A neutral hydrogen distance limit to the relativistic binary PSR J1141-6545

Abstract

We have obtained an HI absorption spectrum of the relativistic binary PSR J1141-6545 and used it to constrain the distance to the system. The spectrum suggests that the pulsar is at, or beyond, the tangent point, estimated to be at 3.7 kpc. PSR J1141-6545 offers the promise of stringent tests of General Relativity (GR) by comparing its observed orbital period derivative with that derived from other relativistic observables. At the distance of PSR J1141-6545 it should be possible to verify GR to an accuracy of just a few percent, as contributions to the observed orbital period derivative from kinematic terms will be a small fraction of that induced by the emission of gravitational radiation. PSR J1141-6545 will thus make an exceptional gravitational laboratory.

arXiv commentAccepted for publication by MNRAS

References in corpus (4)

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Cited by in corpus (13)

• On Pulsar Distance Measurements and their Uncertainties
• Revisiting the radial distribution of pulsars in the Galaxy
• Gravitational-radiation losses from the pulsar-white-dwarf binary PSR J1141-6545
• Self-consistency of relativistic observables with general relativity in the white dwarf-neutron star binary pulsar PSR J1141-6545
• Lense-Thirring frame dragging induced by a fast-rotating white dwarf in a binary pulsar system
• A precise mass measurement of the intermediate-mass binary pulsar PSR J1802-2124
• Modelling annual and orbital variations in the scintillation of the relativistic binary PSR J1141$-$6545
• Geodetic Precession in PSR J1141-6545
• Merger of white dwarf-neutron star binaries: Prelude to hydrodynamic simulations in general relativity
• A 1.05 $M_{\odot }$ Companion to PSR J2222-0137: The Coolest Known White Dwarf?
• A white dwarf companion to the relativistic pulsar PSR J1141-6545
• Tiny-Scale Properties within the Interstellar Medium towards PSR J1644$-$4559: I. Observational Evidence of Turbulence-induced Tiny Scale Atomic Structures
• Characterizing Pulsar Distances Using HI Kinematics