Modeling the Eccentric Nuclear Disk in M31 to Obtain the Mass of the Central Black Hole

Details Modeling the Eccentric Nuclear Disk in M31 to Obtain the Mass of the Central Black Hole Modeling the Eccentric Nuclear Disk in M31 to Obtain the Mass of the Central Black Hole

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.6803s&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #68.03; Bulletin of the American Astronomical Society, Vol. 34, p.1219

Astronomy and Astrophysics

Astronomy

Scientific paper

The off-center brightness peak in the nucleus of M31, along with asymmetries in the nuclear kinematic and photometric profiles, suggests the presence of an underlying eccentric disk of stars orbiting a supermassive black hole. I have developed a method for constructing approximate self-consistent models of weakly self-gravitating, finite dispersion eccentric stellar disks around central black holes. The disks are fixed in a frame rotating at a constant precession speed, and are built by an iteration scheme in which the disk is populated by quasi-periodic orbits using a distribution function written in terms of the Kepler integrals of motion. I will present results from a grid of models computed to constrain the mass of the black hole in M31. In particular, a statistically valid black hole mass will be given, and the properties of the disk that best-fits the most recent high-resolution nuclear observations will be discussed. I have also developed an n-body code which is well suited for stability studies of disk systems with high-eccentricity orbits. Preliminary results on the stability of a particle realization of the best-fit model will be presented. This research was supported by NSF CAREER grant AST 97-03036

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