Assuming this is the case, the pulsar, at the GC’s distance of 9.46 kpc and having a spin-down luminosity of ≤4.3 × 10 ³⁵ erg s ⁻¹, would have a γ -ray luminosity of ≃(5.04 ± 0.44) × 10 ³⁴ erg s ⁻¹ and a γ -ray efficiency of ≳0.12. Based on the results of our analysis and different studies of the sources in the GC, the observed γ -ray emission from the GC could mainly arise from this MSP, like the previous two cases in the GCs NGC 6624 and NGC 6626. We thus consider that we have detected the γ -ray emission of the MSP, and discuss the implications. From timing analysis of the data, a pulse profile that is similar to the radio one is established. Motivated by the recent discovery of the pulsar J1835−3259B with a spin period 1.83 ms in the globular cluster (GC) NGC 6652, we analyze the γ -ray data obtained with the Large Area Telescope on board the Fermi Gamma-ray Space Telescope (Fermi) for the GC and detect the pulsations of this millisecond pulsar (MSP) at a 5.4 σ confidence level (the weighted H-test value is ∼41).
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