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 31.2þ8.4 −6.0M⊙ and 19.4þ5.3 −5.9M⊙ (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, χeff ¼ −0.12þ0.21 −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 880þ450 −390 Mpc corresponding to a redshift of z ¼ 0.18þ0.08 −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 mg ≤ 7.7 × 10−23 eV=c2. In all cases, we find that GW170104 is consistent with general relativity

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., et al.. - In: PHYSICAL REVIEW LETTERS. - ISSN 0031-9007. - 118:22(2017). [10.1103/PhysRevLett.118.221101]

GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2

ASTONE, PIA;CASENTINI, CLAUDIO;COLLA, ALBERTO;DI PACE, SIBILLA;DI PALMA, IRENE;Drago, M.;FRASCA, Simona;INTINI, GIUSEPPE;LEACI, PAOLA;MAJORANA, ETTORE;MANGANO, VALENTINA;MASTROGIOVANNI, SIMONE;MEZZANI, FEDERICA;MILLER, ANDREW LAWRENCE;NARDECCHIA, ILARIA;NATICCHIONI, LUCA;Pannarale, F.;PICCINNI, ORNELLA JULIANA;RAPAGNANI, Piero;RICCI, Fulvio;Salemi, F.;Di Giovanni, M.
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 31.2þ8.4 −6.0M⊙ and 19.4þ5.3 −5.9M⊙ (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, χeff ¼ −0.12þ0.21 −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 880þ450 −390 Mpc corresponding to a redshift of z ¼ 0.18þ0.08 −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 mg ≤ 7.7 × 10−23 eV=c2. In all cases, we find that GW170104 is consistent with general relativity
2017
gravitational-wave observations; compact object formation; galactic distribution
01 Pubblicazione su rivista::01a Articolo in rivista
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., et al.. - In: PHYSICAL REVIEW LETTERS. - ISSN 0031-9007. - 118:22(2017). [10.1103/PhysRevLett.118.221101]
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11573/991314
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