The Local Black Hole Mass Function Derived from the MBH-Pitch Angle and the MBH-Sersic Index Relations
We determined the local supermassive black hole mass function (BHMF) for all galaxy types with complementing the local BHMF for spiral galaxies derived by Davis et al. (2014). We used the empirical relation between supermassive black hole mass and the Sersic index for early type (E/S0) galaxies from the same parent sample with Davis et al. (2014), which is selected from galaxies in the Carnegie-Irvine Galaxy Survey (CGS) which is a very complete sample of the nearby galaxies.The observational simplicity of our approach and direct measurements from the statistically tightest correlations with black hole mass, which are the Sersic index for E/S0 galaxies and pitch angle for spiral galaxies, make it straightforward to estimate an accurate local BHMF. Integrating over the best-fitting mass function, the local mass density of SMBHs from early- and late-type galaxies combined is ρ=3.61+3.80-1.75 x105 M☉ Mpc-3. The errors are estimated from Monte Carlo simulations which include uncertainities in the emprical relations and measurement errors in both Sersic index and Pitch angle. Assuming supermassive black holes form via baryonic accretion, we find that 0.013+0.013-0.006 per cent of baryons are contained in SMBHs at the centers of galaxies in the local universe.
American Astronomical Society Meeting Abstracts #227
- Pub Date:
- January 2016