NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-16 T12:05:33 PDT
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For refcode 2006MNRAS.368.1395M:
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NED Abstract

Copyright by Royal Astronomical Society. 2006MNRAS.368.1395M On the evolution of the black hole: spheroid mass ratio McLure, R. J., Jarvis, M. J., Targett, T. A., Dunlop, J. S.; Best, P. N. We present the results of a study which uses the 3C RR sample of radio-loud active galactic nuclei to investigate the evolution of the black hole:spheroid mass ratio in the most massive early-type galaxies from 0 <z< 2. Radio-loud unification is exploited to obtain virial (linewidth) black hole mass estimates from the 3C RR quasars, and stellar mass estimates from the 3C RR radio galaxies, thereby providing black hole and stellar mass estimates for a single population of early-type galaxies. At low redshift (z 1), the 3C RR sample is consistent with a black hole:spheroid mass ratio of M_bh_/M_sph_ 0.002, in good agreement with that observed locally for quiescent galaxies of similar stellar mass (M_sph_ 5 x 10^11^ M). However, over the redshift interval 0 <z< 2 the 3C RR black hole:spheroid mass ratio is found to evolve as M_bh_/M_sph_ (1 +z)^2.07 +/- 0.76^, reaching M_bh_/M_sph_ 0.008 by redshift z ~- 2. This evolution is found to be inconsistent with the local black hole:spheroid mass ratio remaining constant at a moderately significant level (98 per cent). If confirmed, the detection of evolution in the 3C RR black hole:spheroid mass ratio further strengthens the evidence that, at least for massive early-type galaxies, the growth of the central supermassive black hole may be completed before that of the host spheroid. Key words: black hole physics: galaxies: active: galaxies: nuclei: quasars: general
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