A Possible γ-ray Pulsation from PSR J1740−5340B in the Globular Cluster NGC 6397

Abstract

Recently, a new radio millisecond pulsar (MSP) J1740–5340B, hosted in the globu- lar cluster NGC 6397, was reported with a spin period 5.78 ms in an eclipsing binary system with an orbital period of 1.97 day. Based on a modified radio ephemeris updated by tool tempo2, we analyze the ∼15 year γ-ray data obtained from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope and detect PSR J1740−5340B’s γ-ray pulsation at a confidence level of ∼4σ with a weighted H-test value of ∼26. By performing a phase-resolved analysis, the γ-ray luminosity in on-pulse interval of PSR J1740–5340B is Lγ ∼ 3.8 × 1033 erg/s using the NGC 6397’s distance of 2.48 kpc. And γ-rays from the on-pulse part of PSR J1740−5340B contribute ∼90% of the total observed γ-ray emissions from NGC 6397. No significant γ-ray pulsation of another MSP J1740–5340A in the GC is detected. Considering that the previous four cases of MSPs in GCs, more data in γ-ray, X-ray, and radio are encouraged to finally confirm the γ-ray emissions from MSP J1740−5340B, especially starving for a precise ephemeris.