The X-ray Halo Scaling Relations of Supermassive Black Holes. (arXiv:1904.10972v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gaspari_M/0/1/0/all/0/1">M. Gaspari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eckert_D/0/1/0/all/0/1">D. Eckert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ettori_S/0/1/0/all/0/1">S. Ettori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tozzi_P/0/1/0/all/0/1">P. Tozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bassini_L/0/1/0/all/0/1">L. Bassini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rasia_E/0/1/0/all/0/1">E. Rasia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brighenti_F/0/1/0/all/0/1">F. Brighenti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_M/0/1/0/all/0/1">M. Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borgani_S/0/1/0/all/0/1">S. Borgani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_S/0/1/0/all/0/1">S. D. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tremblay_G/0/1/0/all/0/1">G. Tremblay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_J/0/1/0/all/0/1">J. Stone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Temi_P/0/1/0/all/0/1">P. Temi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_H/0/1/0/all/0/1">H.-Y. K. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tombesi_F/0/1/0/all/0/1">F. Tombesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cappi_M/0/1/0/all/0/1">M. Cappi</a>
We study the correlations between (direct) masses of supermassive black holes
(SMBHs) and X-ray hot halo properties, by using a Bayesian analysis of archival
datasets and theoretical models. We analyze fundamental and composite X-ray
variables (plasma temperature, luminosity, density, pressure, and gas/total
masses) from galactic to cluster scales. We show novel key scalings, with the
tightest relation being the $M_bullet – T_{rm x}$, followed by $M_bullet –
L_{rm x}$ (scatter 0.2-0.3 dex). The tighter scatter and larger correlation
coefficient of the X-ray halo scalings compared with the optical counterparts
(including the $M_bullet-sigma_ast$), together with the multivariate
analysis, suggest that the plasma atmospheres play a more central role than the
stellar component in the growth of SMBHs (and ultramassive BHs), in particular
accounting for the group/cluster core halo. The derived gas mass scalings also
correlate better with $M_bullet$ than dark matter mass. We provide key
insights on environmental features, relic galaxies, and coronae. The comparison
of the optical and X-ray fundamental planes shows that, while stars can be
described mainly via the virial theorem, X-ray halos are better described by
univariate scalings with deviations from self-similar collapse due to feedback
processes. We test 3 major channels for BH growth: hot gas accretion, chaotic
cold accretion (CCA), and hierarchical BH mergers. Hot/Bondi-like models are
ruled out by the data, showing inconsistent anti-correlation with X-ray halos
and too low feeding. Cosmological simulations show that binary SMBH mergers are
a sub-dominant channel over most of the cosmic time and too rare to induce a
central-limit-theorem effect. The scalings are consistent with the predictions
of CCA, the rain of matter condensing out of the turbulent X-ray halos,
sustaining a self-regulated feedback loop throughout cosmic time.
We study the correlations between (direct) masses of supermassive black holes
(SMBHs) and X-ray hot halo properties, by using a Bayesian analysis of archival
datasets and theoretical models. We analyze fundamental and composite X-ray
variables (plasma temperature, luminosity, density, pressure, and gas/total
masses) from galactic to cluster scales. We show novel key scalings, with the
tightest relation being the $M_bullet – T_{rm x}$, followed by $M_bullet –
L_{rm x}$ (scatter 0.2-0.3 dex). The tighter scatter and larger correlation
coefficient of the X-ray halo scalings compared with the optical counterparts
(including the $M_bullet-sigma_ast$), together with the multivariate
analysis, suggest that the plasma atmospheres play a more central role than the
stellar component in the growth of SMBHs (and ultramassive BHs), in particular
accounting for the group/cluster core halo. The derived gas mass scalings also
correlate better with $M_bullet$ than dark matter mass. We provide key
insights on environmental features, relic galaxies, and coronae. The comparison
of the optical and X-ray fundamental planes shows that, while stars can be
described mainly via the virial theorem, X-ray halos are better described by
univariate scalings with deviations from self-similar collapse due to feedback
processes. We test 3 major channels for BH growth: hot gas accretion, chaotic
cold accretion (CCA), and hierarchical BH mergers. Hot/Bondi-like models are
ruled out by the data, showing inconsistent anti-correlation with X-ray halos
and too low feeding. Cosmological simulations show that binary SMBH mergers are
a sub-dominant channel over most of the cosmic time and too rare to induce a
central-limit-theorem effect. The scalings are consistent with the predictions
of CCA, the rain of matter condensing out of the turbulent X-ray halos,
sustaining a self-regulated feedback loop throughout cosmic time.
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