List of gravitational wave observations

This page contains a list of observed/candidate gravitational wave events.

The first measurement of a gravitational wave event

Origin and nomenclature

Direct observation of gravitational waves, which commenced with the detection of an event by LIGO in 2015,[1] plays a key role in gravitational wave astronomy. LIGO has been involved in all subsequent detections to date, with Virgo joining in August 2017.[2]

Joint observation runs of LIGO and VIRGO, designated "O1, O2, etc." span many months, with months of maintenance and upgrades in-between designed to increase the instruments sensitivity and range. Within these run periods, the instruments are capable of detecting gravitational waves.

The first run, O1, ran from September 12, 2015, to January 19, 2016, and succeeded in its first gravitational wave detection. O2 ran for a greater duration, from November 30, 2016, to August 25, 2017.[3] O3 began on April 1, 2019, which was briefly suspended on September 30, 2019, for maintenance and upgrades, thus O3a. O3b marks resuming of the run and began on November 1, 2019. Due to the COVID-19 pandemic[4] O3 was forced to end prematurely.[5] O4 is planned to begin on May 24, 2023; initially planned for March, the project needed more time to stabilize the instruments.

The O4 observing run has been extended from one year to 18 months, following plans to make further upgrades for the O5 run.[2][6] Updated observing plans are published on the official website, containing the latest information on these runs.[6]

Gravitational wave events are named starting with the prefix GW, while observations that trigger an event alert but have not (yet) been confirmed are named starting with the prefix S.[7] Six digits then indicate the date of the event, with the two first digits representing the year, the two middle digits the month and two final digits the day of observation. 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"). Known gravitational wave events come from the merger of two black holes (BH), two neutron stars (NS), or a black hole and a neutron star (BHNS).[8][9] Some objects are in the mass gap between the largest predicted neutron star masses (Tolman–Oppenheimer–Volkoff limit) and the smallest known black holes.

List of gravitational wave events

Events from LIGO & Virgo

O1 & O2/2015-2017 events

O3/2019 Alerts

Confirmed events by distance
3 6 9 12 15 18 21 24 27 30 <100 Mpc 100-200 Mpc 200-500 Mpc 500-1000 Mpc 1-2 Gpc 2-5 Gpc 5+ Gpc BNS mergers NS-BH mergers mass gap BBH mergers

Initial objects by mass
5 10 15 20 25 30 35 40 45 50 1-2 M_☉ 2-3 M_☉ 3-5 M_☉ 5-10 M_☉ 10-20 M_☉ 20-30 M_☉ 30-40 M_☉ 40-50 M_☉ 50-60 M_☉ 60-70 M_☉ 70-80 M_☉ 80-90 M_☉ 90-100 M_☉ neutron star mass gap black hole

List of binary merger events[10][11]

