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The radial velocities of the galaxies in the vicinity of a cluster showsdeviation from the pure Hubble flow due to their gravitational interaction withthe cluster. According to a recent study of Falco et al. (2014) based on ahigh-resolution N-body simulation, the radial velocity profile of the galaxieslocated at distances larger than three times the virial radius of a neighborcluster can be well approximated by a universal formula and could bereconstructed from direct observables provided that the galaxies aredistributed along one dimensional filament. They suggested an algorithm for theestimation of the dynamic mass of a cluster $M_{\rm v}$ by fitting theuniversal formula from the simulation to the reconstructed radial velocityprofile of the filament galaxies around the cluster from observations. We applythe algorithm to two narrow straight filaments (called the Filament A and B)that were identified recently by Kim et al. (2015) in the vicinity of the Virgocluster from the NASA-Sloan-Atlas catalog. The dynamical mass of the Virgocluster is estimated to be $M_{\rmv}=(0.84^{+2.75}_{-0.51})\times10^{15}\,h^{-1}M_{\odot}$ and $M_{\rm v}=(3.24^{+4.99}_{-1.31})\times 10^{15}\,h^{-1}M_{\odot}$ for the cases of theFilament A and B, respectively. We discuss observational and theoreticalsystematics intrinsic to the method of Falco et al. (2014) as well as thephysical implication of the final results.

A New Dynamical Mass Measurement for the Virgo Cluster using the Radial Velocity Profile of the Filament Galaxies