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|Title:||The X-Ray Halo Scaling Relations of Supermassive Black Holes||Authors:||GASPARI, MASSIMO
Johnson, S. D.
Tremblay, G. R.
Stone, J. M.
Yang, H.-Y. K.
|Issue Date:||2019||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||884||Issue:||2||First Page:||169||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, and masses) over galactic to cluster scales for 85 diverse systems. We find new key scalings, with the tightest relation being M_bh - T_x, followed by M_bh - L_x. 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 M_bh - σ_e) suggest that plasma halos play a more central role than stars in tracing and growing SMBHs (especially those that are ultramassive). Moreover, M_bh 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 the main departures from virialization/self-similarity via the optical/X-ray fundamental planes. We test the three major channels for SMBH growth: hot/Bondi-like models have inconsistent anticorrelation with X-ray halos and too low feeding; cosmological simulations find SMBH mergers as subdominant over most of cosmic time and too rare to induce a central-limit-theorem effect; the scalings are consistent with chaotic cold accretion, the rain of matter condensing out of the turbulent X-ray halos that sustains a long-term self-regulated feedback loop. The new correlations are major observational constraints for models of SMBH feeding/feedback in galaxies, groups, and clusters (e.g., to test cosmological hydrodynamical simulations), and enable the study of SMBHs not only through X-rays, but also via the Sunyaev-Zel’dovich effect (Compton parameter), lensing (total masses), and cosmology (gas fractions).||URI:||http://hdl.handle.net/20.500.12386/29221||URL:||https://iopscience.iop.org/article/10.3847/1538-4357/ab3c5d||ISSN:||0004-637X||DOI:||10.3847/1538-4357/ab3c5d||Bibcode ADS:||2019ApJ...884..169G||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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