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GW190521: A Binary Black Hole Merger with a Total Mass of 150 M-circle dot

Title
GW190521: A Binary Black Hole Merger with a Total Mass of 150 M-circle dot
Authors
Ogin, G. H.Oh, J. J.Oh, S. H.Ohme, F.Ohta, H.Okada, M. A.Oliver, M.Oppermann, P.Oram, Richard J.O'Reilly, B.Ormiston, R. G.Ortega, L. F.O'Shaughnessy, R.Ossokine, S.Ottaway, D. J.Overmier, H.Owen, B. J.Pace, A. E.Pagano, G.Page, M. A.Pagliaroli, G.Pai, A.Pai, S. A.Palamos, J. R.Palashov, O.Palomba, C.Pan, H.Panda, P. K.Pang, P. T. H.Pankow, C.Pannarale, F.Pant, B. C.Paoletti, F.Paoli, A.Parida, A.Parker, W.Pascucci, D.Pasqualetti, A.Passaquieti, R.Passuello, D.Patil, M.Patricelli, B.Payne, E.Pearlstone, B. L.Pechsiri, T. C.Pedersen, A. J.Pedraza, M.Pedurand, R.Pele, A.Penn, S.Perego, A.Perez, C. J.Perigois, C.Perreca, A.Petermann, J.Pfeiffer, H. P.Phelps, M.Phukon, K. S.Piccinni, O. J.Pichot, M.Piergiovanni, F.Pierro, V.Pillant, G.Pinard, L.Pinto, I. M.Pirello, M.Pitkin, M.Plastino, W.Pong, D. Y. T.Ponrathnam, S.Popolizio, P.Porter, E. K.Powell, J.Prajapati, A. K.Prasad, J.Prasai, K.Prasanna, R.Pratten, G.Prestegard, T.Principe, M.Prodi, G. A.Prokhorov, L.Punturo, M.Puppo, P.Puerrer, M.Qi, H.Quetschke, V.Quinonez, P. J.Raab, F. J.Raaijmakers, G.Radkins, H.Radulesco, N.Raffai, P.Raja, S.Rajan, C.Rajbhandari, B.Rakhmanov, M.Ramirez, K. E.Ramos-Buades, A.Rana, JavedRao, K.Rapagnani, P.Raymond, V.Razzano, M.Read, J.Regimbau, T.Rei, L.Reid, S.Reitze, D. H.Rettegno, P.Ricci, F.Richardson, C. J.Richardson, J. W.Ricker, P. M.Riemenschneider, G.Riles, K.Rizzo, M.Robertson, N. A.Robinet, F.Rocchi, A.Rolland, L.Rollins, J. G.Roma, V. J.Romanelli, M.Romano, R.Romel, C. L.Romie, J. H.Rose, C. A.Rose, D.Rose, K.Rosinska, D.Rosofsky, S. G.Ross, M. P.Rowan, S.Ruediger, A.Ruggi, P.Rutins, G.Ryan, K.Sachdev, S.Sadecki, T.Sakellariadou, M.Salafia, O. S.Salconi, L.Zendri, J. -P.Zevin, M.Zhang, J.Zhang, L.Zhang, T.Zhao, C.Zhao, G.Zhou, M.Zhou, Z.Zhu, X. J.Zimmerman, A. B.Zucker, M. E.Zweizig, J.LIGO Sci CollaborationVirgo CollaborationChiadini, 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. D.Cripe, J.Croquette, M.Crowder, S. G.Cullen, T. J.Cumming, A.Cunningham, L.Cuoco, E.Dal Canton, T.Dalya, G.D'Angelo, B.Danilishin, S. L.D'Antonio, S.Danzmann, K.Dasgupta, A.Da Silva Costa, C. F.Datrier, L. E. H.Dattilo, V.Dave, I.Davier, M.Davis, D.Daw, E. J.DeBra, D.Deenadayalan, M.Degallaix, J.De laurentis, M.Deleglise, S.Del Pozzo, W.DeMarchi, L. 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G.Nagar, A.Nardecchia, I.Naticchioni, L.Nayak, R. K.Neil, B. F.Neilson, J.Nelemans, G.Nelson, T. J. N.Nery, M.Neunzert, A.Nevin, L.Ng, K. Y.Ng, S.Nguyen, C.Nguyen, P.Nichols, D.Nichols, S. A.Nissanke, S.Nocera, F.North, C.Nuttall, L. K.Obergaulinger, M.Oberling, J.O'Brien, B. D.Oganesyan, G.
Ewha Authors
김정리
SCOPUS Author ID
김정리scopus
Issue Date
2020
Journal Title
PHYSICAL REVIEW LETTERS
ISSN
0031-9007JCR Link

1079-7114JCR Link
Citation
PHYSICAL REVIEW LETTERS vol. 125, no. 10
Publisher
AMER PHYSICAL SOC
Indexed
SCIE; SCOPUS WOS scopus
Document Type
Article
Abstract
On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85(-14)(+21) M-circle dot and 66(-18)(+17) M-circle dot (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65 M-circle dot. We calculate the mass of the remnant to be 142(-16)(+28) M-circle dot, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3(-2.6)(+2.4) Gpc, corresponding to a redshift of 0.82(-0.34)(+0.28). The inferred rate of mergers similar to GW190521 is 0.13(-0.11)(+0.30) Gpc(-3) yr(-1).
DOI
10.1103/PhysRevLett.125.101102
Appears in Collections:
자연과학대학 > 물리학전공 > Journal papers
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