UNBIASED CORRECTION RELATIONS FOR GALAXY CLUSTER PROPERTIES DERIVED FROM<i>CHANDRA</i>AND<i>XMM-NEWTON</i>

Zhao, Huabiao; Li, Cheng-Kui; Chen, Yong; Jia, S.; Song, Liming

doi:10.1088/0004-637x/799/1/47

Cited by 5 publications

(1 citation statement)

References 38 publications

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“…The temperatures measured with Chandra are systematically higher than those measured with XMM-Newton. This trend is consistent with the relation revealed by previous studies (Schellenberger et al 2015;Zhao et al 2015).…”

Section: Spectral Fittingsupporting

confidence: 93%

Weak Merging Scenario of CLASH Cluster A209

Feng,

Yu,

Zhao

et al. 2024

Res. Astron. Astrophys.

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We study the structural and dynamical properties of Abell 209 based on Chandra and XMM-Newton observations. We obtain detailed temperature, pressure and entropy maps with the contour binning method, and find a hot region in the NW direction. The X-ray brightness residual map and corresponding temperature profiles reveal a possible shock front in the NW direction and a cold front feature in the SE direction. Combing with the galaxy luminosity density map we propose a weak merger scenario. A young sub-cluster passing from the SE to NW direction could explain the optical subpeak, the ICM temperature map, the X-ray surface brightness excess, and the X-ray peak offset togethe.

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Section: Spectral Fittingsupporting

confidence: 93%

Weak Merging Scenario of CLASH Cluster A209

Feng,

Yu,

Zhao

et al. 2024

Res. Astron. Astrophys.

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The Scaling Relations and the Fundamental Plane for Radio Halos and Relics of Galaxy Clusters

Yuan

Han

Wen

2015

ApJ

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Diffuse radio emission in galaxy clusters is known to be related to cluster mass and cluster dynamical state. We collect the observed fluxes of radio halos, relics, and mini-halos for a sample of galaxy clusters from the literature, and calculate their radio powers. We then obtain the values of cluster mass or mass proxies from previous observations, and also obtain the various dynamical parameters of these galaxy clusters from optical and X-ray data. The radio powers of relics, halos, and mini-halos are correlated with the cluster masses or mass proxies, as found by previous authors, with the correlations concerning giant radio halos being, in general, the strongest ones. We found that the inclusion of dynamical parameters as the third dimension can significantly reduce the data scatter for the scaling relations, especially for radio halos. We therefore conclude that the substructures in X-ray images of galaxy clusters and the irregular distributions of optical brightness of member galaxies can be used to quantitatively characterize the shock waves and turbulence in the intracluster medium responsible for re-accelerating particles to generate the observed diffuse radio emission. The power of radio halos and relics is correlated with cluster mass proxies and dynamical parameters in the form of a fundamental plane.

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The Y_SZ,Planck – Y_SZ,XMM scaling relation and its difference between cool-core and non-cool-core clusters

Zhu

Wang

Zhao

et al. 2019

Res. Astron. Astrophys.

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We construct a sample of 70 clusters using data from XMM-Newton and Planck to investigate the Y SZ,Planck − Y SZ,XMM scaling relation and the cool-core influences on the relation. Y SZ,XMM is calculated by accurate de-projected temperature and electron number density profiles derived from XMM-Newton. Y SZ,Planck is the latest Planck data restricted to our precise X-ray size θ 500 . To study the cool-core influences on Y SZ,Planck − Y SZ,XMM scaling relation, we apply two criteria, limits of central cooling time and classic mass deposition rate, to distinguish cool-core clusters (CCCs) from non-cool-core clusters (NCCCs). We also use Y SZ,Planck from other papers, which are derived from different methods, to confirm our results. The intercept and slope of the Y SZ,Planck − Y SZ,XMM scaling relation are A = −0.86 ± 0.30, B = 0.83 ± 0.06. The intrinsic scatter is σ ins = 0.14 ± 0.03. The ratio of Y SZ,Planck /Y SZ,XMM is 1.03 ± 0.05, which is perfectly agreed with unity. Discrepancies of Y SZ,Planck − Y SZ,XMM scaling relation between CCCs and NCCCs are found in observation. They are independent of cool-core classification criteria and Y SZ,Planck calculation methods, although discrepancies are more significant under the classification criteria of classic mass deposition rate. The intrinsic scatter of CCCs (0.04) is quite small compared to that of NCCCs (0.27). The ratio of Y SZ,Planck /Y SZ,XMM for CCCs is 0.89 ± 0.05, suggesting that CCCs' Y SZ,XMM may overestimate SZ signal. By contrast, the ratio of Y SZ,Planck /Y SZ,XMM for NCCCs is 1.14 ± 0.12, which indicates that NCCCs' Y SZ,XMM may underestimate SZ signal.

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UNBIASED CORRECTION RELATIONS FOR GALAXY CLUSTER PROPERTIES DERIVED FROMCHANDRAANDXMM-NEWTON

Cited by 5 publications

References 38 publications

Weak Merging Scenario of CLASH Cluster A209

Weak Merging Scenario of CLASH Cluster A209

The Scaling Relations and the Fundamental Plane for Radio Halos and Relics of Galaxy Clusters

The Y_SZ,Planck – Y_SZ,XMM scaling relation and its difference between cool-core and non-cool-core clusters

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UNBIASED CORRECTION RELATIONS FOR GALAXY CLUSTER PROPERTIES DERIVED FROMCHANDRAANDXMM-NEWTON

Cited by 5 publications

References 38 publications

Weak Merging Scenario of CLASH Cluster A209

Weak Merging Scenario of CLASH Cluster A209

The Scaling Relations and the Fundamental Plane for Radio Halos and Relics of Galaxy Clusters

The YSZ,Planck – YSZ,XMM scaling relation and its difference between cool-core and non-cool-core clusters

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The Y_SZ,Planck – Y_SZ,XMM scaling relation and its difference between cool-core and non-cool-core clusters