GW event and time (UTC)[n 1]	Date published	Location area[n 2] (deg²)	Signal to Noise Ratio (SNR)	Luminosity distance (Mpc)[n 3]	Energy radiated/c² (M_☉) [n 4]	Chirp mass (M_☉) [n 5]	Effective spin[n 6]	Primary		Secondary		Remnant			Notes	Ref.
GW event and time (UTC)[n 1]	Date published	Location area[n 2] (deg²)	Signal to Noise Ratio (SNR)	Luminosity distance (Mpc)[n 3]	Energy radiated/c² (M_☉) [n 4]	Chirp mass (M_☉) [n 5]	Effective spin[n 6]	Type	Mass (M_☉)	Type	Mass (M_☉)	Type	Mass (M_☉)	Spin[n 7]	Notes	Ref.
GW150914 09:50:45	2016-02-11	179; mostly to the south	24.4+0.8 −0.8	430+150 −170	3.1+0.4 −0.4	28.6+1.6 −1.5	−0.01+0.12 −0.13	BH [n 8]	35.6+4.8 −3.0	BH [n 9]	30.6+3.0 −4.4	BH	63.1+3.3 −3.0	0.69+0.05 −0.04	First GW detection; first BH merger observed	[17][18][16]
GW151012 09:54:43	2016-06-15	1555	10.0+0.5 −0.5	1060+540 −480	1.5+0.5 −0.5	15.2+2.0 −1.1	0.04+0.28 −0.19	BH	23.3+14.0 −5.5	BH	13.6+4.1 −4.8	BH	35.7+9.9 −3.8	0.67+0.13 −0.11	Formerly candidate LVT151012; accepted as astrophysical since February 2019	[19][11][10]
GW151226 03:38:53	2016-06-15	1033	13.1+0.0 −1.2	440+180 −190	1.0+0.1 −0.2	8.9+0.3 −0.3	0.18+0.20 −0.12	BH	13.7+8.8 −3.2	BH	7.7+2.2 −2.6	BH	20.5+6.4 −1.5	0.74+0.07 −0.05		[20][21]
GW170104 10:11:58	2017-06-01	924	13.0+0.0 −0.0	960+430 −410	2.2+0.5 −0.5	21.5+2.1 −1.7	−0.04+0.17 −0.20	BH	31.0+7.2 −5.6	BH	20.1+4.9 −4.5	BH	49.1+5.2 −3.5	0.66+0.08 −0.10		[12][22]
GW170608 02:01:16	2017-11-16	396; to the north	14.9+0.5 −0.8	320+120 −110	0.9+0.0 −0.1	7.9+0.2 −0.2	0.03+0.19 −0.07	BH	10.9+5.3 −1.7	BH	7.6+1.3 −2.1	BH	17.8+3.2 −0.7	0.69+0.04 −0.04	Smallest BH progenitor masses to date	[23]
GW170729 18:56:29	2018-11-30	1033	10.2+0.6 −0.4	2750+1350 −1320	4.8+1.7 −1.7	35.7+6.5 −4.7	0.36+0.21 −0.25	BH	50.6+16.6 −10.2	BH	34.3+9.1 −10.1	BH	80.3+14.6 −10.2	0.81+0.07 −0.13	Largest progenitor masses until GW190521	[11]
GW170809 08:28:21	2018-11-30	340; towards Cetus	12.4+0.0 −0.2	990+320 −380	2.7+0.6 −0.6	25.0+2.1 −1.6	0.07+0.16 −0.16	BH	35.2+8.3 −6.0	BH	23.8+5.2 −5.1	BH	56.4+5.2 −3.7	0.70+0.08 −0.09		[11]
GW170814 10:30:43	2017-09-27	87; towards Eridanus	16.3+0.9 −0.4	580+160 −210	2.7+0.4 −0.3	24.2+1.4 −1.1	0.07+0.12 −0.11	BH	30.7+5.7 −3.0	BH	25.3+2.9 −4.1	BH	53.4+3.2 −2.4	0.72+0.07 −0.05	First announced detection by three observatories; first polarization measurement	[24][25]
GW170817 12:41:04	2017-10-16	16; NGC 4993	33.0+0.0 −2.1	40±10	≥ 0.04	1.186+0.001 −0.001	0.00+0.02 −0.01	NS	1.46+0.12 −0.10	NS	1.27+0.09 −0.09	NS [n 10]	≤ 2.8[n 11]	≤ 0.89	First NS merger observed in GW; first detection of EM counterpart (GRB 170817A; AT 2017gfo); nearest event to date	[15][28][29]
GW170818 02:25:09	2018-11-30	39; towards Pegasus	11.3+0.0 −0.0	1020+430 −360	2.7+0.5 −0.5	26.7+2.1 −1.7	−0.09+0.18 −0.21	BH	35.5+7.5 −4.7	BH	26.8+4.3 −5.2	BH	59.8+4.8 −3.8	0.67+0.07 −0.08		[11]
GW170823 13:13:58	2018-11-30	1651	11.1+0.4 −0.3	1850±840	3.3+0.9 −0.8	29.3+4.2 −3.2	0.08+0.20 −0.22	BH	39.6+10.0 −6.6	BH	29.4+6.3 −7.1	BH	65.6+9.4 −6.6	0.71+0.08 −0.10		[11]
GW190408_181802 2019-04-08	2020-10-27	140	15.3+0.2 −0.3	1580+400 −590		18.3+1.4 −1.2	−0.03+0.13 −0.19	BH	24.5+5.1 −3.4	BH	18.3+3.2 −3.5	BH	41.0+3.8 −2.7	0.67+0.06 −0.07	Originally designated S190408an.	[30]
GW190412 2019-04-12 05:30:44	2020-04-17	156; towards Virgo or Boötes	18.9+0.2 −0.3	730+140 −170		13.3+0.4 −0.3	0.25+0.08 −0.11	BH	29.7+5.0 −5.3	BH	8.4+1.8 −1.0	BH	37.0+4.1 −3.9	0.67+0.05 −0.07	First possible observation of a merger of two black holes of very different masses. Originally designated S190412m.	[31][32]
GW190413_052954 2019-04-13	2020-10-27	1400	8.9+0.4 −0.7	4100+2410 −1890		24.0+5.4 −3.7	0.01+0.29 −0.33	BH	33.4+12.4 −7.4	BH	23.4+6.7 −6.3	BH	54.3+12.4 −8.4	0.69+0.12 −0.13		[30]
GW190413_134308 2019-04-13	2020-10-27	520	10.0+0.4 −0.5	5150+2440 −2340		31.9+7.3 −4.6	−0.01+0.24 −0.28	BH	45.4+13.6 −9.6	BH	30.9+10.2 −9.6	BH	72.8+15.2 −10.3	0.69+0.10 −0.12		[30]
GW190421_213856 2019-04-21	2020-10-27	1000	10.7+0.2 −0.4	3150+1370 −1420		30.7+5.5 −6.6	−0.05+0.23 −0.26	BH	40.6+10.4 −6.6	BH	31.4+7.5 −8.2	BH	68.6+11.7 −8.1	0.68+0.10 −0.11	Originally designated S190421ar.	[30]
GW190424_180648 2019-04-24 18:06:48	2020-10-27	26000	10.4+0.2 −0.4	2550+1560 −1330		30.3+5.7 −4.2	0.15+0.22 −0.22	BH	39.5+10.9 −6.9	BH	31.0+7.4 −7.3	BH	67.1+12.5 −9.2	0.75+0.08 −0.09		[30]
GW190425 2019-04-25 08:18:05	2020-01-06	28; towards Hercules[33]	12.4+0.3 −0.4	159+69 −72		1.44+0.02 −0.02	0.012+0.01 −0.01	NS	1.60 - 1.87	NS	1.46 - 1.69	?			Originally designated S190425z (z:26th trigger\|UTC day), this trigger was detected by a single LIGO instrument (of three LVC stations), and is considered by some scientists to have been confirmed as a binary neutron star merger.[34] It was published in 2020 that a gamma-ray burst was detected (GRB 190425) ~0.5 seconds after the LIGO trigger, lasting 6 seconds and bearing similarities to GRB170817 (such as weakness [most power in sub-100 keV, or soft X-rays) bands], elevated energetic photon background levels [signal exceeding background by less than a factor of 2], and similar differences from other transients classified as short GRBs). Confidence was established for interpretation of a set of peaks through a control interval of only 2 days prior to the LIGO-Livingston trigger in INTEGRAL Electronic anticoincidence, could not be corroborated by other instruments and wasn't initially noted as a significant event. Non-detection in other instruments may be a consequence of an Earth-occulted source as the Fermi telescope attempted follow-up.[33]	[35][36]
GW190426_152155 2019-04-26 15:21:55	2020-10-27	1300	8.7+0.5 −0.6	370+180 −160		2.41+0.08 −0.08	−0.03+0.32 −0.30	?	5.7+3.9 −2.3	NS	1.5+0.8 −0.5	?			The primary object, being between 3.4 and 9.6 solar masses, is either a black hole or an object in the mass gap. Originally designated S230426c.	[30]
GW190503_185404 2019-05-03 18:54:04	2020-10-27	94; towards Columba, Pictor, or Puppis	12.4+0.2 −0.3	1450+690 −630		30.2+4.2 −4.2	−0.03+0.20 −0.26	BH	43.3+9.1 −8.2	BH	28.4+7.7 −8.0	BH	68.6+8.8 −7.7	0.66+0.09 −0.12	Originally designated S230503bf.	[30]
GW190512_180714 2019-05-12 18:07:14	2020-10-27	220; towards Scorpius or Ophiuchus	12.2+0.2 −0.4	1430+550 −550		14.6+1.3 −1.0	0.03+0.12 −0.13	BH	23.3+5.3 −3.8	BH	12.6+3.6 −2.5	BH	34.5+3.8 −3.5	0.65+0.07 −0.07	Originally designated S230512at.	[30]
GW190513_205428 2019-05-13 20:54:28	2020-10-27	520; towards Sagittarius, Capricornus, Perseus, or Camelopardalis	12.9+0.3 −0.4	2060+880 −800		21.6+3.8 −1.9	0.11+0.28 −0.17	BH	35.7+9.5 −9.2	BH	18.0+7.7 −4.2	BH	51.6+8.2 −5.8	0.68+0.14 −0.12	Originally designated S230513bm.	[30]
GW190514_065416 2019-05-14 06:54:16	2020-10-27	3000	8.2+0.3 −0.6	4100+2700 −2200		28.5+7.9 −4.8	−0.19+0.29 −0.32	BH	39.0+14.7 −8.2	BH	28.4+9.3 −8.8	BH	65+18 −10	0.63+0.11 −0.15		[30]
GW190517_055101 2019-05-17 06:54:16	2020-10-27	470	10.7+0.4 −0.6	1860+1620 −840		26.6+4.0 −4.0	0.52+0.19 −0.19	BH	37.4+11.7 −7.6	BH	25.3+7.0 −7.3	BH	59.3+9.1 −8.9	0.87+0.05 −0.07	Originally designated S190517h.	[30]
