Characterization of Intracluster Medium Temperature Distributions of 62 Galaxy Clusters With XMM-Newton

Frank, Kari A.; Peterson, J. R.; Andersson, Karl; Fabian, A. C.; Sanders, J. S.

doi:10.1088/0004-637x/764/1/46

Cited by 41 publications

(44 citation statements)

References 97 publications

(92 reference statements)

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“…Deep Chandra observations by Nulsen et al (2013) have revealed evidence for a minor merger ∼ 400 Myr ago. However, also based on Chandra data, Hofmann et al (2016) suggest that A2199 is an overall relaxed cluster (a result also found by Frank et al (2013) and Parekh et al (2015)) with a cool core and AGN feedback structures at its centre. These authors find a large scale asymmetry in the temperature distribution between the north and the south, which is also clearly visible in our temperature map.…”

Section: Appendix A: Notes On Individual Clustersmentioning

confidence: 53%

“…• Abell 3562: As A3558, this cluster is also a member of the Shapley supercluster. According to Frank et al (2013) and Parekh et al (2015), it is unrelaxed, as also suggested by its radio halo (Giovannini et al 2009). Matsushita (2011) classifies it as a non-cD cluster with a large deviation from symmetry and a rather large Fe abundance of ∼ 1.5 solar, as for A3558, but we do not measure such a high abundance in either of the two clusters.…”

Section: Appendix A: Notes On Individual Clustersmentioning

confidence: 96%

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Physical properties of the X-ray gas as a dynamical diagnosis for galaxy clusters

Laganá

Durret

Lopes

2019

Monthly Notices of the Royal Astronomical Society

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We analysed XMM-Newton EPIC data for 53 galaxy clusters. Through 2D spectral maps, we provide the most detailed and extended view of the spatial distribution of temperature (kT), pressure (P), entropy (S) and metallicity (Z) of galaxy clusters to date with the aim of correlating the dynamical state of the system to six cool-core diagnoses from the literature. With the objective of building 2D maps and resolving structures in kT, P, S and Z, we divide the data in small regions from which spectra can be extracted. Our analysis shows that when clusters are spherically symmetric the cool-cores (CC) are preserved, the systems are relaxed with little signs of perturbation, and most of the CC criteria agree. The disturbed clusters are elongated, show clear signs of interaction in the 2D maps, and most do not have a cool-core. However, 16 well studied clusters classified as CC by at least four criteria show spectral maps that appear disturbed. All of these clusters but one show clear signs of recent mergers, with a complex structure and geometry but with a cool-core that remains preserved. Thus, although very useful for CC characterization, most diagnoses are too simplistic to reproduce the overall structure and dynamics of galaxy clusters, and therefore the selection of relaxed systems according to these criteria may affect mass estimates. The complex structure of galaxy clusters can be reliably assessed through the 2D maps presented here.

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Section: Appendix A: Notes On Individual Clustersmentioning

confidence: 53%

Section: Appendix A: Notes On Individual Clustersmentioning

confidence: 96%

Physical properties of the X-ray gas as a dynamical diagnosis for galaxy clusters

Laganá

Durret

Lopes

2019

Monthly Notices of the Royal Astronomical Society

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“…Rasia et al 2004;Nagai et al 2007;Nelson et al 2012). The bias could be as high as 30% in case the temperature structure in the ICM is strongly inhomogeneous (Rasia et al 2006), although the mean temperature of local clusters was found to agree with the mass-weighted temperature (Frank et al 2013). The bias 1 − b = 0.72 +0.08 −0.07 recovered above is definitely on the high side of the expectations from numerical simulations.…”

Section: Comparison With Previous Measurementsmentioning

confidence: 73%

The XXL Survey

Eckert

Ettori

Coupon

et al. 2016

A&A

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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“…Frank et al 2013). Therefore, we have used a two-temperature thermal plasma model of collisional ionization emission (CIE).…”

Section: Spectral Modelingmentioning

confidence: 99%

Chemical Enrichment RGS cluster Sample (CHEERS): Constraints on turbulence

Pinto

Sanders

Werner

et al. 2015

A&A

121

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Context. Feedback from active galactic nuclei, galactic mergers, and sloshing are thought to give rise to turbulence, which may prevent cooling in clusters. Aims. We aim to measure the turbulence in clusters of galaxies and compare the measurements to some of their structural and evolutionary properties. Methods. It is possible to measure the turbulence of the hot gas in clusters by estimating the velocity widths of their X-ray emission lines. The Reflection Grating Spectrometers aboard XMM-Newton are currently the only instruments provided with sufficient effective area and spectral resolution in this energy domain. We benefited from excellent 1.6 Ms new data provided by the Chemical Enrichment RGS cluster Sample (CHEERS) project. Results. The new observations improve the quality of the archival data and allow us to place constraints for some clusters, which were not accessible in previous work. One-half of the sample shows upper limits on turbulence less than 500 km s −1 . For several sources, our data are consistent with relatively strong turbulence with upper limits on the velocity widths that are larger than 1000 km s −1 . The NGC 507 group of galaxies shows transonic velocities, which are most likely associated with the merging phenomena and bulk motions occurring in this object. Where both low-and high-ionization emission lines have good enough statistics, we find larger upper limits for the hot gas, which is partly due to the different spatial extents of the hot and cool gas phases. Our upper limits are larger than the Mach numbers required to balance cooling, suggesting that dissipation of turbulence may prevent cooling, although other heating processes could be dominant. The systematics associated with the spatial profile of the source continuum make this technique very challenging, though still powerful, for current instruments. In a forthcoming paper we will use the resonant-scattering technique to place lower-limits on the velocity broadening and provide further insights on turbulence. The ASTRO-H and Athena missions will revolutionize the velocity estimates and discriminate between different spatial regions and temperature phases.

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Characterization of Intracluster Medium Temperature Distributions of 62 Galaxy Clusters With XMM-Newton

Cited by 41 publications

References 97 publications

Physical properties of the X-ray gas as a dynamical diagnosis for galaxy clusters

Physical properties of the X-ray gas as a dynamical diagnosis for galaxy clusters

The XXL Survey

Chemical Enrichment RGS cluster Sample (CHEERS): Constraints on turbulence

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