Radio timing constraints on the mass of the binary pulsar PSR J1528-3146

Context.PSR J1528 3146 is a 60.8 ms pulsar orbiting a heavy white dwarf (WD) companion, with an orbital period of 3.18 d. The pulsar was discovered in the early 2000 s in a survey at 1.4 GHz of intermediate Galactic latitudes conducted with the Parkes radio telescope. The initial timing analysis of PSR J1528 3146, using data recorded from 2001 and 2004, did not reveal any relativistic perturbations to the orbit of the pulsar or to the propagation of its pulses. However, with an orbital eccentricity of similar to 0:0002 and a large companion mass on the order of 1 M fi, this system has been deemed likely to exhibit measurable perturbations. Aims. This work is aimed at characterizing the pulsar's astrometric, spin, and orbital parameters by analyzing timing measurements conducted at the Parkes, MeerKAT, and Nancay radio telescopes over nearly two decades. The measurement of post-Keplerian perturbations to the pulsar's orbit can be used to constrain the masses of the two component stars of the binary and, in turn, to o ffer insights into the history of the system. Methods. We analyzed timing data from the Parkes, MeerKAT, and Nancay radio telescopes collected over about 16 yr, obtaining a precise rotation ephemeris for PSR J1528 3146. A Bayesian analysis of the timing data was carried out to constrain the masses of the two components and the orientation of the orbit. We further analyzed the polarization properties of the pulsar to constrain the orientation of the magnetic axis and of the line of sight with respect to the spin axis. Results. We measured a significant rate of advance of periastron, for the first time, and we set constraints on the Shapiro delay in the system and on the rate of change of the projected semi-major axis of the pulsar's orbit. The Bayesian analysis yielded measurements for the pulsar and companion masses of Mp = 1:61(+0:14) (0:13) M-circle dot and Mc = 1:33(+0:08) (0:07) M-circle dot(68% C.L.), respectively, confirming that the companion is indeed massive. This companion mass as well as other characteristics of PSR J1528 3146 indicate that this pulsar is very similar to PSR J2222 0137, a 32.8 ms pulsar orbiting a WD whose heavy mass ( similar to 1 :32 M-circle dot) has been considered unique among pulsar-WD systems until now. Our measurements suggest common evolutionary scenarios for PSRs J1528 3146 and J2222 0137.