GW190519_153544 2019-05-19 15:35:44	2020-10-27	860	15.6+0.2 −0.3	2530+1830 −920		44.5+6.4 −7.1	0.31+0.20 −0.22	BH	66+11 −12	BH	41+11 −11	BH	101+12 −14	0.79+0.07 −0.13	Originally designated S190519bj.	[30]
GW190521 2019-05-21 03:02:29	2020-09-02	765; towards Coma Berenices, Canes Venatici, or Phoenix	14.2+0.3 −0.3	5300+2400 −2600	7.6+2.2 −1.9	64+13 −8	0.08+0.27 −0.36	BH	85+21 −14	BH	66+17 −18	BH	142+28 −16	0.72+0.09 −0.12	Originally designated S190521g. Largest progenitor masses to date.	[37][38]
GW190521_074359 2019-05-21 07:43:59	2020-10-27	550	25.8+0.1 −0.2	1240+400 −570		32.1+3.2 −2.5	0.09+0.10 −0.13	BH	42.2+5.9 −4.8	BH	32.8+5.4 −6.4	BH	71.0+6.5 −4.4	0.72+0.05 −0.07	Originally designated S190521r.	[30]
GW190527_092055 2019-05-27 09:20:55	2020-10-27	3700	8.1+0.3 −0.9	2500+2500 −1200		24.3+9.2 −4.1	0.11+0.28 −0.28	BH	36.5+16.4 −9.0	BH	22.6+10.5 −8.1	BH	56.4+20.2 −9.3	0.71+0.12 −0.16		[30]
GW190602_175927 2019-06-02 17:59:27	2020-10-27	690	12.8+0.2 −0.3	2700+1800 −1100		49.1+9.1 −8.5	0.07+0.25 −0.24	BH	69+16 −13	BH	48+14 −17	BH	111+18 −15	0.70+0.10 −0.14	Originally designated S190602aq.	[30]
GW190620_030421 2019-06-20 03:04:21	2020-10-27	7200	12.1+0.3 −0.4	2800+1700 −1300		38.3+8.3 −6.5	0.33+0.22 −0.25	BH	57+16 −13	BH	36+12 −12	BH	87+17 −12	0.79+0.08 −0.15		[30]
GW190630_185205 2019-06-30 18:52:05	2020-10-27	1200	15.6+0.2 −0.3	890+560 −370		24.9+2.1 −2.1	0.10+0.12 −0.13	BH	35.1+6.9 −5.6	BH	23.7+5.2 −5.1	BH	56.4+4.4 −4.6	0.70+0.05 −0.07	Originally designated S190630ag.	[30]
GW190701_203306 2019-07-01 20:33:06	2020-10-27	46; towards Eridanus or Cetus	11.3+0.2 −0.3	2060+760 −730		40.3+5.4 −4.9	−0.07+0.23 −0.29	BH	53.9+11.8 −8.0	BH	40.8+8.7 −12.0	BH	90.2+11.3 −8.9	0.66+0.09 −0.13	Originally designated S190701ah.	[30]
GW190706_222641 2019-07-06 22:26:41	2020-10-27	650	12.6+0.2 −0.4	4400+2600 −1900		42.7+10.0 −7.0	0.28+0.26 −0.29	BH	67+15 −16	BH	38+15 −13	BH	99+18 −14	0.78+0.09 −0.18	Originally designated S190706ai.	[30]
GW190707_093326 2019-07-07 09:33:26	2020-10-27	1300	13.3+0.2 −0.4	770+380 −270		8.5+0.7 −0.6	−0.05+0.10 −0.08	BH	11.6+3.3 −1.7	BH	8.4+1.4 −1.7	BH	19.2+1.9 −1.3	0.66+0.03 −0.04	Originally designated S190707q.	[30]
GW190708_232457 2019-07-08 23:24:57	2020-10-27	14000	13.1+0.2 −0.3	880+330 −390		13.2+0.9 −0.6	0.02+0.08 −0.10	BH	17.6+4.7 −2.3	BH	13.2+2.0 −2.7	BH	29.5+2.5 −1.8	0.69+0.04 −0.04		[30]
GW190719_215514 2019-07-09 21:55:14	2020-10-27	2900	8.3+0.3 −0.8	3900+2600 −2000		23.5+6.5 −4.0	0.32+0.29 −0.31	BH	37+18 −10	BH	20.8+9.0 −7.2	BH	55+17 −10	0.78+0.11 −0.17		[30]
GW190720_000836 2019-07-20 00:08:36	2020-10-27	460; mostly towards Cygnus	11.0+0.3 −0.7	790+690 −320		8.9+0.5 −0.8	0.18+0.14 −0.12	BH	13.4+6.7 −3.0	BH	7.8+2.3 −2.2	BH	20.4+4.5 −2.2	0.72+0.06 −0.05	Originally designated S190720a.	[30]
GW190727_060333 2019-07-27 06:03:33	2020-10-27	830	11.9+0.3 −0.5	790+690 −320		28.6+5.3 −3.7	0.11+0.26 −0.25	BH	38.0+9.5 −6.2	BH	29.4+7.1 −8.4	BH	63.8+10.9 −7.5	0.73+0.10 −0.10	Originally designated S190727h.	[30]
GW190728_064510 2019-07-28 06:45:10	2020-10-27	400	13.0+0.2 −0.4	870+260 −370		8.6+0.5 −0.3	0.12+0.20 −0.07	BH	12.3+7.2 −2.2	BH	8.1+1.7 −2.6	BH	19.6+4.7 −1.3	0.71+0.04 −0.04	Originally designated S190728q.	[30]
GW190731_140936 2019-07-31 14:09:36	2020-10-27	3400	8.7+0.2 −0.5	3300+2400 −1700		29.5+7.1 −5.2	0.06+0.24 −0.24	BH	41.5+12.2 −9.0	BH	28.8+9.7 −9.5	BH	67+15 −11	0.70+0.10 −0.13		[30]
GW190803_022701 2019-08-03 02:27:01	2020-10-27	1500	8.6+0.3 −0.5	3300+2000 −1600		27.3+5.7 −4.1	−0.03+0.24 −0.27	BH	37.3+10.6 −7.0	BH	27.3+7.8 −8.2	BH	61.7+11.8 −8.5	0.68+0.10 −0.11		[30]
GW190814 2019-08-14 21:11:18	2020-06-23	18.5; towards Cetus or Sculptor	24.9+0.1 −0.2	241+41 −45		6.09+0.06 −0.06	−0.002+0.06 −0.061	BH	23.2+1.1 −1.0	?	2.59+0.08 −0.09	BH	25.6+1.1 −0.9	0.28+0.02 −0.02	No optical counterpart was discovered despite an extensive search of the probability region. The mass of the lighter component is estimated to be 2.6 times the mass of the Sun, placing it in the mass gap between neutron stars and black holes.[39]	[40][41][42][43][44] [45][46][47][48]
GW190828_063405 2019-08-28 06:34:05	2020-10-27	520	16.2+0.2 −0.3	2130+660 −930		25.0+3.4 −2.1	0.19+0.15 −0.16	BH	32.1+5.8 −4.0	BH	26.2+4.6 −4.8	BH	54.9+7.2 −4.3	0.75+0.06 −0.07	Originally designated S190828j.	[30]
GW190828_065509 2019-08-28 06:55:09	2020-10-27	660	10.0+0.3 −0.5	1600+620 −600		13.3+1.2 −1.0	0.08+0.16 −0.16	BH	24.1+7.0 −7.2	BH	10.2+3.6 −2.1	BH	33.1+5.5 −4.5	0.65+0.08 −0.08	Originally designated S190828l.	[30]
GW190909_114149 2019-09-09 11:41:49	2020-10-27	4700	8.1+0.4 −0.6	3800+3300 −2200		30.9+17.2 −7.5	−0.06+0.37 −0.37	BH	46+53 −13	BH	28+13 −13	BH	72+55 −17	0.66+0.15 −0.20		[30]
GW190910_112807 2019-09-10 11:28:07	2020-10-27	11000	14.1+0.2 −0.3	1460+1030 −580		34.3+4.1 −4.1	0.02+0.18 −0.18	BH	43.9+7.6 −6.1	BH	35.6+6.3 −7.2	BH	75.8+8.5 −8.6	0.70+0.08 −0.07		[30]
GW190915_235702 2019-09-15 23:57:02	2020-10-27	400; towards Coma Berenices, Canes Venatici, or Ursa Major	13.6+0.2 −0.3	1620+710 −610		25.3+3.2 −2.7	0.02+0.20 −0.25	BH	35.3+9.5 −6.4	BH	24.4+5.6 −6.1	BH	57.2+7.1 −6.0	0.70+0.09 −0.11	Originally designated S230915ak.	[30]
GW190924_021846 2019-09-24 02:18:46	2020-10-27	360; towards Hydra or Cancer	11.5+0.3 −0.4	570+220 −220		5.8+0.2 −0.2	0.03+0.30 −0.09	BH	8.9+7.0 −2.0	?	5.0+1.4 −1.9	BH	13.3+5.2 −1.0	0.67+0.05 −0.05	The secondary component, being between 3.1 and 6.4 solar masses, is either a black hole or an object in the mass gap. Originally designated S230924h.	[30]
GW190929_012149 2019-09-29 01:21:49	2020-10-27	2200	10.1+0.6 −0.8	2100+3700 −1100		35.8+14.9 −8.2	0.01+0.34 −0.33	BH	81+33 −33	BH	24+19 −11	BH	102+34 −25	0.66+0.20 −0.31		[30]
GW190930_133541 2019-09-30 13:35:41	2020-10-27	1700	9.5+0.3 −0.5	760+360 −320		8.5+0.5 −0.5	0.14+0.31 −0.15	BH	12.3+12.4 −2.3	?	7.8+1.7 −3.3	BH	19.4+9.2 −1.5	0.72+0.07 −0.06	The secondary component, being between 4.5 and 9.5 solar masses, is either a black hole or an object in the mass gap. Originally designated S190930s.	[30]
GW191103 2019-11-03 01:25:49	2021-11-17	2500	8.9+0.3 −0.5	990+500 −470		8.34+0.66 −0.57	0.21+0.16 −0.10	BH	11.8+6.2 −2.2	BH	7.9+1.7 −2.4	BH	19.0+3.8 −1.7	0.75+0.06 −0.05		[49]
GW191105 2019-11-05 14:35:21	2021-11-17	640	9.7+0.3 −0.5	1150+430 −480		7.82+0.61 −0.45	−0.02+0.13 −0.09	BH	10.7+3.7 −1.6	BH	7.7+1.4 −1.9	BH	17.6+2.1 −1.2	0.67+0.04 −0.05	Originally designated S191105e.	[49]
GW191109 2019-11-09 01:07:17	2021-11-17	1600	17.3+0.5 −0.5	1290+1130 −650		47.5+9.6 −7.5	−0.29+0.42 −0.31	BH	65+11 −11	BH	47+15 −13	BH	107+18 −15	0.61+0.18 −0.19	Originally designated S191109d.	[49]
GW191113 2019-11-13 07:17:53	2021-11-17	3600	7.9+0.5 −1.1	1290+1130 −650		10.7+1.1 −1.0	0.00+0.37 −0.29	BH	29+12 −14	BH	5.9+4.4 −1.3	BH	34+11 −10	0.45+0.33 −0.11		[49]
GW191126 2019-11-26 11:52:59	2021-11-17	1400	8.3+0.2 −0.5	1620+740 −740		8.65+0.95 −0.71	0.21+0.15 −0.11	BH	12.1+5.5 −2.2	BH	8.3+1.9 −2.4	BH	19.6+3.5 −2.0	0.75+0.06 −0.05		[49]
GW191127 2019-11-27 05:02:27	2021-11-17	980	9.2+0.7 −0.6	3400+3100 −1900		29.9+11.7 −9.1	0.18+0.34 −0.36	BH	53+47 −20	BH	24+17 −14	BH	76+31 −29	0.75+0.13 −0.29		[49]
