Discovery and Timing of Millisecond Pulsars in the Globular Cluster M5 with FAST and Arecibo

Abstract

We report on a comprehensive multiwavelength study of the pulsars in the globular cluster (GC) M5, including the discovery of M5G, a new compact noneclipsing “black widow” pulsar. Thanks to the analysis of 34 yr of radio data taken with the Five-hundred-meter Aperture Spherical radio Telescope and Arecibo telescopes, we obtained new phase-connected timing solutions for four pulsars and improved those of the other three. These have resulted in, among other things, (a) much improved proper motions for five pulsars, with transverse velocities (relative to the cluster) that are smaller than their respective escape velocities; (b) 3σ and 1.5σ detections of Shapiro delays in M5F and M5D, respectively; and (c) greatly improved measurement of the periastron advance in M5B, whose value of ω ̇ = 0 .° 01361 ( 6 ) implies that M5B is still likely to be a heavy ( m p = 1.981 − 0.088 + 0.038 M ⊙ ) neutron star. The binary pulsars M5D, M5E, and M5F are confirmed to be in low-eccentricity binary systems, the low-mass companions of which are newly identified to be He white dwarfs using Hubble Space Telescope data. Four pulsars are also found to be associated with X-ray sources. Similarly to the eclipsing pulsar M5C, M5G shows little or no nonthermal X-ray emission, indicative of weak synchrotron radiation produced by intrabinary shocks. All seven pulsars known in M5 have short spin periods (<8 ms), and five are in binary systems with low orbital eccentricities. These characteristics differ from the overall GC pulsar population but confirm the expectations for the pulsar population in a cluster with a small rate of stellar encounters per binary system.

Characterizing the Gamma-Ray Emission Properties of the Globular Cluster M5 with the Fermi-LAT

“…a The eccentricities of M5C and M5G have been set to 0 based on the assumption that the orbits of BW pulsars are circular owing to tidal dissipation (see Table 1 in Zhang et al 2023a).…”

“…b Spin-down powers  E have been calculated based on the intrinsic spin-down rate  P int upper limit corrected for accelerations caused by the gravitational field of the GC for the line of sight of each pulsar (see Table 2 in Zhang et al 2023a).…”

“…01361 w =  yr −1 of M5B is compatible with a heavy neutron star (NS), consistent with previous studies. Although its inclination is not well constrained, M5B is probably not edge-on (Zhang et al 2023a).…”

“…The cluster is at a distance of 7.48 ± 0.60 kpc with a half-mass radius of 5.6 pc. 27 Radio observations using Arecibo and FAST have resulted in the detection of seven MSPs in M5 (Anderson et al 1997;Mott & Freire 2003;Hessels et al 2007;Pan et al 2021;Zhang et al 2023a). The first discoveries were then known as B1516+02A and B1516+02B; they are now known as PSRs J1518+0204A and J1518+0204B.…”

“…The following discoveries are known as J1518+0204C−J1518+0204G, and we will refer to these pulsars as M5A, M5B, M5C, M5D, M5E, M5F, and M5G, respectively. Improved timing solutions for all these pulsars have been derived based on observations using the two telescopes (Zhang et al 2023a).…”