GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence

B. P. Abbott; K. Gill; B. Hughey; M. J. Szczepańczyk; M. Zanolin; et al.

doi:10.1103/PhysRevLett.116.241103

GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence

B. P. Abbott, K. Gill, B. Hughey, M. J. Szczepańczyk, M. Zanolin, et al.

Physics & Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

<p> 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 5 σ. 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+0.7−0.9×10−22. The inferred source-frame initial black hole masses are 14.2+8.3−3.7M&odot; and 7.5+2.3−2.3M&odot; and the final black hole mass is 20.8+6.1−1.7M&odot;. 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+180−190 Mpc corresponding to a redshift 0.09+0.03−0.04. All uncertainties define a 90 % credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.</p>

Original language	American English
Journal	Physical Review Letters
Volume	116
DOIs	https://doi.org/10.1103/PhysRevLett.116.241103
State	Published - Jun 17 2016

Keywords

LIGO
gravitational waves

Disciplines

Astrophysics and Astronomy

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GW151226: Observation of Gravitational Waves from a 22-Solar-MassFinal published version, 1.13 MBLicense: CC BY

https://arxiv.org/pdf/1606.04855v1.pdf

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@article{e5fa9ca5a8dc4782b48d8f2409ce6d87,

title = "GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence",

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 5 σ. 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+0.7−0.9×10−22. The inferred source-frame initial black hole masses are 14.2+8.3−3.7M&odot; and 7.5+2.3−2.3M&odot; and the final black hole mass is 20.8+6.1−1.7M&odot;. 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+180−190 Mpc corresponding to a redshift 0.09+0.03−0.04. All uncertainties define a 90 % credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.",

keywords = "LIGO, gravitational waves",

author = "Abbott, {B. P.} and K. Gill and B. Hughey and Szczepa{\'n}czyk, {M. J.} and M. Zanolin and et al.",

year = "2016",

month = jun,

day = "17",

doi = "10.1103/PhysRevLett.116.241103",

language = "American English",

volume = "116",

journal = "Physical Review Letters",

issn = "1079-7114",

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T1 - GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence

AU - Abbott, B. P.

AU - Gill, K.

AU - Hughey, B.

AU - Szczepańczyk, M. J.

AU - Zanolin, M.

AU - al., et

PY - 2016/6/17

Y1 - 2016/6/17

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 5 σ. 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+0.7−0.9×10−22. The inferred source-frame initial black hole masses are 14.2+8.3−3.7M&odot; and 7.5+2.3−2.3M&odot; and the final black hole mass is 20.8+6.1−1.7M&odot;. 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+180−190 Mpc corresponding to a redshift 0.09+0.03−0.04. 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 5 σ. 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+0.7−0.9×10−22. The inferred source-frame initial black hole masses are 14.2+8.3−3.7M&odot; and 7.5+2.3−2.3M&odot; and the final black hole mass is 20.8+6.1−1.7M&odot;. 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+180−190 Mpc corresponding to a redshift 0.09+0.03−0.04. All uncertainties define a 90 % credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.

KW - LIGO

KW - gravitational waves

UR - https://commons.erau.edu/publication/231

U2 - 10.1103/PhysRevLett.116.241103

DO - 10.1103/PhysRevLett.116.241103

M3 - Article

SN - 1079-7114

VL - 116

JO - Physical Review Letters

JF - Physical Review Letters

ER -

GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence

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