List of gravitational wave observations

The first measurement of a gravitational wave event

This is a list of observed gravitational wave events. Observation of gravitational waves, which commenced with the detection of an event by LIGO in 2015, constitutes part of gravitational wave astronomy. LIGO has played a role in all subsequent detections to date, with Virgo joining in August 2017.

Nomenclature

Gravitational wave events are named starting with the prefix GW. The next two numbers indicate the year the event was observed, the middle two numbers are the month of observation and the final two numbers are the day of the month on which the event was observed. This is similar to the systematic naming for other kinds of astronomical event observations, such as those of gamma-ray bursts. Probable detections that are not confidently identified as gravitational wave events are designated LVT ("LIGO-Virgo trigger").

List of gravitational wave events

List of binary merger events
GW event	Detection time (UTC)	Date published	Location area^{[n 1]} (deg²)	Luminosity distance (Mpc)^{[n 2]}	Energy radiated (c²M_☉)^{[n 3]}	Chirp mass (M_☉)^{[n 4]}	Primary		Secondary		Remnant			Notes	Ref
GW event	Detection time (UTC)	Date published	Location area^{[n 1]} (deg²)	Luminosity distance (Mpc)^{[n 2]}	Energy radiated (c²M_☉)^{[n 3]}	Chirp mass (M_☉)^{[n 4]}	Type	Mass (M_☉)	Type	Mass (M_☉)	Type	Mass (M_☉)	Spin^{[n 5]}	Notes	Ref
GW150914	2015-09-14 09:50:45	2016-02-11	7002600000000000000♠600; mostly to the south	7002440000000000000♠440+160 −180	7000300000000000000♠3.0+0.5 −0.5	7001282000000000000♠28.2+1.8 −1.7	BH ^{[n 6]}	7001354000000000000♠35.4+5.0 −3.4	BH ^{[n 7]}	7001298000000000000♠29.8+3.3 −4.3	BH	7001622000000000000♠62.2+3.7 −3.4	6999680000000000000♠0.68+0.05 −0.06	First GW detection; first BH merger observed; largest progenitor masses to date	^[3]^[4]^[2]
LVT151012	2015-10-12 09∶54:43	2016-06-15	7003160000000000000♠1600	7003100000000000000♠1000+500 −500	7000150000000000000♠1.5+0.3 −0.4	7001151000000000000♠15.1+1.4 −1.1	BH	7001230000000000000♠23+18 −6	BH	7001130000000000000♠13+4 −5	BH	7001350000000000000♠35+14 −4	6999660000000000000♠0.66+0.09 −0.10	Not significant enough to confirm (~13% chance of being noise)	^[5]
GW151226	2015-12-26 03:38:53	2016-06-15	7002850000000000000♠850	7002440000000000000♠440+180 −190	7000100000000000000♠1.0+0.1 −0.2	7000890000000000000♠8.9+0.3 −0.3	BH	7001142000000000000♠14.2+8.3 −3.7	BH	7000750000000000000♠7.5+2.3 −2.3	BH	7001208000000000000♠20.8+6.1 −1.7	6999740000000000000♠0.74+0.06 −0.06		^[6]^[7]
GW170104	2017-01-04 10∶11:58	2017-06-01	7003120000000000000♠1200	7002880000000000000♠880+450 −390	7000200000000000000♠2.0+0.6 −0.7	7001211000000000000♠21.1+2.4 −2.7	BH	7001312000000000000♠31.2+8.4 −6.0	BH	7001194000000000000♠19.4+5.3 −5.9	BH	7001487000000000000♠48.7+5.7 −4.6	6999640000000000000♠0.64+0.09 −0.20	Farthest confirmed event to date	^[8]^[9]
GW170608	2017-06-08 02:01:16	2017-11-16	7002520000000000000♠520; to the north	7002340000000000000♠340+140 −140	6999850000000000000♠0.85+0.07 −0.17	7000790000000000000♠7.9+0.2 −0.2	BH	7001120000000000000♠12+7 −2	BH	7000700000000000000♠7+2 −2	BH	7001180000000000000♠18.0+4.8 −0.9	6999690000000000000♠0.69+0.04 −0.05	Smallest BH progenitor masses to date	^[10]
GW170814	2017-08-14 10∶30:43	2017-09-27	7001600000000000000♠60; towards Eridanus	7002540000000000000♠540+130 −210	7000270000000000000♠2.7+0.4 −0.3	7001241000000000000♠24.1+1.4 −1.1	BH	7001305000000000000♠30.5+5.7 −3.0	BH	7001253000000000000♠25.3+2.8 −4.2	BH	7001532000000000000♠53.2+3.2 −2.5	6999700000000000000♠0.70+0.07 −0.05	First detection by three observatories; first measurement of polarization	^[11]^[12]
GW170817	2017-08-17 12∶41:04	2017-10-16	7001280000000000000♠28; NGC 4993	7001400000000000000♠40+8 −14	> 0.025	7000118800000000000♠1.188+0.004 −0.002	NS	1.36 - 1.60^{[n 8]}	NS	1.17 - 1.36^{[n 9]}	BH ^{[n 10]}	< 7000274000000000000♠2.74+0.04 −0.01 ^{[n 11]}		First NS merger observed in GW; first detection of EM counterpart (GRB 170817A; AT 2017gfo); nearest event to date	^[1]^[15]^[16]