GW191129 2019-11-29 13:40:29	2021-11-17	850	13.1+0.2 −0.3	790+260 −330		7.31+0.43 −0.28	0.06+0.18 −0.06	BH	10.7+4.1 −2.1	BH	6.7+1.5 −1.7	BH	16.8+2.5 −1.2	0.69+0.03 −0.05	Originally designated S191129u.	[49]
GW191204_110529 2019-12-04 11:05:29	2021-11-17	3700	8.8+0.4 −0.6	1800+1700 −1100		19.8+3.6 −3.3	0.05+0.26 −0.27	BH	27.3+11.0 −6.0	BH	19.3+5.6 −6.0	BH	45.0+8.6 −7.6	0.71+0.12 −0.11		[49]
GW191204_171526 2019-12-04 17:15:26	2021-11-17	350; towards Pictor, Caelum, or Eridanus	17.5+0.2 −0.2	650+190 −250		8.55+0.38 −0.27	0.16+0.08 −0.05	BH	11.9+3.3 −1.8	BH	8.2+1.4 −1.6	BH	19.21+1.79 −0.95	0.73+0.03 −0.03	Originally designated S191204r.	[49]
GW191215 2019-12-15 22:30:52	2021-11-17	530	11.2+0.3 −0.4	1930+890 −860		18.4+2.2 −1.7	−0.04+0.17 −0.21	BH	24.9+7.1 −4.1	BH	18.1+3.8 −4.1	BH	41.4+5.1 −4.1	0.68+0.07 −0.07	Originally designated S191215w.	[49]
GW191216 2019-12-16 21:33:38	2021-11-17	490	18.6+0.2 −0.2	340+120 −130		8.33+0.22 −0.19	0.11+0.13 −0.06	BH	12.1+4.6 −2.3	BH	7.7+1.6 −1.9	BH	18.87+2.80 −0.94	0.70+0.03 −0.04	Originally designated S191216ap.	[49]
GW191219 2019-12-19 16:31:20	2021-11-17	1500	9.1+0.5 −0.8	550+250 −160		4.32+0.12 −0.17	0.00+0.07 −0.09	BH	31.1+2.2 −2.8	NS	1.17+0.07 −0.06	BH	32.2+2.2 −2.7	0.14+0.06 −0.06	The event is unconfirmed due to difficulty accurately modelling the extreme mass ratio.	[49]
GW191222 2019-12-22 03:35:37	2021-11-17	2000	12.5+0.2 −0.3	3000+1700 −1700		33.8+7.1 −5.0	−0.04+0.20 −0.25	BH	45.1+10.9 −8.0	BH	34.7+9.3 −10.5	BH	75.5+15.3 −9.9	0.67+0.08 −0.11	Originally designated S191222n.	[49]
GW191230 2019-12-30 18:04:58	2021-11-17	1100	10.4+0.3 −0.4	4300+2100 −1900		36.5+8.2 −5.6	−0.05+0.26 −0.31	BH	49.4+14.0 −9.6	BH	37+11 −12	BH	82+17 −11	0.68+0.11 −0.13		[49]
GW200105 2020-01-05 16:24:26	2021-06-29	7200	13.7+0.2 −0.4	280±110		3.41+0.08 −0.07	−0.01+0.11 −0.15	BH	8.9+1.2 −1.5	NS	1.9+0.3 −0.2	BH	10.4+2.7 −2.0	0.43+0.04 −0.03	First event confirmed to be a black hole and neutron star merger. Originally designated S200105ae.	[50][51]
GW200112 2020-01-12 15:58:38	2021-11-17	4300	19.8+0.1 −0.2	1250+430 −460		27.4+2.6 −2.1	0.06+0.15 −0.15	BH	35.6+6.7 −4.5	BH	28.3+4.4 −5.9	BH	60.8+5.3 −4.3	0.71+0.06 −0.06	Originally designated S200112r.	[49]
GW200114 2020-01-14 02:08:08	2022-08-18	403; towards Gemini, Orion, or Eridanus		1250+1500 −400		68+6 −4	−0.75+0.50 −0.15	BH	78+10 −10	BH	70+10 −10	BH	140+15 −15		Originally designated S200114f. The event was initially published as an unmodeled gravitational wave burst, and different studies have offered conflicting interpretations. One study suggested it was a nearby high-mass black hole merger with component masses of 118+10 −12 and 89+18 −8 M_sun which was poorly modeled because of its high mass.[52] Another study interpreted it as a somewhat smaller black hole merger taking place at the same time as a detector glitch.[53] Both studies conclude the signal is most likely a real event, and the latter model is included in the table.	[52][53]
GW200115 2020-01-15 04:23:09	2021-06-29	600	11.3+0.3 −0.5	300+150 −100		2.42+0.05 −0.07	−0.19+0.23 −0.35	BH	5.7+1.8 −2.1	NS	1.5+0.7 −0.3	BH	7.8+1.4 −1.6	0.38+0.04 −0.03	Second event confirmed to be a black hole and neutron star merger. Originally designated S200115j.	[50][54]
GW200128 2020-01-28 02:20:11	2021-11-17	2600	10.6+0.3 −0.4	3400+2100 −1800		32.0+7.5 −5.5	0.12+0.24 −0.25	BH	42.2+11.6 −8.1	BH	32.6+9.5 −9.2	BH	71+16 −11	0.74+0.10 −0.10	Originally designated S200128d.	[49]
GW200129 2020-01-29 06:54:58	2021-11-17	130; towards Equuleus, Delphinus, or Vulpecula	26.8+0.2 −0.2	900+290 −380		27.2+2.1 −2.3	0.11+0.11 −0.16	BH	34.5+9.9 −3.2	BH	28.9+3.4 −9.3	BH	60.3+4.0 −3.3	0.73+0.06 −0.05	Originally designated S200129m.	[49]
GW200202 2020-02-02 15:43:12	2021-11-17	170	10.8+0.2 −0.4	410+150 −160		7.49+0.24 −0.20	0.04+0.13 −0.06	BH	10.1+3.5 −1.4	BH	7.3+1.1 −1.7	BH	16.76+1.87 −0.66	0.69+0.03 −0.04		[49]
GW200208_130117 2020-02-08 13:01:17	2021-11-17	30; towards Pyxis or Antlia	10.8+0.3 −0.4	2230+1000 −850		27.7+3.6 −3.1	−0.07+0.22 −0.27	BH	37.8+9.2 −8.2	BH	27.5+6.1 −7.4	BH	62.5+7.3 −6.4	0.66+0.09 −0.13	Originally designated S200208q.	[49]
GW200208_222617 2020-02-08 22:26:17	2021-11-17	2000	7.4+1.4 −1.2	4100+4400 −1900		19.6+10.7 −5.1	0.45+0.43 −0.44	BH	51+104 −30	BH	12.3+9.0 −5.7	BH	61+100 −25	0.83+0.14 −0.27		[49]
GW200209 2020-02-09 08:54:52	2021-11-17	730	9.6+0.4 −0.5	3400+1900 −1800		26.7+6.0 −4.2	−0.12+0.24 −0.30	BH	35.6+10.5 −6.8	BH	27.1+7.8 −7.8	BH	59.9+13.1 −8.9	0.66+0.10 −0.12		[49]
GW200210 2020-02-10 09:22:54	2021-11-17	1800	8.4+0.5 −0.7	940+430 −340		6.56+0.38 −0.40	0.02+0.22 −0.21	BH	24.1+7.5 −4.6	?	2.83+0.47 −0.42	BH	26.7+7.2 −4.3	0.34+0.13 −0.08	The secondary component, being between 2.41 and 3.30 solar masses, is an object in the mass gap.	[49]
GW200216 2020-02-16 22:08:04	2021-11-17	2900	8.1+0.4 −0.5	3800+3000 −2000		32.9+9.3 −8.5	0.10+0.34 −0.36	BH	51+22 −13	BH	30+14 −16	BH	78+19 −13	0.70+0.14 −0.24		[49]
GW200219 2020-02-19 09:44:15	2021-11-17	700	10.7+0.3 −0.5	3400+1700 −1500		27.6+5.6 −3.8	−0.08+0.23 −0.29	BH	37.5+10.1 −6.9	BH	27.9+7.4 −8.4	BH	62.2+11.7 −7.8	0.66+0.10 −0.13	Originally designated S200219ac.	[49]
GW200220_061928 2020-02-20 06:19:28	2021-11-17	3000	7.2+0.4 −0.7	6000+4800 −3100		62+23 −15	0.06+0.40 −0.38	BH	87+40 −23	BH	61+26 −25	BH	141+51 −31	0.71+0.15 −0.17		[49]
GW200220_124850 2020-02-20 12:48:50	2021-11-17	3200	8.5+0.3 −0.5	4000+2800 −2200		28.2+7.3 −5.1	−0.07+0.27 −0.33	BH	38.9+14.1 −8.6	BH	27.9+9.2 −9.0	BH	64+16 −11	0.67+0.11 −0.14		[49]
GW200224 2020-02-24 22:22:34	2021-11-17	50; towards Virgo or Crater	20.0+0.2 −0.2	1710+490 −640		31.1+3.2 −2.6	0.10+0.15 −0.15	BH	40.0+6.9 −4.5	BH	32.5+5.0 −7.2	BH	68.6+6.6 −4.7	0.73+0.07 −0.07	Originally designated S200224ca.	[49]
GW200225 2020-02-25 06:04:21	2021-11-17	370; towards Ursa Minor or Cepheus	12.5+0.3 −0.4	1150+510 −530		14.2+1.5 −1.4	−0.12+0.17 −0.28	BH	19.3+5.0 −3.0	BH	14.0+2.8 −3.5	BH	32.1+3.5 −2.8	0.66+0.07 −0.13	Originally designated S200225q.	[49]
GW200302 2020-03-02 01:58:11	2021-11-17	6000	10.8+0.3 −0.4	1480+1020 −700		23.4+4.7 −3.0	0.01+0.25 −0.26	BH	37.8+8.7 −8.5	BH	20.0+8.1 −5.7	BH	55.5+8.9 −8.6	0.66+0.13 −0.15	Originally designated S200302c.	[49]
GW200306 2020-03-06 09:37:14	2021-11-17	4600	7.8+0.4 −0.6	2100+1700 −1100		17.5+3.5 −3.0	0.32+0.28 −0.46	BH	28.3+17.1 −7.7	BH	14.8+6.5 −6.4	BH	41.7+12.3 −6.9	0.78+0.11 −0.26		[49]
GW200308 2020-03-08 17:36:09	2021-11-17	2000	7.1+0.5 −0.5	5400+2700 −2600		19.0+4.8 −2.8	0.65+0.21 −0.17	BH	36.4+11.2 −9.6	BH	13.8+7.2 −3.3	BH	47.4+11.1 −7.7	0.91+0.03 −0.08		[49]
GW200311 2020-03-11 11:58:53	2021-11-17	35; towards Cetus	17.8+0.2 −0.2	1170+280 −400		26.6+2.4 −2.0	−0.02+0.16 −0.20	BH	34.2+6.4 −3.8	BH	27.7+4.1 −5.9	BH	59.0+4.8 −3.9	0.69+0.07 −0.08	Originally designated S200311bg.	[49]
GW200316 2020-03-16 21:57:56	2021-11-17	190	10.3+0.4 −0.7	1120+470 −440		8.75+0.62 −0.55	0.13+0.27 −0.10	BH	13.1+10.2 −2.9	BH	7.8+1.9 −2.9	BH	20.2+7.4 −1.9	0.70+0.04 −0.04	Originally designated S200316bj.	[49]
GW200322 2020-03-22 09:11:33	2021-11-17	6500	6.0+1.7 −1.2	3600+7000 −2000		15.5+15.7 −3.7	0.24+0.45 −0.51	BH	34+48 −18	BH	14.0+16.8 −8.7	BH	53+38 −26	0.78+0.16 −0.17		[49]

