The Non-Uniformity of Galaxy Cluster Metallicity Profiles. (arXiv:1811.05987v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lovisari_L/0/1/0/all/0/1">Lorenzo Lovisari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reiprich_T/0/1/0/all/0/1">Thomas Reiprich</a>
We study a sample of 207 nearby galaxy groups and clusters observed with
XMM-Newton. Key aspects of this sample include the large size, the high data
quality, and the large diversity of cluster dynamical states. We determine the
overall metallicity within 0.3R$_{500}$ and the radial distribution of the
metals. On average, we find a mild dependence of the core metallicity with the
average temperature of the system in agreement with previous results. However,
we identify the cause of this mild dependence to be due to relaxed systems
only; disturbed systems do not show this trend, on average. The large scatter
observed in this relation is strongly associated with the dynamical state of
the systems: relaxed systems have on average a higher metallicity in the core
than disturbed objects. The radial profiles of relaxed systems are centrally
peaked and show a steep decrease with radius, flattening beyond
0.3-0.4R$_{500}$. The metallicity of disturbed systems is also higher in the
center but at much lower values than what is observed for relaxed objects. This
finding is consistent with the picture that cluster mergers mix the abundance
distribution by inducing large scale motions. The scatter of the radial
profiles is quite large, but while for relaxed systems it decreases almost
monotonically as function of the radius, for disturbed systems it shows a
significant boost at large radii. Systems with a central radio source have a
flatter profile indicating that central AGNs are an efficient mechanism to
uplift and redistribute the metals in the ICM.
We study a sample of 207 nearby galaxy groups and clusters observed with
XMM-Newton. Key aspects of this sample include the large size, the high data
quality, and the large diversity of cluster dynamical states. We determine the
overall metallicity within 0.3R$_{500}$ and the radial distribution of the
metals. On average, we find a mild dependence of the core metallicity with the
average temperature of the system in agreement with previous results. However,
we identify the cause of this mild dependence to be due to relaxed systems
only; disturbed systems do not show this trend, on average. The large scatter
observed in this relation is strongly associated with the dynamical state of
the systems: relaxed systems have on average a higher metallicity in the core
than disturbed objects. The radial profiles of relaxed systems are centrally
peaked and show a steep decrease with radius, flattening beyond
0.3-0.4R$_{500}$. The metallicity of disturbed systems is also higher in the
center but at much lower values than what is observed for relaxed objects. This
finding is consistent with the picture that cluster mergers mix the abundance
distribution by inducing large scale motions. The scatter of the radial
profiles is quite large, but while for relaxed systems it decreases almost
monotonically as function of the radius, for disturbed systems it shows a
significant boost at large radii. Systems with a central radio source have a
flatter profile indicating that central AGNs are an efficient mechanism to
uplift and redistribute the metals in the ICM.
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