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GW190425: Observation of a Compact Binary Coalescence with Total Mass sim 3.4 M_odot

The LIGO Scientific Collaboration, The Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., et al. (in preparation). GW190425: Observation of a Compact Binary Coalescence with Total Mass sim 3.4 M_odot.

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2001.01761.pdf (Preprint), 29MB
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### Creators

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Creators:
The LIGO Scientific Collaboration, Author
The Virgo Collaboration, Author
Abbott, B. P., Author
Abbott, R., Author
Abbott, T. D., Author
Abraham, S., Author
Acernese, F., Author
Ackley, K., Author
Affeldt, C.1, Author
Agathos, M., Author
Agatsuma, K., Author
Aggarwal, N., Author
Aguiar, O. D., Author
Aiello, L., Author
Ain, A., Author
Ajith, P., Author
Allen, G., Author
Affiliations:
1Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24010
2Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290
3Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011
4Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_2541714
5Binary Merger Observations and Numerical Relativity, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2461691

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
Abstract: On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from 1.12 to 2.52 $M_{\odot}$ (1.45 to 1.88 $M_{\odot}$ if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass $1.44^{+0.02}_{-0.02} M_{\odot}$ and the total mass $3.4^{+0.3}_{-0.1}\,M_{\odot}$ of this system are significantly larger than those of any other known binary neutron star system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic binary neutron star population. Under the assumption that the signal was produced by a binary neutron star coalescence, the local rate of neutron star mergers is updated to $250-2810 \text{Gpc}^{-3}\text{yr}^{-1}$.

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Dates: 2020-01-06
Publication Status: Not specified
Pages: 32 pages, 19 figures, submitted to ApJL
Publishing info: -
Rev. Method: -
Identifiers: arXiv: 2001.01761
URI: http://arxiv.org/abs/2001.01761
Degree: -

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