Gravitational Wave Transient Catalog 1. Credit:LIGO Scientific Collaboration and Virgo Collaboration/Georgia Tech/S. Ghonge & K. Jani

Candidate events and marginal detections

There is possible detection of nanohertz waves by observation of the timing of pulsars, but they have not been confirmed at the 5 sigma level of confidence, as yet.[55]

Marginal detections from O1 and O2

In addition to well-constrained detections listed above, a number of low-significance detections of possible signals were made by LIGO and Virgo. Their characteristics are listed below, only including detections with a <50% chance of being noise:

Marginal event detections
Candidate event	Detection time (UTC)	Date published	Luminosity distance (Mpc)[n 12]	Detector [n 13]	False alarm rate (year)	Effective spin	Primary		Secondary		Probability of terrestrial noise	Notes	Ref
Candidate event	Detection time (UTC)	Date published	Luminosity distance (Mpc)[n 12]	Detector [n 13]	False alarm rate (year)	Effective spin	Type	Mass (M_☉)	Type	Mass (M_☉)	Probability of terrestrial noise	Notes	Ref
151205	2015-12-05 19:55:25	2019-10-11	3000+2400 −1600	H,L	0.61	0.14+0.40 −0.38	BH	67+28 −17	BH	42+16 −19	0.47		[56]
170121	2017-01-21 21:25:36	2019-04-15		H,L		−0.3±0.3	BH	29+4 −3	BH		<0.01		[57]
170304	2017-03-04 16:37:53	2019-10-11	2300+1600 −1200	H,L	2.5	0.11+0.29 −0.27	BH	44.9+17.6 −9.4	BH	31.8+9.5 −11.6	0.30		[56]
170402	2017-04-02 21:51:50	2019-10-21		H,L							0.32		[58]
170727	2017-07-27 01:04:30	2019-10-11	2200+1500 −1100	H,L	180	−0.05+0.25 −0.30	BH	41.6+12.8 −7.9	BH	30.4+7.9 −8.2	0.006		[56]
170817A	2017-08-17 03:02:46	2019-10-21		H,L,V	11.5	0.5±0.2	BH	56+16 −10	BH	40+10 −11	0.14		[58]

Observation candidates from O3/2019

From observation run O3/2019 on, observations are published as Open Public Alerts to facilitate multi-messenger observations of events.[59][60][61] Candidate event records can be directly accessed at the Gravitational-Wave Candidate Event Database (GraceDB).[62] On 1 April 2019, the start of the third observation run was announced with a circular published in the public alerts tracker.[63] The first O3/2019 binary black hole detection alert was broadcast on 8 April 2019. A significant percentage of O3 candidate events detected by LIGO are accompanied by corresponding triggers at Virgo.

False alarm rates are mixed, with more than half of events assigned false alarm rates greater than 1 per 20 years, contingent on presence of glitches around signal, foreground electromagnetic instability, seismic activity, and operational status of any one of the three LIGO-Virgo instruments. For instance, events S190421ar and S190425z weren't detected by Virgo and LIGO's Hanford site, respectively.

The LIGO/Virgo collaboration took a short break from observing during the month of October 2019 to improve performance and prepare for future plans, with no signals detected in that month as a result.[64]

The Kamioka Gravitational Wave Detector (KAGRA) in Japan became operational on 25 February 2020,[65] likely improving the detection and localization of future gravitational wave signals.[66] However, KAGRA does not report their signals in real-time on GraceDB as LIGO and Virgo do, so the results of their observation run will likely not be published until the end of O3.

The LIGO-Virgo collaboration ended the O3 run early on March 27, 2020, due to health concerns from the COVID-19 pandemic.[5][67]

Candidate detections from O3 by month
1 2 3 4 5 6 7 8 9 10 19/04 19/05 19/06 19/07 19/08 19/09 19/10 19/11 19/12 20/01 20/02 20/03 BNS mergers NS-BH mergers mass gap BBH mergers terrestrial noise false positives unidentified

O3 detections by distance
2 4 6 8 10 12 14 16 18 20 <100 Mpc 100-200 Mpc 200-500 Mpc 500-1000 Mpc 1-2 Gpc 2-5 Gpc 5+ Gpc BNS mergers NS-BH mergers mass gap BBH mergers

List of unconfirmed O3 event alerts[10][11]

GW event	Detection time (UTC)	Location area[n 14] (deg²)	Luminosity distance (Mpc)[n 15]	Detector [n 16]	False alarm Rate (Hz)	False alarm chance in O3[n 17]	Classification					Notes	Ref
GW event	Detection time (UTC)	Location area[n 14] (deg²)	Luminosity distance (Mpc)[n 15]	Detector [n 16]	False alarm Rate (Hz)	False alarm chance in O3[n 17]	NS / NS [n 18]	NS / BH [n 19]	BH / BH [n 20]	Mass gap [n 21]	Terrestrial [n 22]	Notes	Ref
S190901ap	2019-09-01 23:31:01	14753	241±79	L,V	7.0 10⁻⁹	0.181	0.861	0.0	0.0	0.0	0.139		[68]
S190910d	2019-09-10 01:26:19	2482	632±186	H,L	3.7 10⁻⁹	0.100	0.0	0.976	0.0	0.0	0.024		[69]
S190910h	2019-09-10 08:29:58	24264	230±88	L	3.6 10⁻⁸	0.642	0.612	0.0	0.0	0.0	0.388	Detected by only the Livingston detector, resulting in a bad sky localization.	[70]
S190923y	2019-09-23 12:55:59	2107	438±133	H,L	4.8 10⁻⁸	0.746	0.0	0.677	0.0	0.0	0.322		[71]
S190930t	2019-09-30 14:34:07	24220	108±38	L	1.5 10⁻⁸	0.348	0.0	0.743	0.0	0.0	0.257	Detected by only the Livingston detector, resulting in a bad sky localization; last detection of the O3a run.	[72]
S191205ah	2019-12-05 21:52:08	6378	385±164	H,L,V	1.2 10⁻⁸	0.290	0.0	0.932	0.0	0.0	0.068		[73]
S191213g	2019-12-13 04:34:08	4480	201±81	H,L,V	3.5 10⁻⁸	0.631	0.768	0.0	0.0	0.0	0.232		[74]
S200213t	2020-02-13 04:10:40	2326	201±80	H,L,V	1.8 10⁻⁸	0.401	0.629	0.0	0.0	0.0	0.371		[75]

Observation candidates from O4/2023

On 15 June 2022, LIGO announced to start the O4 observing run in March 2023.[76] As the date got closer, engineering challenges delayed the observing run to May 2023.[77] An engineering run to assess the sensitivity of LIGO, Virgo, and KAGRA began in April, with the Hanford detector's first operations beginning on April 29,[78] and the Livingston and Virgo detectors' first operations beginning on May 5.[79]

Near the end of the engineering run on 15 May 2023, LIGO announced that O4 would be beginning on 24 May 2023, running for 20 months with up to 2 months of maintenance. The LIGO detectors failed to achieve the hoped for 160-190 Mpc sensitivity for neutron star mergers, but did achieve an improved 130-150 Mpc sensitivity over O3's 100-140 Mpc, later improving to nearly 160 Mpc for both detectors by late 2023. Virgo was found to have a damaged mirror, delaying its observing run until Fall 2023 at the earliest, and KAGRA achieved its planned 1 Mpc neutron star merger sensitivity, with further plans to upgrade beyond 10 Mpc by the end of the observing run.

On 18 May 2023, near the end of the engineering run and shortly before O4 proper, the first candidate gravitational wave event was detected. VIRGO achieved a 31 Mpc neutron star merger sensitivity (similar to its performance during O2 in 2017) by September, but additional issues delayed its observation run until December 2023.