Notes

↑ The area of the sky within which it was possible to localize the source.
↑ 1 Mpc is approximately 3.26 Mly.
↑ c²M_☉ is about 1.8×10³ foe; 1.8×10⁴⁷ J; 1.8×10⁵⁴ erg; 4.3×10⁴⁶ cal; 1.7×10⁴⁴ BTU; 5.0×10⁴⁰ kWh, or 4.3×10³⁷ tonnes of TNT.
↑ The chirp mass, very roughly similar to the geometric mean of the binary's masses, is the binary parameter most relevant to the evolution of the inspiral gravitational waveform, and thus is the mass that can be measured most accurately.
↑ Values of the dimensionless spin parameter c J/G M² for black holes range from zero to a maximum of one. The macroscopic properties of an isolated astrophysical (uncharged) black hole are fully determined by its mass and spin. Values for other objects can potentially exceed one. The largest value known for a neutron star is ≤ 0.4, and commonly used equations of state would limit that value to < 0.7.^[1]
↑ Spin estimate is 6999260000000000000♠0.26+0.52
−0.24.^[2]
↑ Spin estimate is 6999320000000000000♠0.32+0.54
−0.29.^[2]
↑ Mass based on presumption of low spin (constrained to match observations of binary neutron stars extrapolated to time of merger); the estimate without this assumption is 1.36 - 2.26 M_☉.
↑ Mass based on presumption of low spin; the estimate without this assumption is 0.86 - 1.36 M_☉.
↑ A hypermassive neutron star is believed to have formed initially and then collapsed into a black hole within milliseconds, as evidenced by the large amount of ejecta (much of which would have been swallowed by an immediately forming black hole) and the lack of evidence for emissions being powered by neutron star spin-down, which would occur for longer-surviving neutron stars.^[13]
↑ Based on total mass prior to merger for the presumption of low spin; the mass estimate for the binary without this assumption is 7000282000000000000♠2.82+0.47
−0.09 M_☉. Besides the loss of mass due to GW emission that occurred during the merger, the event is thought to have ejected 0.05 ±0.02 M_☉ of material.^[14]

