X-ray scaling relations for a representative sample of Planck selected clusters observed with XMM-Newton. (arXiv:2002.11740v1 [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:+Schellenberger_G/0/1/0/all/0/1">Gerrit Schellenberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sereno_M/0/1/0/all/0/1">Mauro Sereno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ettori_S/0/1/0/all/0/1">Stefano Ettori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pratt_G/0/1/0/all/0/1">Gabriel W. Pratt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Forman_W/0/1/0/all/0/1">William R. Forman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_C/0/1/0/all/0/1">Christine Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrade_Santos_F/0/1/0/all/0/1">Felipe Andrade-Santos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Randall_S/0/1/0/all/0/1">Scott Randall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraft_R/0/1/0/all/0/1">Ralph Kraft</a>
We report the scaling relations derived by fitting the X-ray parameters
determined from analyzing the XMM-Newton observations of 120 galaxy clusters in
the Planck Early Sunyaev-Zel’dovich sample spanning the redshift range of
0.059$<$$z$$<$0.546. We find that the slopes of all the investigated scaling
relations significantly deviate from the self-similar predictions, if
self-similar redshift evolution is assumed. When the redshift evolution is left
free to vary, the derived slopes are more in agreement with the self-similar
predictions. Relaxed clusters have on average $sim$30$%$ higher X-ray
luminosity than disturbed clusters at a given mass, a difference that,
depending on the relative fraction of relaxed and disturbed clusters in the
samples (e.g. SZ vs X-ray selected), have a strong impact in the normalization
obtained in different studies. Using the core-excised cluster luminosities
reduces the scatter and brings into better agreement the $L$-$M_{tot}$ and
$L$-$T$ relations determined for different samples. $M_{tot}$-$T$,
$M_{tot}$-$Y_X$, and $M_{tot}$-$M_{gas}$ relations show little dependence on
the dynamical state of the clusters, but the normalizations of these relations
may depend on the mass range investigated. Although most of the clusters
investigated in this work reside at relatively low redshift, the fits prefer
values of $gamma$, the parameter accounting for the redshift evolution,
different from the self-similar predictions. This suggests an evolution
($<$2$sigma$ level, with the exception of the $M_{tot}$-$T$ relation) of the
scaling relations. For the first time, we find significant evolution
($>$3$sigma$) of the $M_{tot}$-$T$ relation, pointing to an increase of the
kinetic-to-thermal energy ratio with redshift. This is consistent with a
scenario in which higher redshift clusters are on average more disturbed than
their lower redshift counterparts.
We report the scaling relations derived by fitting the X-ray parameters
determined from analyzing the XMM-Newton observations of 120 galaxy clusters in
the Planck Early Sunyaev-Zel’dovich sample spanning the redshift range of
0.059$<$$z$$<$0.546. We find that the slopes of all the investigated scaling
relations significantly deviate from the self-similar predictions, if
self-similar redshift evolution is assumed. When the redshift evolution is left
free to vary, the derived slopes are more in agreement with the self-similar
predictions. Relaxed clusters have on average $sim$30$%$ higher X-ray
luminosity than disturbed clusters at a given mass, a difference that,
depending on the relative fraction of relaxed and disturbed clusters in the
samples (e.g. SZ vs X-ray selected), have a strong impact in the normalization
obtained in different studies. Using the core-excised cluster luminosities
reduces the scatter and brings into better agreement the $L$-$M_{tot}$ and
$L$-$T$ relations determined for different samples. $M_{tot}$-$T$,
$M_{tot}$-$Y_X$, and $M_{tot}$-$M_{gas}$ relations show little dependence on
the dynamical state of the clusters, but the normalizations of these relations
may depend on the mass range investigated. Although most of the clusters
investigated in this work reside at relatively low redshift, the fits prefer
values of $gamma$, the parameter accounting for the redshift evolution,
different from the self-similar predictions. This suggests an evolution
($<$2$sigma$ level, with the exception of the $M_{tot}$-$T$ relation) of the
scaling relations. For the first time, we find significant evolution
($>$3$sigma$) of the $M_{tot}$-$T$ relation, pointing to an increase of the
kinetic-to-thermal energy ratio with redshift. This is consistent with a
scenario in which higher redshift clusters are on average more disturbed than
their lower redshift counterparts.
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