Candidate detections from O4 by month
5 10 15 20 25 30 23/05 23/06 23/07 23/08 23/09 23/10 23/11 23/12 BNS mergers NS-BH mergers mass gap BBH mergers unidentified

O4 detections by distance
5 10 15 20 25 30 35 40 45 50 <100 Mpc 100-200 Mpc 200-500 Mpc 500-1000 Mpc 1-2 Gpc 2-5 Gpc 5+ Gpc BNS mergers NS-BH mergers mass gap BBH mergers

List of O4 event alerts

GW event	Detection time (UTC)	Location area[n 23] (deg²)	Luminosity distance (Mpc)[n 24]	Detector [n 25]	False Alarm Rate (Hz)	False Alarm chance in O4[n 26]	Classification					Notes	Ref
GW event	Detection time (UTC)	Location area[n 23] (deg²)	Luminosity distance (Mpc)[n 24]	Detector [n 25]	False Alarm Rate (Hz)	False Alarm chance in O4[n 26]	NS / NS [n 27]	NS / BH [n 28]	BH / BH [n 29]	Mass gap [n 30]	Terrestrial [n 31]	Notes	Ref
S230518h	2023-05-18 12:59:07	460; near the galactic plane	204±57	H,L	3.2 10⁻¹⁰	0.015	0.0	0.864	0.037	0.0	0.099	Detected during the engineering phase, before the official start of O4.	[80]
S230520ae	2023-05-20 22:48:41	1702	2014±663	H,L	3.1 10⁻⁹	0.133	0.0	0.0	~1.0	0.0	1.4e-7		[81]
S230522a	2023-05-22 09:38:04	24219	3102±1032	L	1.0 10⁻⁸	0.383	0.0	0.0	0.99973	0.00071	0.00027		[82]
S230522n	2023-05-22 15:30:32	29021	2221±870	L	6.5 10⁻⁹	0.261	0.0	0.0	0.993	0.0041	0.0069		[83]
S230524b	2023-05-24 06:13:20	24224	2437±891	L	8.3 10⁻⁷	~1.0[n 32]	0.0	0.0	0.725	0.0041	0.275		[84]
S230525a	2023-05-25 02:38:17	24219	1166±390	L	7.5 10⁻⁷	~1.0[n 33]	0.0	0.0	0.724	0.0082	0.276	Detected by only the Livingston detector, resulting in a bad sky localization.	[85]
S230527bv	2023-05-27 17:25:29	3318; mostly towards Canis Major, Monoceros, Canis Minor, or Hydra	3876±2027	H,L	2.1 10⁻⁷	0.9999[n 34]	0.0	0.0	0.882	0.0	0.118		[86]
S230528a	2023-05-28 02:27:14	1787	261±108	H,L	3.0 10⁻⁷	~1.0[n 35]	0.0053	0.011	0.0	0.626	0.357	The other component is a neutron star.	[87]
S230528ay	2023-05-28 11:10:53	97; towards Sculptor or Aquarius	?	H,L	7.0 10⁻⁷	~1.0[n 36]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting a millisecond at a frequency of hundreds of Hertz.	[88]
S230528bt	2023-05-28 14:51:29	6597	7412±2488	H,L	2.9 10⁻⁷	~1.0[n 37]	0.0	0.0	0.880	0.043	0.120		[89]
S230529ay	2023-05-29 18:15:00	25022	201±63	L	2.0 10⁻¹⁰	0.0092	0.0043	0.0089	0.0	0.916	0.070	The other component is a neutron star. Detected by only the Livingston detector, resulting in a bad sky localization.	[90]
S230531f	2023-05-31 00:21:25	5522	?	H,L	8.5 10⁻⁷	~1.0[n 38]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 8 milliseconds at a frequency of ~650 Hertz.	[91]
S230601bf	2023-06-01 22:41:34	2531	3565±1260	H,L	1.7 10⁻¹⁵	7.8 10⁻⁸	0.0	0.0	~1.0	0.0022	6.4e-9		[92]
S230604z	2023-06-04 09:20:31	2481	392±201	H,L	2.7 10⁻⁷	~1.0[n 39]	0.0	0.042	0.706	0.017	0.252		[93]
S230605o	2023-06-05 06:53:43	1077	1067±333	H,L	4.5 10⁻⁹	0.190	0.0	0.0	0.988	0.0	0.012		[94]
S230606d	2023-06-06 00:43:05	1221	2545±874	H,L	1.1 10⁻⁸	0.412	0.0	0.0	0.99928	0.0	0.00072		[95]
S230606z	2023-06-06 06:53:20	5989	4497±2023	H,L	4.2 10⁻⁷	~1.0[n 40]	0.0	0.0	0.835	0.0	0.165		[96]
S230608as	2023-06-08 20:50:47	1694	3447±1079	H,L	1.4 10⁻¹⁰	0.0064	0.0	0.0	0.99981	0.0	0.00019		[97]
S230609a	2023-06-09 01:08:24	3507	4537±1433	H,L	8.0 10⁻⁸	0.976	0.0	0.0	0.956	0.043	0.044		[98]
S230609u	2023-06-09 06:49:58	1287	3390±1125	H,L	1.0 10⁻⁸	0.374	0.0	0.0	0.961	0.0	0.038		[99]
S230615av	2023-06-15 16:08:26	7017	12726±4301	H,L	1.4 10⁻⁷	0.9988[n 41]	0.0	0.0	0.912	0.026	0.088		[100]
S230615ax	2023-06-15 16:30:04	1569	?	H,L	5.1 10⁻⁷	~1.0[n 42]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 6 milliseconds at a frequency of ~250 Hertz.	[101]
S230615az	2023-06-15 17:50:08	4416	260±133	H,L	1.5 10⁻⁷	0.9991[n 43]	0.847	0.0	0.0	0.0069	0.153		[102]
S230621bq	2023-06-21 23:47:43	790	?	H,L	9.3 10⁻⁷	~1.0[n 44]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 2 milliseconds at a frequency of hundreds of Hertz.	[101]
S230623at	2023-06-23 17:18:09	736; towards Hydra	124±34	H,L	2.0 10⁻⁷	0.9999[n 45]	0.0	0.00080	0.634	0.072	0.293		[103]
S230623be	2023-06-23 21:04:07	2308	?	H,L	8.9 10⁻⁷	~1.0[n 46]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 22 milliseconds at a frequency of ~60 Hertz.	[101]
S230624av	2023-06-24 11:31:03	1718	2556±787	H,L	1.3 10⁻⁸	0.455	0.0	0.0	0.953	0.0	0.047		[104]
S230626ad	2023-06-26 06:07:13	7579	?	H,L	9.4 10⁻⁷	~1.0[n 47]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 163 milliseconds at a frequency of 40 Hertz.	[101]
S230627c	2023-06-27 01:53:37	90; towards Leo, Leo Minor, Ursa Major, or Draco	278±68	H,L	3.2 10⁻¹⁰	0.015	0.0	0.365	0.354	0.251	0.030		[105]
S230628aj	2023-06-28 16:42:24	1861	421±125	H,L	2.1 10⁻⁷	0.9999[n 48]	0.0	0.00085	0.679	0.014	0.306		[106]
S230628ax	2023-06-28 23:12:00	705	2047±585	H,L	3.2 10⁻¹⁰	0.015	0.0	0.0	~1.0	0.0	2.4e-5		[107]
S230630am	2023-06-30 12:58:06	3642	8710±2735	H,L	2.4 10⁻⁸	0.676	0.0	0.0	0.941	0.042	0.017		[108]
S230630bq	2023-06-30 23:45:32	1975	1150±360	H,L	7.7 10⁻⁹	0.303	0.0	0.00076	0.890	0.079	0.031		[109]
S230702an	2023-07-02 18:54:53	2267	2428±849	H,L	1.5 10⁻¹²	7.2 10⁻⁵	0.0	0.0	~1.0	0.0	2.8e-5		[110]
S230704f	2023-07-04 02:12:11	1948	2965±978	H,L	2.8 10⁻⁹	0.123	0.0	0.0	0.997	0.0	0.0026		[111]
S230704bd	2023-07-04 21:26:16	6293	15450±5072	H,L	5.9 10⁻⁷	~1.0[n 49]	0.0	0.0	0.735	0.020	0.245		[112]
S230706ah	2023-07-06 10:43:33	1553	2143±684	H,L	4.3 10⁻⁸	0.863	0.0	0.0	0.939	0.035	0.027		[113]
S230707ai	2023-07-07 12:40:47	2714	3766±1135	H,L	1.4 10⁻⁸	0.474	0.0	0.0	0.951	0.0	0.049		[114]
S230708t	2023-07-08 05:37:05	1227	3010±988	H,L	4.3 10⁻⁸	0.867	0.0	0.0	0.973	0.0041	0.027		[115]
S230708z	2023-07-08 07:18:59	3373	4647±1696	H,L	7.0 10⁻⁸	0.962	0.0	0.0	0.954	0.0041	0.046		[116]
S230708cf	2023-07-08 23:09:35	2525	2056±608	H,L	1.6 10⁻⁸	0.515	0.0	0.0	0.989	0.0	0.011		[117]
S230709i	2023-07-09 02:25:02	2408	?	H,L	5.2 10⁻⁷	~1.0[n 50]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 5 milliseconds at a frequency of hundreds of Hertz.	[118]
S230709bi	2023-07-09 12:27:27	2644	4364±1585	H,L	3.1 10⁻⁹	0.133	0.0	0.0	0.997	0.0	0.0028		[119]
S230711b	2023-07-11 02:07:05	4775	6214±2136	H,L	4.8 10⁻⁷	~1.0[n 51]	0.0	0.0	0.758	0.034	0.208		[120]
S230712d	2023-07-12 01:33:43	454	?	H,L	9.8 10⁻⁷	~1.0[n 52]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 6 milliseconds at a frequency of ~550 Hertz.	[121]
S230712ak	2023-07-12 08:55:17	4255	?	H,L	4.2 10⁻⁷	~1.0[n 53]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 20 milliseconds at a frequency of tens of Hertz.	[122]
S230713ar	2023-07-13 10:22:24	1494	?	H,L	6.3 10⁻⁷	~1.0[n 54]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 2 milliseconds at a frequency of hundreds of Hertz.	[123]
S230716j	2023-07-16 01:13:00	3935	?	H,L	6.3 10⁻⁷	~1.0[n 55]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 5 milliseconds at a frequency of ~800 Hertz.	[124]
S230716o	2023-07-16 03:01:19	2351	508±203	H,L	5.0 10⁻⁷	~1.0[n 56]	0.0	0.0064	0.568	0.176	0.250		[125]
S230723ac	2023-07-23 10:18:23	1117	1551±436	H,L	5.3 10⁻⁸	0.917	0.0	0.0	0.867	0.0	0.133		[126]
