NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-03-20 T14:17:07 PDT
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For refcode 2008MNRAS.386.2242H:
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Copyright by Royal Astronomical Society. 2008MNRAS.386.2242H The black hole mass-stellar velocity dispersion correlation: bulges versus pseudo-bulges Jian Hu Abstract. We investigate the correlation between the supermassive black holes (SMBHs) mass (M_bh_) and the stellar velocity dispersion ({sigma}_*_) in two types of host galaxies: the early-type bulges (disc galaxies with classical bulges or elliptical galaxies) and pseudo-bulges. In the form log (M_bh_/M_sun_) = {alpha} + {beta} log ({sigma}_*_/200 km s^-1^), the best-fitting results for the 39 early-type bulges are the slope {beta} = 4.06 +/- 0.28 and the normalization {alpha} = 8.28 +/- 0.05; the best-fitting results for the nine pseudo-bulges are {beta} = 4.5 +/- 1.3 and {alpha} = 7.50 +/- 0.18. Both relations have intrinsic scatter in log M_bh_ of ~<0.27 dex. The M_bh_-{sigma}_*_ relation for pseudo-bulges is different from the relation in the early-type bulges over the 3{sigma} significance level. The contrasting relations indicate the formation and growth histories of SMBHs depend on their host type. The discrepancy between the slope of the M_bh_-{sigma}_*_ relations using different definition of velocity dispersion vanishes in our sample, a uniform slope will constrain the coevolution theories of the SMBHs and their host galaxies more effectively. We also find the slope for the 'core' elliptical galaxies at the high-mass range of the relation appears steeper ({beta} ~= 5-6), which may be the imprint of their origin of dissipationless mergers. Key words: black hole physics, galaxies: bulges, galaxies: formation, galaxies: fundamental parameters, galaxies: nuclei
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