We extract the shape of the stellar velocity ellipsoid as a function of radius in M87 from van der Marel’s (1994) velocity dispersion data. We include the gravitational force of a central black hole with the mass quoted by Harms et al. (1994). The kinematical data are corrected for the effects of seeing and instrumental blurring using a nonparametric algorithm. We find that the stellar motions in M87 are slightly radially anisotropic throughout the main body of the galaxy, with σr 1.2σt. However σt exceeds σr within the inner 1′′ − 2′′ by a statistically significant amount. A number of models for the formation of nuclear black holes predict a tangential anisotropy in the stellar motions, and our results provide evidence for such an effect in M87. (Refer to PDF file for exact formulas).

Publication Date



Archived in: arXiv:astro-ph/9610112 v1 15 Oct 1996 AND Rutgers Astrophysics Preprint Series No. 195 This work was supported by NSF grant AST 90-16515 and NASA grant NAG 5-2803 to DM.ISSN:1538-3881 Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type


Department, Program, or Center

School of Physics and Astronomy (COS)


RIT – Main Campus