  We present independent measurements of the masses of the galaxy clusters in
the local universe by employing the Dynamical Mass Estimator (DME) originally
developed by Falco et al in 2014. In the catalog of the galaxy groups/clusters
constructed by Tempel et al. from the Sloan Digital Sky Survey Data Release 10,
we search for those as the targets around which the neighbor galaxies
constitute thin straight filamentary structures in the configuration space
spanned by the redshifts and the projected distances. Out of the $29$ Sloan
clusters that have $100$ or more member galaxies, a total of six targets are
found to have filamentary structures in their bound zones. For each of the six
targets, we construct the profile of the recession velocities of the filament
galaxies, which depends on the cluster mass and the angle of the filament
relative the line of the sight direction. Fitting the constructed profile to
the universal formula with constant amplitude and slope, we statistically
determine the dynamical mass of each cluster and compare it with the previous
estimates made by a conventional method. The weak and strong points of the DME
as well as its prospect for the measurements of the dynamical masses of the
high-$z$ clusters are discussed.
