Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 475, Issue 1, Pages L57-L61Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnrasl/sly003
Keywords
gravitation; surveys; binaries: close; pulsars: individual: PSR J1757-1854
Categories
Funding
- Australian Government
- Science and Technology Facilities Council in the UK
- ARC Centres of Excellence [CE110001020, CE170100004]
- West Virginia University
- European Research Council (ERC) [279702]
- Max Planck Society
- ERC [610058]
- NSF [AST-1517003, OIA-1458952]
- Science and Technology Facilities Council [ST/P000649/1] Funding Source: researchfish
- Office Of The Director
- Office of Integrative Activities [1458952] Funding Source: National Science Foundation
- STFC [ST/P000649/1] Funding Source: UKRI
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We report the discovery of PSR J1757-1854, a 21.5-ms pulsar in a highly-eccentric, 4.4-h orbit with a neutron star (NS) companion. PSR J1757-1854 exhibits some of the most extreme relativistic parameters of any known pulsar, including the strongest relativistic effects due to gravitational-wave damping, with a merger time of 76 Myr. Following a 1.6-yr timing campaign, we have measured five post-Keplerian parameters, yielding the two component masses (m(p) = 1.3384(9) M-circle dot and m(c) = 1.3946(9) M-circle dot) plus three tests of general relativity, which the theory passes. The larger mass of the NS companion provides important clues regarding the binary formation of PSR J1757-1854. With simulations suggesting 3-sigma measurements of both the contribution of Lense-Thirring precession to the rate of change of the semimajor axis and the relativistic deformation of the orbit within similar to 7-9 yr, PSR J1757-1854 stands out as a unique laboratory for new tests of gravitational theories.
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