On two mass estimators for clusters of galaxies

The two most common mass estimators that use velocity dispersions and posit ions of objects in a stellar system, the virial mass estimator (VME) and th e projected mass estimator (PME), are revisited and tested using N-body exp eriments. We consider here only spherical, isolated, and isotropic velocity dispersion systems. We have found that the PME can overestimate masses by approximate to 20%, f or realistic cluster mass profiles, if applied only to regions around the t otal system's effective radius. The VME can yield a correct mass at differe nt radii provided that the potential energy term is correctly taken into ac count and the system is completely sampled; otherwise, it may lead to simil ar errors as the PME. A surface pressure (3PV) term recently alluded to be usually neglected when using the VME and therefore required as a correction term is here found no t necessarily required, although it can be used to yield a reasonable corre ction term. The preferred method here, however, is the virial theorem due t o its simplicity and better agreement with N-body experiments. The possible reasons for the mass discrepancies found when using the PME and the VME in some N-body simulations are also briefly discussed.