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We describe the observation of GW170104, a gravitational-wave signal produced by the coalescence of a pair of stellar-mass black holes. The signal was measured on January 4, 2017 at 10∶11:58.6 UTC by the twin advanced detectors of the Laser Interferometer Gravitational-Wave Observatory during their second observing run, with a network signal-to-noise ratio of 13 and a false alarm rate less than 1 in 70 000 years. The inferred component black hole masses are
31.2 +8.4 −6.0
M⊙ and
19.4 + 5.3 −5.9 M⊙
(at the 90% credible level). The black hole spins are best constrained through measurement of the effective inspiral spin parameter, a mass-weighted combination of the spin components perpendicular to the orbital plane,
χ_eff = −0.12 +0.21 −0.30. This result implies that spin configurations with both component spins positively aligned with the orbital angular momentum are disfavored. The source luminosity distance is 880 +450 −390 Mpc corresponding to a redshift of z = 0.18 +0.08 −0.07. We constrain the magnitude of modifications to the gravitational-wave dispersion relation and perform null tests of general relativity. Assuming that gravitons are dispersed in vacuum like massive particles, we bound the graviton mass to m_g ≤ 7.7 ×10−23 eV/c^2. In all cases, we find that GW170104 is consistent with general relativity.
Abbott, B. ., Abbott, R., Abbott, T. ., Acernese, F., Ackley, K., Adams, C., et al. (2017). GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2. PHYSICAL REVIEW LETTERS, 118(22), 221101-1-221101-17 [10.1103/PhysRevLett.118.221101].
GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2
Abbott, B. .p.;Abbott, R.;Abbott, T. .d.;Acernese, F.;Ackley, K.;Adams, C.;Adams, T.;Addesso, P.;Adhikari, R. .x.;Adya, V. .b.;Affeldt, C.;Afrough, M.;Agarwal, B.;Agathos, M.;Agatsuma, K.;Aggarwal, N.;Aguiar, O. .d.;Aiello, L.;Ain, A.;Ajith, P.;Allen, B.;Allen, G.;Allocca, A.;Altin, P. .a.;Amato, A.;Ananyeva, A.;Anderson, S. .b.;Anderson, W. .g.;Antier, S.;Appert, S.;Arai, K.;Araya, M. .c.;Areeda, J. .s.;Arnaud, N.;Arun, K. .g.;Ascenzi, S.;Ashton, G.;Ast, M.;Aston, S. .m.;Astone, P.;Aufmuth, P.;Aulbert, C.;Aultoneal, K.;Avila Alvarez, A.;Babak, S.;Bacon, P.;Bader, M. .k. .m.;Bae, S.;Baker, P. .t.;Baldaccini, F.;Ballardin, G.;Ballmer, S. .w.;Banagiri, S.;Barayoga, J. .c.;Barclay, S. .e.;Barish, B. .c.;Barker, D.;Barone, F.;Barr, B.;Barsotti, L.;Barsuglia, M.;Barta, D.;Bartlett, J.;Bartos, I.;Bassiri, R.;Basti, A.;Batch, J. .c.;Baune, C.;Bawaj, M.;Bazzan, M.;Bécsy, B.;Beer, C.;Bejger, M.;Belahcene, I.;Bell, A. .s.;Berger, B. .k.;Bergmann, G.;Berry, C. .p. .l.;Bersanetti, D.;Bertolini, A.;Betzwieser, J.;Bhagwat, S.;Bhandare, R.;Bilenko, I. .a.;Billingsley, G.;Billman, C. .r.;Birch, J.;Birney, R.;Birnholtz, O.;Biscans, S.;Bisht, A.;Bitossi, M.;Biwer, C.;Bizouard, M. .a.;Blackburn, J. .k.;Blackman, J.;Blair, C. .d.;Blair, D. .g.;Blair, R. .m.;Bloemen, S.;Bock, O.;Bode, N.;Boer, M.;Bogaert, G.;Bohe, A.;Bondu, F.;Bonnand, R.;Boom, B. .a.;Bork, R.;Boschi, V.;Bose, S.;Bouffanais, Y.;Bozzi, A.;Bradaschia, C.;Brady, P. .r.;Braginsky, V. .b.;BRANCHESI, MARICA;Brau, J. .e.;Briant, T.;Brillet, A.;Brinkmann, M.;Brisson, V.;Brockill, P.;Broida, J. .e.;Brooks, A. .f.;Brown, D. .a.;Brown, D. .d.;Brown, N. .m.;Brunett, S.;Buchanan, C. .c.;Buikema, A.;Bulik, T.;Bulten, H. .j.;Buonanno, A.;Buskulic, D.;Buy, C.;Byer, R. .l.;Cabero, M.;Cadonati, L.;Cagnoli, G.;Cahillane, C.;Calderón Bustillo, J.;Callister, T. .a.;Calloni, E.;Camp, J. .b.;Canepa, M.;Canizares, P.;Cannon, K. .c.;Cao, H.;Cao, J.;Capano, C. .d.;Capocasa, E.;Carbognani, F.;Caride, S.;Carney, M. .f.;Casanueva Diaz, J.;Casentini, C.;Caudill, S.;Cavaglià, M.;Cavalier, F.;Cavalieri, R.;Cella, G.;Cepeda, C. .b.;CERBONI BAIARDI, LORENZO;Cerretani, G.;Cesarini, E.;Chamberlin, S. .j.;Chan, M.;Chao, S.;Charlton, P.;Chassande Mottin, E.;Chatterjee, D.;Chatziioannou, K.;Cheeseboro, B. .d.;Chen, H. .y.;Chen, Y.;Cheng, H. 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2017
Abstract
We describe the observation of GW170104, a gravitational-wave signal produced by the coalescence of a pair of stellar-mass black holes. The signal was measured on January 4, 2017 at 10∶11:58.6 UTC by the twin advanced detectors of the Laser Interferometer Gravitational-Wave Observatory during their second observing run, with a network signal-to-noise ratio of 13 and a false alarm rate less than 1 in 70 000 years. The inferred component black hole masses are
31.2 +8.4 −6.0
M⊙ and
19.4 + 5.3 −5.9 M⊙
(at the 90% credible level). The black hole spins are best constrained through measurement of the effective inspiral spin parameter, a mass-weighted combination of the spin components perpendicular to the orbital plane,
χ_eff = −0.12 +0.21 −0.30. This result implies that spin configurations with both component spins positively aligned with the orbital angular momentum are disfavored. The source luminosity distance is 880 +450 −390 Mpc corresponding to a redshift of z = 0.18 +0.08 −0.07. We constrain the magnitude of modifications to the gravitational-wave dispersion relation and perform null tests of general relativity. Assuming that gravitons are dispersed in vacuum like massive particles, we bound the graviton mass to m_g ≤ 7.7 ×10−23 eV/c^2. In all cases, we find that GW170104 is consistent with general relativity.
Abbott, B. ., Abbott, R., Abbott, T. ., Acernese, F., Ackley, K., Adams, C., et al. (2017). GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2. PHYSICAL REVIEW LETTERS, 118(22), 221101-1-221101-17 [10.1103/PhysRevLett.118.221101].
Abbott, B. .p.; Abbott, R.; Abbott, T. .d.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. .x.; Adya, V. .b.; Affeldt, ...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/865862
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.