Searches for Shapiro delay in seven binary pulsars using the MeerKAT telescope. Issue 2 (2nd January 2023)

• Record Type: Journal Article
• Authors: Shamohammadi, M; Bailes, M; Freire, P C C; Parthasarathy, A; Reardon, D J; Shannon, R M; Venkatraman Krishnan, V; Bernadich, M C i; Cameron, A D; Champion, D J; Corongiu, A; Flynn, C; Geyer, M; Kramer, M; Miles, M T; Possenti, A; Spiewak, R
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 520:Issue 2(2023)
• Page Start: 1789
• Page End: 1806
• Publication Date: 2023-01-02
• Subjects: telescopes -- stars: neutron -- ulsars: general -- pulsars: individual: PSR J0101−6422, PSR J1101−6424, PSR J1125−6014, PSR J1514−4946, PSR J1614−2230, PSR J1732−5049, PSR J1909−3744; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac3719
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Precision timing of millisecond pulsars (MSPs) in binary systems enables observers to detect the relativistic Shapiro delay induced by space–time curvature. When favourably aligned, this enables constraints to be placed on the component masses and system orientation. Here, we present the results of timing campaigns on seven binary MSPs observed with the 64-antenna MeerKAT radio telescope that show evidence of Shapiro delay: PSRs J0101−6422, J1101−6424, J1125−6014, J1514−4946, J1614−2230, J1732−5049, and J1909−3744. Evidence for Shapiro delay was found in all of the systems, and for three the orientations and data quality enabled strong constraints on their orbital inclinations and component masses. For PSRs J1125−6014, J1614−2230, and J1909−3744, we determined pulsar masses to be $M_{\rm p} = 1.68\pm 0.17$, $1.94\pm 0.03$, and $1.45 \pm 0.03 \, {\rm M_{\odot }}$, and companion masses to be $M_{\rm c} = 0.33\pm 0.02$, $0.495\pm 0.005$, and $0.205 \pm 0.003 \, {\rm M_{\odot }}$, respectively. This provides the first independent confirmation of PSR J1614−2230's mass, one of the highest known. The Shapiro delays measured for PSRs J0101−6422, J1101−6424, J1514−4946, and J1732−5049 were only weak, and could not provide interesting component mass limits. Despite a large number of MSPs being routinely timed, relatively few have accurate masses via Shapiro delays. We use simulations to show that this is expected, and provide a formula for observers to assess how accurately a pulsar mass can be determined. We also discuss the observed correlation between pulsar companion masses and spin period, and the anticorrelation between recycled pulsar mass and their companion masses.