Details
| Original language | English |
|---|---|
| Article number | L3 |
| Number of pages | 24 |
| Journal | Astrophysical Journal Letters |
| Volume | 892 |
| Issue number | 1 |
| Publication status | Published - 19 Mar 2020 |
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 to 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 and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) 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 BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810.
ASJC Scopus subject areas
- Physics and Astronomy(all)
- Astronomy and Astrophysics
- Earth and Planetary Sciences(all)
- Space and Planetary Science
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In: Astrophysical Journal Letters, Vol. 892, No. 1, L3, 19.03.2020.
Research output: Contribution to journal › Article › Research › peer review
}
TY - JOUR
T1 - GW190425
T2 - Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M o
AU - The LIGO Scientific Collaboration
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Abraham, S.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adhikari, R. X.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Allen, G.
AU - Allocca, A.
AU - Aloy, M. A.
AU - Altin, P. A.
AU - Amato, A.
AU - Anand, S.
AU - Ananyeva, A.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Angelova, S. V.
AU - Antier, S.
AU - Appert, S.
AU - Arai, K.
AU - Araya, M. C.
AU - Areeda, J. S.
AU - Arène, M.
AU - Arnaud, N.
AU - Aronson, S. M.
AU - Arun, K. G.
AU - Ascenzi, S.
AU - Ashton, G.
AU - Aston, S. M.
AU - Astone, P.
AU - Danilishin, S. L.
AU - Danzmann, K.
AU - Heurs, M.
AU - Lück, H.
AU - Steinmeyer, D.
AU - Vahlbruch, H.
AU - Wei, L.-w.
AU - Wilken, D. M.
AU - Willke, B.
AU - Wittel, H.
AU - Bose, Sukanta
AU - Brown, D. D.
AU - Chen, Y. B.
AU - Cheng, Hai-Ping
AU - Gniesmer, J.
AU - Hanke, Manuela
AU - Hennig, J.
AU - Hübner, M. T.
AU - Lang, R. N.
AU - Lee, C. H.
AU - Lee, H. K.
AU - Lee, H. M.
AU - Lee, H. W.
AU - Lee, J.
AU - Lee, K.
AU - Li, X.
AU - Rose, C. A.
AU - Rose, D.
AU - Sanders, J. R.
AU - S., Roy
AU - Schmidt, Patricia
AU - Sun, L.
AU - Wu, D. S.
AU - Zhang, L.
AU - Zhu, X. J.
AU - Zhou, Minchuan
AU - Bergmann, G.
AU - Bisht, Aparna
AU - Bode, Nina
AU - Booker, P.
AU - Brinkmann, Marc
AU - Cabero, M.
AU - de Varona, O.
AU - Hochheim, S.
AU - Junker, J.
AU - Kastaun, W.
AU - Kaufer, Stefan
AU - Kirchhoff, R.
AU - Koch, P.
AU - Koper, N.
AU - Köhlenbeck, S. M.
AU - Khan, S.
AU - Krämer, C.
AU - Kringel, Volker
AU - Kuehn, G.
AU - Leavey, S.
AU - Lehmann, J.
AU - Lough, James
AU - Mehmet, Moritz
AU - Meylahn, Fabian
AU - Mukund, Nikhil
AU - Nery, M.
AU - Ohme, F.
AU - Oppermann, P.
AU - Schreiber, Emil
AU - Schulte, B. W.
AU - Setyawati, Y.
AU - Steinke, M.
AU - Rüdiger, A.
AU - Phelps, M.
AU - Weinert, Michael
AU - Wellmann, F.
AU - Weßels, Peter
AU - Winkler, W.
AU - Woehler, J.
AU - Aufmuth, Peter
AU - Bergamin, Fabio
AU - Mukherjee, Arunava
AU - Standke, M.
N1 - Funding Information: SK acknowledges SERB, DST, Govt. of India for financial support through project ECR/2016/000022. AS acknowledges Council of Scientific and Industrial Research for Senior Research Fellowship.
PY - 2020/3/19
Y1 - 2020/3/19
N2 - 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 to 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 and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) 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 BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810.
AB - 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 to 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 and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) 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 BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810.
UR - http://www.scopus.com/inward/record.url?scp=85084498879&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/ab75f5
DO - 10.3847/2041-8213/ab75f5
M3 - Article
VL - 892
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 1
M1 - L3
ER -