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Millisecond pulsars can serve as effective probes to investigate the presenceof Intermediate-mass Black Holes (IMBHs) within Galactic globular clusters(GCs). Based on the standard structure models for GCs, we conduct simulationsto analyze the distributions of pulsar accelerations within the central regionof NGC 6517. By comparing the measured accelerations of pulsars obtained fromtheir period derivatives $\dot P$ to the simulated distribution profiles, wedemonstrate that a central excess of dark mass is required to account for themeasured accelerations. Our analysis, which relies on existing pulsar timingobservations, is currently unable to differentiate between two possiblescenarios: an IMBH precisely situated at the core of the cluster with mass$\gtrsim 9000^{+4000}_{-3000}~M_{\odot}$, or a central concentration of stellarmass dark remnants with a comparable total mass. However, with additionalacceleration measurements from a few more pulsars in the cluster, it will bepossible to differentiate the source of the nonluminous matter.

Evidence of Dark Contents in the Center of NGC 6517