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A list of selected globular clusters has been compiled for which measured tidal radii, luminosites, and distances seem currently most reliable. Using this material, an investigation is conducted of the distribution of cluster perigalactica on the basis of simple galactic mass models having either a logarithmic potential or a point-mass potential. The results give mean perigalactic distances too large to be consistent with published analyses of the cluster radial velocities. The most likely source of this systematic discrepancy appears to be an underestimate of the true cluster m/l ratio by a factor of 2-3, and possible observational errors in the measured tidal radii. It is also found that the observed dispersion of cluster densities at a given galactocentric distance is much smaller than that expected for an isotropic velocity dispersion, even though the observed dispersion is plainly generated mostly by random observational errors.
Innanen et al. (Tue,) studied this question.