S230725am	2023-07-25 13:16:48	3415	613±203	H,L	5.0 10⁻⁷	~1.0[n 57]	0.0	0.00057	0.454	0.047	0.498		[127]
S230726a	2023-07-26 00:29:40	27774	2132±714	L	3.8 10⁻¹⁴	1.8 10⁻⁶	0.0	0.0	~1.0	0.0	1.4e-7	Detected by only the Livingston detector, resulting in a bad sky localization.	[128]
S230728ap	2023-07-28 08:36:28	3495	2731±1445	H,L	1.0 10⁻⁷	0.9917[n 58]	0.0	0.0	0.940	0.0	0.060		[129]
S230729z	2023-07-29 08:23:17	1945	1495±444	H,L	3.4 10⁻⁹	0.158	0.0	0.0	0.942	0.055	0.0030		[130]
S230731an	2023-07-31 21:53:07	599	1001±242	H,L	3.2 10⁻¹⁰	0.015	0.0	0.174	0.771	0.053	0.0022		[131]
S230802aq	2023-08-02 11:33:59	25885	576±246	H	2.2 10⁻⁸	0.646	0.0	0.020	0.289	0.657	0.035	The other component is a black hole. Detected by only the Hanford detector, resulting in a bad sky localization.	[132]
S230805x	2023-08-05 03:42:49	2235	3852±1193	H,L	9.2 10⁻⁹	0.349	0.0	0.0	0.99975	0.0	0.00025		[133]
S230805bm	2023-08-05 11:59:27	11617	?	H,L	2.7 10⁻⁷	~1.0[n 59]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 15 milliseconds at a frequency of 1370 Hertz.	[134]
S230806ak	2023-08-06 20:40:41	3715	5423±1862	H,L	3.0 10⁻⁹	0.129	0.0	0.0	0.997	0.0	0.0026		[135]
S230807f	2023-08-07 20:50:45	5436	5272±1900	H,L	7.1 10⁻⁸	0.964	0.0	0.0	0.913	0.041	0.047		[136]
S230811n	2023-08-11 03:21:16	810	1905±672	H,L	3.2 10⁻¹⁰	0.015	0.0	0.0	~1.0	0.0	2.2e-5		[137]
S230814r	2023-08-14 06:19:20	3389	3788±1416	H,L	4.8 10⁻⁸	0.894	0.0	0.0	0.932	0.0	0.068		[138]
S230814ah	2023-08-14 23:09:01	25259	330±105	L	1.7 10⁻²¹	8.6 10⁻¹⁴	0.0	0.0	~1.0	0.0	2.0e-14	Detected by only the Livingston detector, resulting in a bad sky localization.	[139]
S230819ax	2023-08-19 17:19:10	4044	4216±1645	H,L	8.8 10⁻⁹	0.338	0.0	0.0	0.993	0.0	0.0072		[140]
S230820bq	2023-08-20 21:25:15	1373	3600±1437	H,L	4.2 10⁻⁸	0.861	0.0	0.0	0.958	0.0	0.042		[141]
S230822ac	2023-08-22 04:39:49	5534	9962±3231	H,L	3.6 10⁻⁷	~1.0[n 60]	0.0	0.0	0.778	0.035	0.187		[142]
S230822bm	2023-08-22 23:03:37	3974	5154±1771	H,L	2.6 10⁻⁸	0.700	0.0	0.0	0.939	0.042	0.019		[143]
S230824r	2023-08-24 03:30:47	3279	4701±1563	H,L	1.6 10⁻¹¹	0.00076	0.0	0.0	~1.0	0.0	2.9e-5		[144]
S230824bp	2023-08-24 13:53:31	5095	?	H,L	5.0 10⁻⁷	~1.0[n 61]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 22 milliseconds at a frequency of tens of Hertz.	[145]
S230825k	2023-08-25 04:13:34	3012	5283±2117	H,L	2.4 10⁻⁹	0.105	0.0	0.0	0.939	0.059	0.0022		[146]
S230825aq	2023-08-25 11:31:24	3789	?	H,L	3.5 10⁻⁷	~1.0[n 62]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 6 milliseconds at a frequency of ~100 Hertz.	[147]
S230828aq	2023-08-28 16:07:06	6428	?	H,L	5.2 10⁻⁷	~1.0[n 63]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 13 milliseconds at a frequency of 800 Hertz.	[148]
S230830q	2023-08-30 06:47:44	1677	3843±1289	H,L	1.3 10⁻⁷	0.9980[n 64]	0.0	0.0	0.923	0.0041	0.077		[149]
S230831e	2023-08-31 01:54:14	3803	4900±2126	H,L	2.0 10⁻⁸	0.603	0.0	0.0	0.985	0.0073	0.015		[150]
S230902af	2023-09-02 15:03:25	7622	10221±3354	H,L	4.0 10⁻⁷	~1.0[n 65]	0.0	0.0	0.764	0.034	0.202		[151]
S230904n	2023-09-04 05:10:13	2015	1095±327	H,L	2.2 10⁻⁹	0.100	0.0	0.0007	0.927	0.064	0.009		[152]
S230904bg	2023-09-04 19:45:32	3059	4581±1531	H,L	8.0 10⁻⁷	~1.0[n 66]	0.0	0.0	0.688	0.0073	0.312		[153]
S230908aa	2023-09-08 09:24:37	699	?	H,L	8.9 10⁻⁷	~1.0[n 67]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 62 milliseconds at a frequency of 1420 Hertz.	[154]
S230911ae	2023-09-11 19:53:24	27759	1623±584	H	1.9 10⁻¹²	8.8 10⁻⁵	0.0	0.0	~1.0	0.0	3.6e-6	Detected by only the Hanford detector, resulting in a bad sky localization.	[155]
S230911ar	2023-09-11 23:51:36	3178	?	H,L	3.8 10⁻⁷	~1.0[n 68]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 5 milliseconds at a frequency of ~700 Hertz.	[156]
S230914ak	2023-09-14 11:14:01	1532	2676±827	H,L	9.0 10⁻¹⁰	0.041	0.0	0.0	0.992	0.0	0.0083		[157]
S230916bm	2023-09-16 19:03:58	3188	?	H,L	8.8 10⁻⁷	~1.0[n 69]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 20 milliseconds at a frequency of ~50 Hertz.	[158]
S230917af	2023-09-17 10:04:17	238	?	H,L	4.6 10⁻⁷	~1.0[n 70]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 14 milliseconds at a frequency of 1050 Hertz.	[159]
S230919bj	2023-09-19 21:57:12	708	1491±402	H,L	3.2 10⁻¹⁰	0.015	0.0	0.0	0.99965	0.0	0.00035		[160]
S230920al	2023-09-20 07:11:24	2180	3139±1003	H,L	3.2 10⁻¹⁰	0.015	0.0	0.0	~1.0	0.0	1.1e-5		[161]
S230922g	2023-09-22 02:03:44	324; towards Pisces Austrinus or Aquarius	1491±443	H,L	1.9 10⁻²⁴	0.0	0.0	0.0	~1.0	0.0	0.0		[162]
S230922q	2023-09-22 04:06:58	4658	6653±2348	H,L	3.6 10⁻¹⁰	0.017	0.0	0.0	~1.0	0.0	2.2e-5		[163]
S230924an	2023-09-24 12:44:53	835	2358±596	H,L	3.2 10⁻¹⁰	0.015	0.0	0.0	~1.0	0.0	1.9e-5		[164]
S230925cj	2023-09-25 23:58:25	4087	?	H,L	2.1 10⁻⁷	0.9999[n 71]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 30 milliseconds at a frequency of ~20 Hertz.	[165]
S230927g	2023-09-27 02:49:41	493	?	H,L	7.2 10⁻⁷	~1.0[n 72]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 1 millisecond at a frequency of hundreds of Hertz.	[166]
S230927l	2023-09-27 04:37:29	1177	2966±1041	H,L	1.1 10⁻⁸	0.394	0.0	0.0	0.976	0.0	0.024		[167]
S230927be	2023-09-27 15:38:32	298	1059±289	H,L	3.2 10⁻¹⁰	0.015	0.0	0.0	0.99966	0.0	0.00034		[168]
S230928cb	2023-09-28 21:58:27	3093	5604±1692	H,L	9.5 10⁻¹⁰	0.043	0.0	0.0	~1.0	0.0	2.8e-5		[169]
S230930al	2023-09-30 11:07:30	2799	5123±1615	H,L	7.4 10⁻⁹	0.291	0.0	0.0	0.994	0.0041	0.0061		[170]
S231001aq	2023-10-01 14:02:20	3323	2567±958	H,L	5.0 10⁻⁹	0.207	0.0	0.0	0.996	0.0044	0.0040		[171]
S231004bq	2023-10-04 23:23:46	4742	7960±2738	H,L	7.6 10⁻⁷	~1.0[n 73]	0.0	0.0	0.677	0.030	0.292		[172]
S231005j	2023-10-05 02:10:30	5480	6417±2246	H,L	3.2 10⁻⁸	0.777	0.0	0.0	0.978	0.0	0.022		[173]
S231005ah	2023-10-05 09:15:49	2497	3707±1335	H,L	2.0 10⁻⁹	0.091	0.0	0.0	0.998	0.0041	0.0015		[174]
S231007w	2023-10-07 13:47:20	2648	3721±1231	H,L	6.1 10⁻⁷	~1.0[n 74]	0.0	0.0	0.746	0.0041	0.254		[175]
S231007am	2023-10-07 17:13:31	5225	?	H,L	2.2 10⁻⁷	~1.0[n 75]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 4 milliseconds at a frequency of ~500 Hertz.	[176]
S231008ap	2023-10-08 14:25:21	3102	3531±1320	H,L	1.5 10⁻⁹	0.069	0.0	0.0	0.9986	0.0	0.0014		[177]
S231014r	2023-10-14 04:05:48	1807	2857±903	H,L	1.0 10⁻⁸	0.382	0.0	0.0	0.992	0.0	0.0080		[178]
S231017e	2023-10-17 00:59:24	10355	?	H,L	6.2 10⁻⁷	~1.0[n 76]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 26 milliseconds at a frequency of ~30 Hertz.	[179]
S231018br	2023-10-18 16:43:52	462	?	H,L	8.1 10⁻⁷	~1.0[n 77]	0.0	0.0	0.0	0.0	?	Unidentified gravitational wave "burst" lasting 31 milliseconds at a frequency of 328 Hertz.	[180]
S231020ba	2023-10-20 14:29:47	1339	1168±361	H,L	1.3 10⁻⁹	0.057	0.0	0.076	0.851	0.066	0.0070		[181]
S231020bw	2023-10-20 18:05:09	888	2868±924	H,L	3.5 10⁻¹⁰	0.016	0.0	0.0	0.99965	0.0	0.00035		[182]
S231025a	2023-10-25 03:11:24	2254	233±135	H,L	9.3 10⁻⁷	~1.0[n 78]	0.587	0.0016	0.0	0.0	0.412		[183]
S231025ap	2023-10-25 14:23:06	4584	4394±1526	H,L	3.7 10⁻⁷	~1.0[n 79]	0.0	0.0	0.794	0.035	0.170		[184]

