Abstract
We report the observation of a gravitational-wave signal produced by the coalescence of two stellar-mass black holes. The signal, GW151226, was observed by the twin detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) on December 26, 2015 at 03:38:53 UTC. The signal was initially identified within 70 s by an online matched-filter search targeting binary coalescences. Subsequent off-line analyses recovered GW151226 with a network signal-to-noise ratio of 13 and a significance greater than 5σ. The signal persisted in the LIGO frequency band for approximately 1 s, increasing in frequency and amplitude over about 55 cycles from 35 to 450 Hz, and reached a peak gravitational strain of 3.4-0.9+0.7×10-22. The inferred source-frame initial black hole masses are 14.2-3.7+8.3M and 7.5-2.3+2.3M, and the final black hole mass is 20.8-1.7+6.1M. We find that at least one of the component black holes has spin greater than 0.2. This source is located at a luminosity distance of 440-190+180 Mpc corresponding to a redshift of 0.09-0.04+0.03. All uncertainties define a 90% credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.
| Original language | English |
|---|---|
| Article number | 241103 |
| Number of pages | 14 |
| Journal | Physical Review Letters |
| Volume | 116 |
| Issue number | 24 |
| DOIs | |
| Publication status | Published - 15 Jun 2016 |
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GW151226 : Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence. / LIGO Scientific Collaboration and Virgo Collaboration.
In: Physical Review Letters, Vol. 116, No. 24, 241103, 15.06.2016.Research output: Contribution to journal › Article › Research › peer-review
TY - JOUR
T1 - GW151226
T2 - Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence
AU - Ackley, K
AU - Ashton, G
AU - Lasky, P D
AU - Levin, Y
AU - Qiu, S
AU - Sammut, L
AU - Thrane, E
AU - Zhu, Xingjiang
AU - LIGO Scientific Collaboration and Virgo Collaboration
AU - Mandel, Ilya
PY - 2016/6/15
Y1 - 2016/6/15
N2 - We report the observation of a gravitational-wave signal produced by the coalescence of two stellar-mass black holes. The signal, GW151226, was observed by the twin detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) on December 26, 2015 at 03:38:53 UTC. The signal was initially identified within 70 s by an online matched-filter search targeting binary coalescences. Subsequent off-line analyses recovered GW151226 with a network signal-to-noise ratio of 13 and a significance greater than 5σ. The signal persisted in the LIGO frequency band for approximately 1 s, increasing in frequency and amplitude over about 55 cycles from 35 to 450 Hz, and reached a peak gravitational strain of 3.4-0.9+0.7×10-22. The inferred source-frame initial black hole masses are 14.2-3.7+8.3M and 7.5-2.3+2.3M, and the final black hole mass is 20.8-1.7+6.1M. We find that at least one of the component black holes has spin greater than 0.2. This source is located at a luminosity distance of 440-190+180 Mpc corresponding to a redshift of 0.09-0.04+0.03. All uncertainties define a 90% credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.
AB - We report the observation of a gravitational-wave signal produced by the coalescence of two stellar-mass black holes. The signal, GW151226, was observed by the twin detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) on December 26, 2015 at 03:38:53 UTC. The signal was initially identified within 70 s by an online matched-filter search targeting binary coalescences. Subsequent off-line analyses recovered GW151226 with a network signal-to-noise ratio of 13 and a significance greater than 5σ. The signal persisted in the LIGO frequency band for approximately 1 s, increasing in frequency and amplitude over about 55 cycles from 35 to 450 Hz, and reached a peak gravitational strain of 3.4-0.9+0.7×10-22. The inferred source-frame initial black hole masses are 14.2-3.7+8.3M and 7.5-2.3+2.3M, and the final black hole mass is 20.8-1.7+6.1M. We find that at least one of the component black holes has spin greater than 0.2. This source is located at a luminosity distance of 440-190+180 Mpc corresponding to a redshift of 0.09-0.04+0.03. All uncertainties define a 90% credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.
UR - http://www.scopus.com/inward/record.url?scp=84975517093&partnerID=8YFLogxK
U2 - 10.1103/PhysRevLett.116.241103
DO - 10.1103/PhysRevLett.116.241103
M3 - Article
AN - SCOPUS:84975517093
VL - 116
JO - Physical Review Letters
JF - Physical Review Letters
SN - 0031-9007
IS - 24
M1 - 241103
ER -