We used a large sample of upper limits and accurate estimates of supermassive black holes (SBHs) masses coupled with libraries of kinematic parameters (derived from literature) and photometric parameters (extracted from Sloan Digital Sky Survey i-band images) to establish correlations between the SBH and host galaxy properties. We tested if the SBH mass M_BH is fundamentally driven by either bulge or galaxy properties. We explored for correlations between M_BH and stellar velocity dispersion sigma, bulge luminosity L_bulge, bulge mass M_bulge, Sérsic index n and concentration of the bulge, galaxy luminosity L_gal, circular velocity V_c, galaxy stellar mass M_star,gal, virial mass M_e, gal, and dynamical mass M_dyn, gal. We verified the tightness of the M_BH-sigma relation and found that correlations with other galaxy parameters do not yield tighter trends. We confirmed that the fundamental plane of the SBH is mainly driven by sigma, with a small tilt being due to the effective radius, r_e.

On the correlations between bulge/galaxy properties and supermassive black hole mass

CORSINI, ENRICO MARIA;
2012

Abstract

We used a large sample of upper limits and accurate estimates of supermassive black holes (SBHs) masses coupled with libraries of kinematic parameters (derived from literature) and photometric parameters (extracted from Sloan Digital Sky Survey i-band images) to establish correlations between the SBH and host galaxy properties. We tested if the SBH mass M_BH is fundamentally driven by either bulge or galaxy properties. We explored for correlations between M_BH and stellar velocity dispersion sigma, bulge luminosity L_bulge, bulge mass M_bulge, Sérsic index n and concentration of the bulge, galaxy luminosity L_gal, circular velocity V_c, galaxy stellar mass M_star,gal, virial mass M_e, gal, and dynamical mass M_dyn, gal. We verified the tightness of the M_BH-sigma relation and found that correlations with other galaxy parameters do not yield tighter trends. We confirmed that the fundamental plane of the SBH is mainly driven by sigma, with a small tilt being due to the effective radius, r_e.
2012
54th MEETING OF THE ITALIAN ASTRONOMICAL SOCIETY. ITALIAN ASTRONOMY: PERSPECTIVES FOR THE NEXT DECADE
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11577/2527072
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