References

1 2 Abbott, B. P.; et al. (LIGO Scientific Collaboration & Virgo Collaboration) (16 October 2017). "GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral". Physical Review Letters. 119 (16). arXiv:1710.05832. Bibcode:2017PhRvL.119p1101A. doi:10.1103/PhysRevLett.119.161101.
1 2 3 The LIGO Scientific Collaboration and The Virgo Collaboration (3 June 2016). "An improved analysis of GW150914 using a fully spin-precessing waveform model". arXiv:1606.01210 [gr-qc]. Bibcode:2016PhRvX...6d1014A. doi:10.1103/PhysRevX.6.041014. Cite uses deprecated parameter |class= (help)
↑ Abbott, B. P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (11 February 2016). "Observation of Gravitational Waves from a Binary Black Hole Merger". Physical Review Letters. 116 (6): 061102. arXiv:1602.03837. Bibcode:2016PhRvL.116f1102A. doi:10.1103/PhysRevLett.116.061102. PMID 26918975.
↑ Tushna Commissariat (11 February 2016). "LIGO detects first ever gravitational waves – from two merging black holes". Physics World.
↑ Abbott, B. P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (21 October 2016). "Binary Black Hole Mergers in the first Advanced LIGO Observing Run". Physical Review X. 6: 041015. arXiv:1606.04856. Bibcode:2016PhRvX...6d1015A. doi:10.1103/PhysRevX.6.041015.
↑ Abbott, B. P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (15 June 2016). "GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence". Physical Review Letters. 116 (24): 241103. arXiv:1606.04855. Bibcode:2016PhRvL.116x1103A. doi:10.1103/PhysRevLett.116.241103. PMID 27367379.
↑ Nemiroff, R.; Bonnell, J., eds. (15 June 2016). "GW151226: A Second Confirmed Source of Gravitational Radiation". Astronomy Picture of the Day. NASA.
↑ Abbott, B. P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (1 June 2017). "GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2". Physical Review Letters. 118: 221101. arXiv:1706.01812. Bibcode:2017PhRvL.118v1101A. doi:10.1103/PhysRevLett.118.221101.
↑ Overbye, Dennis (1 June 2017). "Gravitational Waves Felt From Black-Hole Merger 3 Billion Light-Years Away". New York Times. Retrieved 1 June 2017.
↑ Abbott, Benjamin P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (18 December 2017). "GW170608: Observation of a 19-solar-mass Binary Black Hole Coalescence". The Astrophysical Journal Letters. 851 (2). arXiv:1711.05578. Bibcode:2017ApJ...851L..35A. doi:10.3847/2041-8213/aa9f0c.
↑ Abbott, Benjamin P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (2017-10-06). "GW170814: A three-detector observation of gravitational waves from a binary black hole coalescence". Phys. Rev. Lett. 119 (14): 141101. arXiv:1709.09660. Bibcode:2017PhRvL.119n1101A. doi:10.1103/PhysRevLett.119.141101. Lay summary (PDF).
↑ Overbye, Dennis (27 September 2017). "New Gravitational Wave Detection From Colliding Black Holes". The New York Times. Retrieved 28 September 2017.
↑ Margalit, B.; Metzger, B. D. (2017-12-01). "Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817". The Astrophysical Journal. 850 (2): L19. arXiv:1710.05938. Bibcode:2017ApJ...850L..19M. doi:10.3847/2041-8213/aa991c.
↑ Drout, M. R.; Piro, A. L.; Shappee, B. J.; et al. (2017-10-16). "Light curves of the neutron star merger GW170817/SSS17a: Implications for r-process nucleosynthesis" (PDF). Science: eaaq0049. arXiv:1710.05443 [astro-ph.HE]. Bibcode:2017Sci...358.1570D. doi:10.1126/science.aaq0049. Cite uses deprecated parameter |class= (help)
↑ Abbott, B. P.; et al. (LIGO, Virgo and other collaborations) (October 2017). "Multi-messenger Observations of a Binary Neutron Star Merger" (PDF). The Astrophysical Journal. 848 (2): L12. arXiv:1710.05833 [astro-ph.HE]. Bibcode:2017ApJ...848L..12A. doi:10.3847/2041-8213/aa91c9. Cite uses deprecated parameter |class= (help)
↑ Cho, Adrian (16 October 2017). "Merging neutron stars generate gravitational waves and a celestial light show". Science. Retrieved 16 October 2017.

External links

"Detections". LIGO.

This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.

[1] The area of the sky within which it was possible to localize the source.

[2] 1 Mpc is approximately 3.26 Mly.

[3] ²M_☉ is about 1.8×10³ foe; 1.8×10⁴⁷ J; 1.8×10⁵⁴ erg; 4.3×10⁴⁶ cal; 1.7×10⁴⁴ BTU; 5.0×10⁴⁰ kWh, or 4.3×10³⁷ tonnes of TNT.

[4] The chirp mass, very roughly similar to the geometric mean of the binary's masses, is the binary parameter most relevant to the evolution of the inspiral gravitational waveform, and thus is the mass that can be measured most accurately.

[6] Values of the dimensionless spin parameter c J/G M² for black holes range from zero to a maximum of one. The macroscopic properties of an isolated astrophysical (uncharged) black hole are fully determined by its mass and spin. Values for other objects can potentially exceed one. The largest value known for a neutron star is ≤ 0.4, and commonly used equations of state would limit that value to < 0.7.^[1]

[8] Spin estimate is 6999260000000000000♠0.26+0.52
−0.24.^[2]

[9] Spin estimate is 6999320000000000000♠0.32+0.54
−0.29.^[2]

[20] Mass based on presumption of low spin (constrained to match observations of binary neutron stars extrapolated to time of merger); the estimate without this assumption is 1.36 - 2.26 M_☉.

[21] Mass based on presumption of low spin; the estimate without this assumption is 0.86 - 1.36 M_☉.

[23] A hypermassive neutron star is believed to have formed initially and then collapsed into a black hole within milliseconds, as evidenced by the large amount of ejecta (much of which would have been swallowed by an immediately forming black hole) and the lack of evidence for emissions being powered by neutron star spin-down, which would occur for longer-surviving neutron stars.^[13]

[25] Based on total mass prior to merger for the presumption of low spin; the mass estimate for the binary without this assumption is 7000282000000000000♠2.82+0.47
−0.09 M_☉. Besides the loss of mass due to GW emission that occurred during the merger, the event is thought to have ejected 0.05 ±0.02 M_☉ of material.^[14]

[PRL-171016-5] 1 2 Abbott, B. P.; et al. (LIGO Scientific Collaboration & Virgo Collaboration) (16 October 2017). "GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral". Physical Review Letters. 119 (16). arXiv:1710.05832. Bibcode:2017PhRvL.119p1101A. doi:10.1103/PhysRevLett.119.161101.

