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GW190425: Observation of a Compact Binary Coalescence with Total Mass similar to 3.4 M-circle dot

Title
GW190425: Observation of a Compact Binary Coalescence with Total Mass similar to 3.4 M-circle dot
Authors
Abbott, B. P.Abbott, R.Abbott, T. D.Abraham, S.Acernese, F.Ackley, K.Adams, C.Adhikari, R. X.Adya, V. B.Affeldt, C.Agathos, M.Agatsuma, K.Aggarwal, N.Aguiar, O. D.Aiello, L.Ain, A.Ajith, P.Allen, G.Allocca, A.Aloy, M. A.Altin, P. A.Amato, A.Anand, S.Ananyeva, A.Anderson, S. B.Anderson, W. G.Angelova, S. V.Antier, S.Appert, S.Arai, K.Araya, M. C.Areeda, J. S.Arene, M.Arnaud, N.Aronson, S. M.Arun, K. G.Ascenzi, S.Ashton, G.Aston, S. M.Astone, P.Aubin, F.Aufmuth, P.AultONeal, K.Austin, C.Avendano, V.Avila-Alvarez, A.Babak, S.Bacon, P.Badaracco, F.Bader, M. K. M.Bae, S.Baird, J.Baker, P. T.Baldaccini, F.Ballardin, G.Ballmer, S. W.Bals, A.Banagiri, S.Barayoga, J. C.Barbieri, C.Barclay, S. E.Barish, B. C.Barker, D.Barkett, K.Barnum, S.Barone, F.Barr, B.Barsotti, L.Barsuglia, M.Barta, D.Bartlett, J.Bartos, I.Bassiri, R.Basti, A.Bawaj, M.Bayley, J. C.Baylor, A. C.Bazzan, M.Becsy, B.Bejger, M.Belahcene, I.Bell, A. S.Beniwal, D.Benjamin, M. G.Berger, B. K.Bergmann, G.Bernuzzi, S.Berry, C. P. L.Bersanetti, D.Bertolini, A.Betzwieser, J.Bhandare, R.Bidler, J.Biggs, E.Bilenko, I. A.Bilgili, S. A.Billingsley, G.Birney, R.Birnholtz, O.Biscans, S.Bischi, M.Biscoveanu, S.Bisht, A.Bitossi, M.Bizouard, M. A.Blackburn, J. K.Blackman, J.Blair, C. D.Blair, D. G.Blair, R. M.Bloemen, S.Bobba, F.Bode, N.Boer, M.Boetzel, Y.Bogaert, G.Bondu, F.Bonnand, R.Booker, P.Boom, B. A.Bork, R.Boschi, V.Bose, S.Bossilkov, V.Bosveld, J.Bouffanais, Y.Bozzi, A.Bradaschia, C.Brady, P. R.Bramley, A.Branchesi, M.Brau, J. E.Breschi, M.Briant, T.Briggs, J. H.Brighenti, F.Brillet, A.Brinkmann, M.Brockill, P.Brooks, A. F.Brooks, J.Brown, D. D.Brunett, S.Buikema, A.Bulik, T.Bulten, H. J.Buonanno, A.Buskulic, D.Buy, C.Byer, R. L.Cabero, M.Cadonati, L.Cagnoli, G.Cahillane, C.Bustillo, J. CalderonCallister, T. A.Calloni, E.Camp, J. B.Campbell, W. A.Canepa, M.Cannon, K. C.Cao, H.Cao, J.Carapella, G.Carbognani, F.Caride, S.Carney, M. F.Carullo, G.Diaz, J. CasanuevaCasentini, C.Caudill, S.Cavaglia, M.Cavalier, F.Cavalieri, R.Cella, G.Cerda-Duran, P.Cesarini, E.Chaibi, O.Chakravarti, K.Chamberlin, S. J.Chan, M.Chao, S.Charlton, P.Chase, E. A.Chassande-Mottin, E.Chatterjee, D.Chaturvedi, M.Chatziioannou, K.Cheeseboro, B. D.Chen, H. Y.Chen, X.Chen, Y.Cheng, H. -P.Cheong, C. K.Chia, H. Y.Chiadini, F.Chincarini, A.Chiummo, A.Cho, G.Cho, H. S.Cho, M.Christensen, N.Chu, Q.Chua, S.Chung, K. W.Chung, S.Ciani, G.Cieslar, M.Ciobanu, A. A.Ciolfi, R.Cipriano, F.Cirone, A.Clara, F.Clark, J. A.Clearwater, P.Cleva, F.Coccia, E.Cohadon, P. -F.Cohen, D.Colleoni, M.Collette, C. G.Collins, C.Colpi, M.Cominsky, L. R.Constancio, M., Jr.Conti, L.Cooper, S. J.Corban, P.Corbitt, T. R.Cordero-Carrion, I.Corezzi, S.Corley, K. R.Cornish, N.Corre, D.Corsi, A.Cortese, S.Costa, C. A.Cotesta, R.Coughlin, M. W.Coughlin, S. B.Coulon, J. -P.Countryman, S. T.Couvares, P.Covas, P. B.Cowan, E. E.Coward, D. M.Cowart, M. J.Coyne, D. C.Coyne, R.Creighton, J. D. E.Creighton, T. 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Ewha Authors
김정리
SCOPUS Author ID
김정리scopus
Issue Date
2020
Journal Title
ASTROPHYSICAL JOURNAL LETTERS
ISSN
2041-8205JCR Link

2041-8213JCR Link
Citation
ASTROPHYSICAL JOURNAL LETTERS vol. 892, no. 1
Publisher
IOP PUBLISHING LTD
Indexed
SCIE; SCOPUS WOS
Document Type
Article
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 from1.12 to 2.52 M-circle dot (1.46-1.87 M-circle dot 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-circle dot. and the total mass 3.4(-0.1)(+0.3) M-circle dot. 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 Gpc(-3) yr(-1).
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DOI
10.3847/2041-8213/ab75f5
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자연과학대학 > 물리학전공 > Journal papers
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