Deriving the mass distribution of M87 from globular clusters

Abstract

We describe a maximum-likelihood method for determining the mass distribution in spherical stellar systems from the radial velocities of a population of discrete test particles. The method assumes a parametric form for the mass distribution and a non-parametric two-integral distribution function. We apply the method to a sample of 161 globular clusters in M87. We find that the mass within 32 kpc is $(2.4\pm 0.6)\times 10^{12}$M${}_{\odot }$, and the exponent of the density profile $\rho \propto r^{-\alpha }$ in the range 10-100 kpc is $\alpha =1.6\pm 0.4$.The energy distribution suggests a few kinematically distinct groups of globular clusters. The anisotropy of the globular-cluster velocity distribution cannot be determined reliably with the present data. Models fitted to an NFW potential yield similar mass estimates but cannot constrain the concentration radius $r_c$ in the range 10-500 kpc.

arXiv comment32 pages, 12 figures, accepted to publish in ApJ

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