[Improved-7] 1 2 3 The LIGO Scientific Collaboration and The Virgo Collaboration (3 June 2016). "An improved analysis of GW150914 using a fully spin-precessing waveform model". arXiv:1606.01210 [gr-qc]. Bibcode:2016PhRvX...6d1014A. doi:10.1103/PhysRevX.6.041014. Cite uses deprecated parameter |class= (help)

[PRL116-061102-10] Abbott, B. P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (11 February 2016). "Observation of Gravitational Waves from a Binary Black Hole Merger". Physical Review Letters. 116 (6): 061102. arXiv:1602.03837. Bibcode:2016PhRvL.116f1102A. doi:10.1103/PhysRevLett.116.061102. PMID 26918975.

[PhysicsWorld-2016-02-11-11] Tushna Commissariat (11 February 2016). "LIGO detects first ever gravitational waves – from two merging black holes". Physics World.

[PRX2016-12] Abbott, B. P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (21 October 2016). "Binary Black Hole Mergers in the first Advanced LIGO Observing Run". Physical Review X. 6: 041015. arXiv:1606.04856. Bibcode:2016PhRvX...6d1015A. doi:10.1103/PhysRevX.6.041015.

[PRL116-241103-13] Abbott, B. P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (15 June 2016). "GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence". Physical Review Letters. 116 (24): 241103. arXiv:1606.04855. Bibcode:2016PhRvL.116x1103A. doi:10.1103/PhysRevLett.116.241103. PMID 27367379.

[APOD-2016-06-15-14] Nemiroff, R.; Bonnell, J., eds. (15 June 2016). "GW151226: A Second Confirmed Source of Gravitational Radiation". Astronomy Picture of the Day. NASA.

[15] Abbott, B. P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (1 June 2017). "GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2". Physical Review Letters. 118: 221101. arXiv:1706.01812. Bibcode:2017PhRvL.118v1101A. doi:10.1103/PhysRevLett.118.221101.

[NYT-20170601-16] Overbye, Dennis (1 June 2017). "Gravitational Waves Felt From Black-Hole Merger 3 Billion Light-Years Away". New York Times. Retrieved 1 June 2017.

[APJ-17] Abbott, Benjamin P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (18 December 2017). "GW170608: Observation of a 19-solar-mass Binary Black Hole Coalescence". The Astrophysical Journal Letters. 851 (2). arXiv:1711.05578. Bibcode:2017ApJ...851L..35A. doi:10.3847/2041-8213/aa9f0c.

[PRL-20171006-18] Abbott, Benjamin P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (2017-10-06). "GW170814: A three-detector observation of gravitational waves from a binary black hole coalescence". Phys. Rev. Lett. 119 (14): 141101. arXiv:1709.09660. Bibcode:2017PhRvL.119n1101A. doi:10.1103/PhysRevLett.119.141101. Lay summary (PDF).

[NYT-20170927-19] Overbye, Dennis (27 September 2017). "New Gravitational Wave Detection From Colliding Black Holes". The New York Times. Retrieved 28 September 2017.

[Margalit2017-22] Margalit, B.; Metzger, B. D. (2017-12-01). "Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817". The Astrophysical Journal. 850 (2): L19. arXiv:1710.05938. Bibcode:2017ApJ...850L..19M. doi:10.3847/2041-8213/aa991c.

[DroutPiro2017-24] Drout, M. R.; Piro, A. L.; Shappee, B. J.; et al. (2017-10-16). "Light curves of the neutron star merger GW170817/SSS17a: Implications for r-process nucleosynthesis" (PDF). Science: eaaq0049. arXiv:1710.05443 [astro-ph.HE]. Bibcode:2017Sci...358.1570D. doi:10.1126/science.aaq0049. Cite uses deprecated parameter |class= (help)

[ApJ2017.10-26] Abbott, B. P.; et al. (LIGO, Virgo and other collaborations) (October 2017). "Multi-messenger Observations of a Binary Neutron Star Merger" (PDF). The Astrophysical Journal. 848 (2): L12. arXiv:1710.05833 [astro-ph.HE]. Bibcode:2017ApJ...848L..12A. doi:10.3847/2041-8213/aa91c9. Cite uses deprecated parameter |class= (help)

[SM-20171016-27] Cho, Adrian (16 October 2017). "Merging neutron stars generate gravitational waves and a celestial light show". Science. Retrieved 16 October 2017.