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NGC 4993 hosts a binary neutron star merger emitting gravitational waves andelectromagnetic waves, GW170817/GRB 170817A. The distance to this galaxy is notwell established. We select the globular cluster candidates from the HubbleSpace Telescope/ACS F606W images of NGC 4993 in the archive, using thestructural parameters of the detected sources. The radial number densitydistribution of these candidates shows a significant central concentrationaround the galaxy center at the galactocentric distance $r<50''$, showing thatthey are mostly the members of NGC 4993. Also the luminosity function of thesecandidates is fit well by a Gaussian function. Therefore the selectedcandidates at $r<50''$ are mostly considered to be globular clusters in NGC4993. We derive an extinction-corrected turnover Vega magnitude in theluminosity function of the globular clusters at $20''<r<50''$, F606W (max)$_0=25.36\pm0.08$ ($V_0 =25.52\pm0.11$)} mag. Adopting the calibration of theturnover magnitudes of the globular clusters, $M_V({\rm max})=-7.58\pm0.11$, wederive a distance to NGC 4993, $d=41.65\pm3.00$ Mpc ($(m-M)_0=33.10\pm0.16$).The systematic error of this method can be as large as $\pm0.3$ mag. This valueis consistent with the previous distance estimates based on the fundamentalplane relation and the gravitational wave method in the literature. Thedistance in this study can be used to constrain the values of the parametersincluding the inclination angle of the binary system in the models ofgravitational wave analysis.

A Globular Cluster Luminosity Function Distance to NGC 4993 Hosting a Binary Neutron Star Merger GW170817/GRB 170817A