The neutron star mass, distance, and inclination from precision timing of the brilliant millisecond pulsar J0437$-$4715

TL;DR

This paper presents precise measurements of the neutron star PSR J0437-4715's mass, distance, and orbital inclination using 26 years of radio timing data, aiding neutron star equation of state constraints.

Contribution

It provides the most accurate pulsar mass, distance, and inclination measurements to date, improving constraints on neutron star properties and informing X-ray pulse profile models from NICER.

Findings

Pulsar mass measured as 1.418±0.044 M_sun

Distance determined as 156.96±0.11 pc

Orbital inclination angle measured as 137.506±0.016 degrees

Abstract

The observation of neutron stars enables the otherwise impossible study of fundamental physical processes. The timing of binary radio pulsars is particularly powerful, as it enables precise characterization of their (three-dimensional) positions and orbits. PSR~J0437$-$4715 is an important millisecond pulsar for timing array experiments and is also a primary target for the Neutron Star Interior Composition Explorer (NICER). The main aim of the NICER mission is to constrain the neutron star equation of state by inferring the compactness ($M_p/R$) of the star. Direct measurements of the mass $M_p$ from pulsar timing therefore substantially improve constraints on the radius $R$ and the equation of state. Here we use observations spanning 26 years from Murriyang, the 64-m Parkes radio telescope, to improve the timing model for this pulsar. Among the new precise measurements are the pulsar mass $M_p=1.418\pm 0.044$ $M_{\odot}$, distance $D=156.96 \pm 0.11$ pc, and orbital inclination angle $i=137.506 \pm 0.016^\circ$, which can be used to inform the X-ray pulse profile models inferred from NICER observations. We demonstrate that these results are consistent between multiple data sets from the Parkes Pulsar Timing Array (PPTA), each modeled with different noise assumptions. Using the longest available PPTA data set, we measure an apparent second derivative of the pulsar spin frequency and discuss how this can be explained either by kinematic effects due to the proper motion and radial velocity of the pulsar or excess low-frequency noise such as a gravitational-wave background.