Discovery of a millisecond pulsar in the 5.4 day binary 3FGL J1417.5-4402: observing the late phase of pulsar recycling

TL;DR

This paper reports the discovery of a millisecond pulsar in a 5.4-day binary system, providing insights into pulsar recycling and binary evolution, with implications for neutron star mass and system dynamics.

Contribution

It presents the first detection of a millisecond pulsar in a wide binary with a non-eclipsing companion, expanding understanding of pulsar recycling in different binary configurations.

Findings

Pulsar has a 2.66 ms period and a 5.4-day orbit.

Neutron star mass estimated between 1.77 and 2.13 solar masses.

Discrepancy between optical and radio distance estimates.

Abstract

In a search of the unidentified Fermi gamma-ray source 3FGL J1417.5-4402 with the Parkes radio telescope, we discovered PSR J1417-4402, a 2.66 ms pulsar having the same 5.4 day orbital period as the optical and X-ray binary identified by Strader et al. The existence of radio pulsations implies that the neutron star is currently not accreting. Substantial outflows from the companion render the radio pulsar undetectable for more than half of the orbit, and may contribute to the observed Halpha emission. Our initial pulsar observations, together with the optically inferred orbit and inclination, imply a mass ratio of 0.171+/-0.002, a companion mass of M_2=0.33+/-0.03 Msun, and a neutron star mass in the range 1.77<M_1<2.13 Msun. However, there remains a discrepancy between the distance of 4.4 kpc inferred from the optical properties of the companion and the smaller radio dispersion measure distance of 1.6 kpc. The smaller distance would reduce the inferred Roche-lobe filling factor, increase the inferred inclination angle, and decrease the masses. As a wide binary, PSR J1417-4402 differs from the radio-eclipsing black widow and redback pulsars being discovered in large numbers by Fermi. It is probably a system that began mass transfer onto the neutron star after the companion star left the main sequence. The companion should end its evolution as a He white dwarf in a 6-20 day orbit, i.e., as a typical binary millisecond pulsar companion.