  I re-examine mass estimates of the Coma cluster from pre-ASCA X-ray spectral
observations. A large range of model dark matter distributions are examined,
under the assumptions of hydrostatic equilibrium and spherical symmetry, to
determine the widest possible allowed range on the total mass of the cluster.
Within a radius of 1 Mpc, the total cluster mass is tightly constrained to be
(6.2 +/- 0.9) x 10**14 solar masses and the ratio of luminous baryonic matter
to total matter lies between 13% and 17%. Within a radius of 3 Mpc the total
mass is (1.3 +/- 0.5) x 10**15 solar masses and the luminous matter fraction is
20%-40%. I find that the ``universal'' dark matter density profile proposed by
Navarro, Frenk, and White, based on N-body simulations of a standard
cold-dark-matter dominated Universe, predicts a steep temperature gradient
within the core of the cluster that is a poor fit to the Coma data and can be
rejected at greater than 99% confidence.
