Dynamical modeling of the stellar nucleus of M 31

Abstract

We present stellar dynamical models of the lopsided, double-peaked nucleus of M 31, derived from Hubble Space Telescope (HST) photometry. A Schwarzschild-type method, in conjunction with Richardson-Lucy deconvolution, was employed to construct steadily rotating, hot, stellar disks. The stars orbit a massive dark object, on prograde and retrograde quasi-periodic loop orbits. Our results support Tremaine's eccentric disk model, extended to include a more massive disk, non zero pattern speed ( $\Omega$), and different viewing angle. Most of the disk mass populated prograde orbits, with $\simeq$3.4% on retrograde orbits. The best fits to photometric and kinematic maps were disks with $\Omega\simeq 16\mbox{\,km\, s${}^{-1}$\, pc${}^{-1}$ }$ . We speculate on the origins of the lopsidedness, invoking recent work on the linear overstability of nearly Keplerian disks, that possess even a small amount of a counter - rotating component. Accretion of material - no more massive than a globular cluster - onto a preexisting stellar disk, will account for the mass in our retrograde orbits, and could have stimulated the lopsidedness seen in the nucleus of M 31.