2018MNRAS.475.1887Y -
Mon. Not. R. Astron. Soc., 475, 1887-1911 (2018/April-1)
Linking black hole growth with host galaxies: the accretion-stellar mass relation and its cosmic evolution.
YANG G., BRANDT W.N., VITO F., CHEN C.-T.J., TRUMP J.R., LUO B., SUN M.Y., XUE Y.Q., KOEKEMOER A.M., SCHNEIDER D.P., VIGNALI C. and WANG J.-X.
Abstract (from CDS):
Previous studies suggest that the growth of supermassive black holes (SMBHs) may be fundamentally related to host-galaxy stellar mass (M*). To investigate this SMBH growth-M* relation in detail, we calculate long-term SMBH accretion rate as a function of M* and redshift [(M*, z)] over ranges of log (M*/M☉) = 9.5-12 and z = 0.4-4. Our (M*, z) is constrained by high-quality survey data (GOODS-South, GOODS-North and COSMOS), and by the stellar mass function and the X-ray luminosity function. At a given M*, is higher at high redshift. This redshift dependence is stronger in more massive systems [for log (M*/M☉) ≃ 11.5, is three decades higher at z = 4 than at z = 0.5], possibly due to AGN feedback. Our results indicate that the ratio between and average star formation rate () rises towards high M* at a given redshift. This / dependence on M* does not support the scenario that SMBH and galaxy growth are in lockstep. We calculate SMBH mass history [MBH(z)] based on our (M*, z) and the M*(z) from the literature, and find that the MBH-M* relation has weak redshift evolution since z ≃ 2. The MBH/M* ratio is higher towards massive galaxies: it rises from ≃1/5000 at log M* <= 10.5 to ≃1/500 at log M* >= 11.2. Our predicted MBH/M* ratio at high M* is similar to that observed in local giant ellipticals, suggesting that SMBH growth from mergers is unlikely to dominate over growth from accretion.
Abstract Copyright:
© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Journal keyword(s):
galaxies: active - galaxies: evolution - galaxies: nuclei - X-rays: galaxies
Simbad objects:
8
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