  We perform a combined analysis of stellar kinematics and line-of-sight
accelerations of millisecond pulsars to investigate the mass contents of Omega
Centauri. We consider multiple mass components: the visible photometric
distribution, a central cluster of dark remnants, an intermediate-mass black
hole, and a distribution of intermediate extension traced by the pulsars. By
self-consistently incorporating multiple independent datasets, including the
effects of different centers, we obtain significant constraints on these mass
distributions. Our results strongly favor an extended central mass of ~ 2 - 3 x
10^5 Msun, emulating a cluster of heavy stellar remnants, over an IMBH, with a
3-sigma upper limit of 6 x 10^3 Msun on its mass. Pulsar timing observations
provide significant constraints, favoring a central mass distribution that is ~
20% more massive and extended. Notably, we observe a clear linear scaling
between the pulsar distribution and stellar encounter rates, showing excellent
agreement with the expectation from millisecond pulsar formation models and
motivating a profile for their distribution, providing the first validation of
its kind where positions are linked to their place of formation in globular
clusters. Our findings highlight the effectiveness of this novel methodology in
exploring the structure of star clusters, setting a promising precedent amid
the advent of the rapidly growing number of observations and discoveries
currently being experienced in this field.
