  The observed radial and transverse velocities of individual stars in M15 are
implemented as inputs to a fully non-parametric code (CHASSIS) in order to
estimate the equilibrium stellar distribution function and the
three-dimensional mass density profile. In particular, the paper explores the
possibility of the existence of a central black hole in M15 via several runs
that utilize the radial velocity data set which offers kinematic measurements
closer to the centre of the cluster than the proper motion data. These runs are
distinguished from each other in the choice of the initial seed for the cluster
characteristics; however, the profiles identified by the algorithm at the end
of each run concur with each other, within error bars, thus confirming the
robustness of CHASSIS. The recovered density profiles are noted to exhibit
unequivocal flattening, inner to about 0.0525pc. Also, the enclosed mass
profile is very close to being a power-law function of radius inside 0.1pc and
is not horizontal. Simplistically speaking, these trends negate the possibility
of the central mass to be concentrated in a black hole, the lower bound on the
radius of the sphere of influence of which would be $\gtrsim$0.041pc, had it
existed. However, proper analysis suggests that the mass enclosed within the
inner 0.01pc could be in the form of a black hole of mass
$\sim{10^3}$M$_{\odot}$, under two different scenarios, which are discussed.
The line-of-sight velocity dispersion is visually found to be very similar to
the observed dispersion profile. The enclosed mass and velocity dispersion
profiles calculated from runs done with the proper motion data are found to be
consistent with the profiles obtained with the radial velocity data.
