̊m PSR J1455-3330 is a ∼7. 98 ms pulsar in a ∼76. 17 day nearly circular orbit with a white dwarf companion. In this work, we combine the available Lovell, Nançay decimetric Radio Telescope, Green Bank, and MeerKAT pulsar timing data spanning approximately 30 years to measure the kinematic and relativistic effects of PSR J1455-3330 to constrain its 3D orbital geometry and component masses. We detect a relativistic Shapiro delay signal. We measure a significant orthometric amplitude of h₃ = 0. 307^ +0. 022 _ -0. 026 μs and an orthometric ratio of ̌arsigma = 0. 551^ +0. 057 _ -0. 054. We measured the change in projected semi-major axis, dot x = -202. 1^ +2. 5 _ -2. 7 -16, ̊m -1, with high significance, parallax, ̌arpi = 1. 11 (6) mas, parallax derived distance 0. 90 (5) kpc, and a precise total proper motion magnitude of 12. 432 (2) mas yr -1. A self-consistent analysis of all kinematic and relativistic effects, assuming general relativity, yielded two solutions: (1) a pulsar mass of M_ ̊m p = 1. 39^ +0. 38 _ -0. 18, ̊m M_⊙, a companion mass of M_ ̊m c = 0. 293^ +0. 056 _ -0. 026 ̊m M_⊙, an orbital inclination of i = 63 (2) ^ ̧irc, and a longitude of the ascending node of Ω = 212 (12) ^ ̧irc or (2) a pulsar mass of M_ ̊m p = 1. 53^ +1. 10 _ -0. 22, ̊m M_⊙, a companion mass of M_ ̊m c = 0. 309^ +0. 163 _ -0. 026, ̊m M_⊙, an orbital inclination of i = 123 (4) ^ ̧irc, and a longitude of the ascending node of Ω = 334 (12) ^ ̧irc. All uncertainties represent the 68. 27% credibility region. These results strongly favour a helium-dominated white dwarf companion.
Pillay et al. (Thu,) studied this question.