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A Fundamental Plane Relation for Black Hole Masses and their Redshift Evolution | | Philip F. Hopkins
; Lars Hernquist
; Thomas J. Cox
; Brant Robertson
; Elisabeth Krause
; | | Date: |
11 Jan 2007 | | Abstract: | We study the relation between black hole (BH) mass and host galaxy properties in simulations of major galaxy mergers. We show that the simulations predict the existence of a BH fundamental plane (BHFP), of the form M_BH ~ sigma^3 R_e^0.5 (~ M_stellar^0.5 sigma^2), analogous to the FP of ellipticals. Comparing with existing BH measurements, observed systems indeed follow an identical BHFP relation, favoring such a BHFP over a simple relation between M_BH and any of sigma, M_stellar, M_dyn, or R_e alone at >99.9% significance. This can be roughly understood as a ’tilted’ correlation between BH mass and spheroid binding energy, or from the condition for feedback to power a pressure-driven outflow. While changes in halo circular velocity, merger orbital parameters, progenitor disk redshifts and gas fractions, ISM gas pressurization, and other parameters can drive changes in e.g. sigma at fixed M_stellar, and therefore changes in the M_BH-sigma or M_BH-M_stellar relations, the BHFP is robust. Given the empirical trend of decreasing R_e at fixed stellar mass at high redshift, the BHFP predicts BHs will be more massive at fixed M_stellar, in agreement with recent observations. This evolution is driven by the fact that disks (merger progenitors) have larger gas fractions at high redshifts. Adopting the observed evolution of disk f_gas with redshift, our simulations predict the observed trends in both R_e(M_stellar) and M_BH(M_stellar). We discuss the implications of this BHFP for the masses of the largest BHs and apparent ’outliers’ in the M_BH-sigma and M_BH-M_stellar relations. | | Source: | arXiv, astro-ph/0701351 | | Services: | Forum | Review | PDF | Favorites | |
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