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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 11σ measurement of the orthometric amplitude, h_3 = 6.8(6) × 10^−7, and a 16σ measurement of the orthometric ratio, ς = 0.81(5). Given the relatively high orbital inclination, i = 79(2)°, of this binary system, we obtain constraints on the companion mass of |$m_{\rm {c}}=0.31^{+0.08 }_{ -0.06}\, \mathrm{M}_{\odot }$|⁠. The pulsar mass is currently less well constrained, with a value of |$2.0^{+0.8 }_{ -0.5}\, \mathrm{M}_{\odot }$|⁠. 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° and that PSR J1811–2405 is an orthogonal rotator. In addition, the μs-level timing precision together with its narrow profile makes PSR J1811–2405 a good candidate for inclusion in the pulsar timing arrays being used to detect nHz gravitational waves.
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C. Ng, L. Guillemot, P.C.C. Freire, M. Kramer, D.J. Champion, et al.. Shapiro delay in PSR~J1811$-$2405. Mon.Not.Roy.Astron.Soc., 2020, 493 (1), pp.1261-1267. ⟨10.1093/mnras/staa337⟩. ⟨hal-02491328⟩

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