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Impact of magnetic field on the gas mass fraction of galaxy clusters
New Astronomy ( IF 2 ) Pub Date : 2021-04-01 , DOI: 10.1016/j.newast.2020.101531
Sandhya Jagannathan , Sunil Malik , Deepak Jain , T.R. Seshadri

Magnetic fields have been observed in galaxy clusters with strengths of the order of $\sim \mu$G. The non-thermal pressure exerted by magnetic fields also contributes to the total pressure in galaxy clusters and can in turn affect the estimates of the gas mass fraction, $f_{gas}$. In this paper, we have considered a central magnetic field strength of $5\mu$G, motivated by observations and simulations of galaxy clusters. The profile of the magnetic field has also been taken from the results obtained from simulations and observations. The role of magnetic field has been taken into account in inferring the gas density distribution through the hydrostatic equilibrium condition (HSE) by including the magnetic pressure. We have found that the resultant gas mass fraction is smaller with magnetic field as compared to that without magnetic field. However, this decrease is dependent on the strength and the profile of the magnetic field. We have also determined the total mass using the NFW profile to check for the dependency of $f_{gas}$ estimates on total mass estimators. From our analysis, we conclude that for the magnetic field strength that galaxy clusters seem to possess, the non-thermal pressure from magnetic fields has an impact of $\approx 1~\%$ on the gas mass fraction of galaxy clusters. However, with upcoming facilities like Square Kilometre Array (SKA), it can be further expected to improve with more precise observations of the magnetic field strength and profile in galaxy clusters, particularly in the interior region.

中文翻译:

磁场对星系团气体质量分数的影响

已经在星系团中观察到磁场强度约为 $\sim \mu$G。磁场施加的非热压力也会影响星系团的总压力,进而影响气体质量分数 $f_{gas}$ 的估计。在本文中,我们考虑了 $5\mu$G 的中心磁场强度,其动机是对星系团的观察和模拟。磁场的分布也取自模拟和观察获得的结果。在通过流体静力平衡条件 (HSE) 通过包括磁压力推断气体密度分布时,已考虑到磁场的作用。我们发现,与没有磁场的情况相比,有磁场的合成气体质量分数更小。然而,这种减少取决于磁场的强度和分布。我们还使用 NFW 配置文件确定了总质量,以检查 $f_{gas}$ 估计值对总质量估计值的依赖性。根据我们的分析,我们得出结论,对于星系团似乎具有的磁场强度,来自磁场的非热压力对星系团的气体质量分数有$\approx 1~\%$的影响。然而,随着即将到来的设施,如平方公里阵列(SKA),可以通过更精确地观测星系团,特别是内部区域的磁场强度和轮廓,进一步改进。我们还使用 NFW 配置文件确定了总质量,以检查 $f_{gas}$ 估计值对总质量估计值的依赖性。根据我们的分析,我们得出结论,对于星系团似乎具有的磁场强度,来自磁场的非热压力对星系团的气体质量分数有$\approx 1~\%$的影响。然而,随着即将到来的设施,如平方公里阵列(SKA),可以通过更精确地观测星系团,特别是内部区域的磁场强度和轮廓,进一步改进。我们还使用 NFW 配置文件确定了总质量,以检查 $f_{gas}$ 估计值对总质量估计值的依赖性。根据我们的分析,我们得出结论,对于星系团似乎具有的磁场强度,来自磁场的非热压力对星系团的气体质量分数有$\approx 1~\%$的影响。然而,随着即将到来的设施,如平方公里阵列(SKA),可以通过更精确地观测星系团,特别是内部区域的磁场强度和轮廓,进一步改进。磁场的非热压对星系团的气体质量分数有$\approx 1~\%$的影响。然而,随着即将到来的设施,如平方公里阵列(SKA),可以通过更精确地观测星系团,特别是内部区域的磁场强度和轮廓,进一步改进。来自磁场的非热压对星系团的气体质量分数有$\approx 1~\%$的影响。然而,随着即将到来的设施,如平方公里阵列(SKA),可以通过更精确地观测星系团,特别是内部区域的磁场强度和轮廓,进一步改进。
更新日期:2021-04-01
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