Shapiro delay in PSR~J1811$-$2405

Abstract

This paper presents the first detection of Shapiro delay from the binary millisecond pulsar PSR J1811-2405. We report a 11-$\sigma$ measurement of the orthometric amplitude, h${}_3$=6.8(6)x10${}^{-7}$, and a 16-$\sigma$ measurement of the orthometric ratio, $\varsigma$= 0.81(5). Given the relatively high orbital inclination, i= 79(2) deg, of this binary system, we obtain constraints on the companion mass of m${}_c$= 0.31$\begin{array}{c}+0.08\\ -0.06\end{array}{M}_{\odot }$. The pulsar mass is currently less well constrained, with a value of 2.0$\begin{array}{c}+0.8\\ -0.5\end{array}{M}_{\odot }$. The companion mass and the orbital period are in agreement with the prediction made by previous numerical calculations of the evolution of compact binary systems. From a study of the polarization, we find that the orbital inclination angle is ~100 deg and that PSR J1811-2405 is an orthogonal rotator. In addition, the $\mu$s-level timing precision together with its narrow profile make PSR J1811-2405 a good candidate for inclusion in the pulsar timing arrays being used to detect nHz Gravitational waves.

7 pages, 5 figures, accepted by MNRAS

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