope (HST) strong-lensing data, and HST and Subaru Suprime-Cam weak-lensing data. The multiwavelength data set is used to constrain parametric models for the distribution of dark and baryonic matter in a sample of six massive galaxy clusters selected from the Cluster Lensing And Supernova survey with Hubble (CLASH). For five of the six clusters, the multiwavelength data set is well described by a relatively simple model that assumes spherical symmetry, hydrostatic equilibrium, and entirely thermal pressure support. The joint analysis yields considerably better constraints on the total mass and concentration of the clusters compared to analysis of any one data set individually. The resulting constraints are consistent with simulation-based predictions for the concentration-mass relation. The subsample of five galaxy clusters is used to place an upper limit on the fraction of pressure support in the intracluster medium (ICM) due to nonthermal processes, such as turbulence and bulk flow of the gas. We constrain the nonthermal pressure fraction at r 500c to be <0.11 at 95% confidence. This is in tension with state-of-the-art hydrodynamical simulations, which predict a nonthermal pressure fraction of ≈0.25 at r 500c for clusters of similar mass and redshift. This tension may be explained by the sample selection and/or our assumption of spherical symmetry.

show abstract

LoCuSS: Testing hydrostatic equilibrium in galaxy clusters

Cited by 114 publications

References 40 publications

Calibrating the Planck Cluster Mass Scale with Cluster Velocity Dispersions

Calibrating the Planck Cluster Mass Scale with Cluster Velocity Dispersions

The XXL Survey

Constraints on the Mass, Concentration, and Nonthermal Pressure Support of Six CLASH Clusters from a Joint Analysis of X-Ray, SZ, and Lensing Data

Contact Info

Product

Resources

About