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A pulsar in a binary with a compact object in the mass gap between neutron stars and black holes

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arxiv 2401.09872 v1 pith:Q2AKPBSL submitted 2024-01-18 astro-ph.HE gr-qcnucl-th

A pulsar in a binary with a compact object in the mass gap between neutron stars and black holes

Ewan D. Barr , Arunima Dutta , Paulo C. C. Freire , Mario Cadelano , Tasha Gautam , Michael Kramer , Cristina Pallanca , Scott M. Ransom
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Alessandro Ridolfi Benjamin W. Stappers Thomas M. Tauris Vivek Venkatraman Krishnan Norbert Wex Matthew Bailes Jan Behrend Sarah Buchner Marta Burgay Weiwei Chen David J. Champion C.-H. Rosie Chen Alessandro Corongiu Marisa Geyer Y. P. Men Prajwal V. Padmanabh Andrea Possenti
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keywords masspulsarbinarycompactmassesmassiveblackcompanion
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Among the compact objects observed in gravitational wave merger events a few have masses in the gap between the most massive neutron stars (NSs) and least massive black holes (BHs) known. Their nature and the formation of their merging binaries are not well understood. We report on pulsar timing observations using the Karoo Array Telescope (MeerKAT) of PSR J0514-4002E, an eccentric binary millisecond pulsar in the globular cluster NGC 1851 with a total binary mass of $3.887 \pm 0.004$ solar masses. The companion to the pulsar is a compact object and its mass (between $2.09$ and $2.71$ solar masses, 95% confidence interval) is in the mass gap, so it either is a very massive NS or a low-mass BH. We propose the companion was formed by a merger between two earlier NSs.

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Cited by 6 Pith papers

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    Parameterized inspiral tests on GW230529 find consistency with GR, with |δφ̂_{-2}| ≲ 8×10^{-5} and ℓ_GB ≲ 0.51 M_⊙ in ESGB theories.

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