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Session 111 - Massive Black Holes and Dynamics of Galaxy Cores.
Oral session, Thursday, January 16
Harbour A,

[111.03] A Massive Black Hole in NGC 3379: 3-Integral Models

K. Gebhardt, D. Richstone (U. Michigan), J. Kormendy (U. Hawaii), R. Bender (Universitäts-Sternwarte, Munich), S. Faber (UCSC), T. Lauer (KPNO), J. Magorrian, S. Tremaine (CITA)

\def\MsunM_ødot \def\deg\ifmmode^\circ\else^\circ\fi \def\kmskm s^-1 \def\iei.e.

We fit axisymmetric, 3-integral models to NGC 3379 using HST/FOS observations of the galaxy center and ground-based spectroscopy along the major and minor axes. WFPC2 and ground-based images are used to constrain the light distribution. The models are fitted using maximum entropy. The data consists of two-dimensional coverage of the line-of-sight velocity distributions (LOSVD's), the maximum kinematic information obtainable. Models include inclinations from 27\deg\ (intrinsic galaxy type E6) to 90\deg\ (intrinsic E1), and black hole masses from 0 - 10^9\Msun.

The model with the minimum \chi^2 fit to the data has a black hole of 6\times 10^7\Msun and an inclination of 27\deg. The allowed range of black hole masses is from 4\times 10^7 to 1\times 10^8\Msun. Edge-on models (90\deg\ inclination) are not able to match the data. The intrinsic shape of the best fit model is an E6 galaxy. The internal velocity dispersions are not isotropic. The radial and the \phi dispersion profiles are similar; however, the \theta dispersion profile is about one half smaller at all radii. The internal rotation rises quickly at small radii due to the presence of the black hole.

Program listing for Thursday