  We use recently published measurements of the kinematics, surface brightness
and stellar mass-to-light ratio of the globular cluster NGC 2419 to examine the
possibility that this Galactic halo satellite is embedded in a low-mass dark
matter halo. NGC 2419 is a promising target for such a study, since its extreme
Galactocentric distance and large mass would have greatly facilitated the
retention of dark matter. A Markov-Chain Monte Carlo approach is used to
investigate composite dynamical models containing a stellar and a dark matter
component. We find that it is unlikely that a significant amount of dark matter
(less than approx. 6% of the luminous mass inside the tidal limit of the
cluster) can be present if the stars follow an anisotropic Michie model and the
dark matter a double power law model. However, we find that more general
models, derived using a new technique we have developed to compute
non-parametric solutions to the spherical Jeans equation, suggest the presence
of a significant dark matter fraction (approximately twice the stellar mass).
Thus the presence of a dark matter halo around NGC 2419 cannot be fully ruled
out at present, yet any dark matter within the 10 arcmin visible extent of the
cluster must be highly concentrated and cannot exceed 1.1x10^6 Solar masses
(99% confidence), in stark contrast to expectations for a plausible progenitor
halo of this structure.
