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Date and Time of the Query: 2019-03-18 T14:32:31 PDT
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For refcode 2012MNRAS.419.2497B:
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Copyright by Royal Astronomical Society. 2012MNRAS.419.2497B On the correlations between galaxy properties and supermassive black hole mass Beifiori, A.; Courteau, S.; Corsini, E. M.; Zhu, Y. Abstract. We use a large sample of upper limits and accurate estimates of supermassive black hole (SMBH) masses coupled with libraries of host galaxy velocity dispersions, rotational velocities and photometric parameters extracted from Sloan Digital Sky Survey i-band images to establish correlations between the SMBH and host galaxy parameters. We test whether the mass of the black hole, M_blackhole_, is fundamentally driven by either local or global galaxy properties. We explore correlations between M_blackhole_ and stellar velocity dispersion {sigma}_e_, i-band bulge luminosity L_i, bulge_, bulge mass M_bulge_, bulge Sersic index n, bulge mean effective surface brightness <{mu}_e, bulge_>, i-band luminosity of the galaxy L_i, gal_, galaxy stellar mass M_*_._gal_, maximum circular velocity V_c_, and galaxy dynamical and effective masses M_dyn, gal_ and M_e, gal_. We verify the tightness of the M_blackhole_-{sigma}_e_ relation and find that correlations with other galaxy parameters do not yield tighter trends. We do not find differences in the M_blackhole_-{sigma}_e_ relation of barred and unbarred galaxies. The M_blackhole_-{sigma}_e_ relation of pseudo-bulges is also coarser and has a different slope than that involving classical bulges. The M_blackhole_-M_bulge_ is not as tight as the M_blackhole_-{sigma}_e_ relation, despite the bulge mass proving to be a better proxy of M_blackhole_ than bulge luminosity, and despite adding the bulge effective radius as an additional fitting parameter. Contrary to various published reports, we find a rather poor correlation between M_blackhole_ and n (or <{mu}_e, bulge_>), suggesting that M_blackhole_ is not related to the bulge light concentration. The correlations between M_blackhole_ and galaxy luminosity or mass are not a marked improvement over the M_blackhole_-{sigma}_e_ relation. These scaling relations depend sensitively on the host galaxy morphology: early-type galaxies follow a tighter relation than late-type galaxies. If V_c_ is a proxy for the dark matter halo mass, the large scatter of the M_blackhole_-V_c_ relation then suggests that M_blackhole_ is more coupled to the baryonic rather than the dark matter. We have tested the need for a third parameter in the M_blackhole_ scaling relations, through various linear correlations with bulge and galaxy parameters, only to confirm that the Fundamental Plane of the SMBH Is mainly driven by {sigma}_e_ with a small tilt due to the effective radius. We provide a compendium of galaxy structural properties for most of the SMBH hosts known to date. Key words: black hole physics, galaxies: fundamental parameters, galaxies: kinematics and dynamics, galaxies: photometry, galaxies: statistics
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