The X-ray Halo Scaling Relations of Supermassive Black Holes
M. Gaspari, D. Eckert, S. Ettori, P. Tozzi, L. Bassini, E. Rasia, F., Brighenti, M. Sun, S. Borgani, S. D. Johnson, G. R. Tremblay, J. M. Stone, P., Temi, H.-Y. K. Yang, F. Tombesi, M. Cappi
TL;DR
This study reveals new tight correlations between supermassive black hole masses and X-ray plasma properties of hot halos, emphasizing the importance of plasma halos over stars in SMBH growth and providing key constraints for theoretical models.
Contribution
It introduces novel, tightly correlated X-ray halo scaling relations with SMBH masses, highlighting the role of hot plasma in SMBH growth and feedback mechanisms.
Findings
$M_ullet-T_{ m x}$ relation is the tightest correlation.
X-ray halo scalings have less scatter than optical counterparts.
Chaotic cold accretion explains the observed scalings.
Abstract
We carry out a comprehensive Bayesian correlation analysis between hot halos and direct masses of supermassive black holes (SMBHs), by retrieving the X-ray plasma properties (temperature, luminosity, density, pressure, masses) over galactic to cluster scales for 85 diverse systems. We find new key scalings, with the tightest relation being the , followed by . The tighter scatter (down to 0.2 dex) and stronger correlation coefficient of all the X-ray halo scalings compared with the optical counterparts (as the ) suggest that plasma halos play a more central role than stars in tracing and growing SMBHs (especially those that are ultramassive). Moreover, correlates better with the gas mass than dark matter mass. We show the important role of the environment, morphology, and relic galaxies/coronae, as well as…
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