Notes

The detection date of a GW event is indicated by its designation; i.e., event GW150914 was detected on 2015-09-14.
The relatively large and distant area of the sky within which it is claimed to be 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 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. It is related to, but less than, the geometric mean $(m_{geo})$ of the binary masses, according to $m_{geo}\left({\frac {m_{geo}}{m_{1}+m_{2}}}\right)^{1/5}$ , thus ranging from ~87% of $m_{geo}$ when the masses are the same to ~78% when they differ by an order of magnitude.
The dimensionless effective inspiral spin parameter is: ${\frac {m_{1}a_{1}cos\theta _{LS_{1}}+m_{2}a_{2}cos\theta _{LS_{2}}}{m_{1}+m_{2}}},$ [12] where $m$ is the mass of a black hole, $a$ is its spin, and $\theta _{LS}$ is the angle between the orbital angular momentum and a merging black hole's spin (ranging from $0$ when aligned to $\pi$ when antialigned). It is the mass-weighted linear combination of the components of the black holes' spins aligned with the orbital axis[12][11] and has values ranging from −1 to 1 (the extremes correspond to situations with both black hole spins exactly antialigned and aligned, respectively, with orbital angular momentum).[13] This is the spin parameter most relevant to the evolution of the inspiral gravitational waveform, and it can be measured more accurately than those of the premerger BHs.[14]
Values of the dimensionless spin parameter $a=$ c J/G M² for a black hole 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.[15]
Spin estimate is 0.26+0.52
−0.24.[16]
Spin estimate is 0.32+0.54
−0.29.[16]
Based on a descending spin-down chirp observed in GW post-merger, a magnetar was produced that survived at least 5 seconds.[26]
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.[27]
1 Mpc is approximately 3.26 Mly.
Which instruments observed the event. (H = LIGO Hanford, L=LIGO Livingston, V=Virgo)
The area of the sky within which it was possible to localize the source.
1 Mpc is approximately 3.26 Mly.
Which instruments observed the event. (H = LIGO Hanford, L=LIGO Livingston, V=Virgo)
The chance a random signal of this significance would occur at any point in O3's 11-month run. Calculated by 1 - (1-false alarm rate in Hz)^28,512,000. This is not the chance of the given signal being 'real' or not: Background contamination (such as earthquakes) can cause statistically significant signals as well, and although four detections have a >50% chance to have occurred randomly in O3, there is only a 19.4% chance that none of these signals would be real.
Probability that both components have mass < 3 M_☉
Probability that one component has mass < 3 M_☉ and the other has mass > 5 M_☉
Probability that both components have mass > 5 M_☉
Probability that at least one component has a mass in the range 3-5 M_☉, between those of known neutron stars and black holes, a range sometimes identified as the "lower" mass gap
Probability that the source is terrestrial or non-cosmological (e.g. foreground noises and signals [e.g. "noise"] or a technical/systematic error ["glitch"])
The area of the sky within which it was possible to localize the source.
1 Mpc is approximately 3.26 Mly.
Which instruments observed the event. (H = LIGO Hanford, L=LIGO Livingston, V=Virgo)
The chance a random signal of this significance would occur at any point in O4's 20-month run. Calculated by 1 - (1-false alarm rate in Hz)^46,656,000. This is not the chance of the given signal being 'real' or not: Background contamination (such as earthquakes) can cause statistically significant signals as well.
Probability that both components have mass < 3 M_☉
Probability that one component has mass < 3 M_☉ and the other has mass > 5 M_☉
Probability that both components have mass > 5 M_☉
Probability that at least one component has a mass in the range 3-5 M_☉, between those of known neutron stars and black holes, a range sometimes identified as the "lower" mass gap
Probability that the source is terrestrial or non-cosmological (e.g. foreground noises and signals [e.g. "noise"] or a technical/systematic error ["glitch"])
During O4, random noise is expected to be as significant as this event 39 times; 0.5 times by this point in the run.
During O4, random noise is expected to be as significant as this event 35 times; 0.5 times by this point in the run.
During O4, random noise is expected to be as significant as this event 10 times; 0.2 times by this point in the run.
During O4, random noise is expected to be as significant as this event 14 times; 0.3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 33 times; 0.7 times by this point in the run.
During O4, random noise is expected to be as significant as this event 13 times; 0.3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 40 times; 1 time by this point in the run.
During O4, random noise is expected to be as significant as this event 13 times; 0.4 times by this point in the run.
During O4, random noise is expected to be as significant as this event 19 times; 0.7 times by this point in the run.
During O4, random noise is expected to be as significant as this event 7 times; 0.4 times by this point in the run.
During O4, random noise is expected to be as significant as this event 24 times; 1 time by this point in the run.
During O4, random noise is expected to be as significant as this event 7 times; 0.4 times by this point in the run.
During O4, random noise is expected to be as significant as this event 43 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 9 times; 0.6 times by this point in the run.
During O4, random noise is expected to be as significant as this event 42 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 44 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 10 times; 0.8 times by this point in the run.
During O4, random noise is expected to be as significant as this event 28 times; 2 times by this point in the run.
During O4, random noise is expected to be as significant as this event 24 times; 2 times by this point in the run.
During O4, random noise is expected to be as significant as this event 22 times; 2 times by this point in the run.
During O4, random noise is expected to be as significant as this event 46 times; 5 times by this point in the run.
During O4, random noise is expected to be as significant as this event 21 times; 2 times by this point in the run.
During O4, random noise is expected to be as significant as this event 30 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 31 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 23 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 23 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 5 times; 0.6 times by this point in the run.
During O4, random noise is expected to be as significant as this event 13 times; 2 times by this point in the run.
During O4, random noise is expected to be as significant as this event 17 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 23 times; 4 times by this point in the run.
During O4, random noise is expected to be as significant as this event 16 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 24 times; 5 times by this point in the run.
During O4, random noise is expected to be as significant as this event 6 times; 1 time by this point in the run.
During O4, random noise is expected to be as significant as this event 19 times; 4 times by this point in the run.
During O4, random noise is expected to be as significant as this event 37 times; 8 times by this point in the run.
During O4, random noise is expected to be as significant as this event 42 times; 9 times by this point in the run.
During O4, random noise is expected to be as significant as this event 18 times; 4 times by this point in the run.
During O4, random noise is expected to be as significant as this event 41 times; 9 times by this point in the run.
During O4, random noise is expected to be as significant as this event 21 times; 5 times by this point in the run.
During O4, random noise is expected to be as significant as this event 10 times; 2 times by this point in the run.
During O4, random noise is expected to be as significant as this event 34 times; 8 times by this point in the run.
During O4, random noise is expected to be as significant as this event 36 times; 9 times by this point in the run.
During O4, random noise is expected to be as significant as this event 28 times; 7 times by this point in the run.
During O4, random noise is expected to be as significant as this event 10 times; 3 times by this point in the run.
During O4, random noise is expected to be as significant as this event 29 times; 8 times by this point in the run.
During O4, random noise is expected to be as significant as this event 38 times; 11 times by this point in the run.
During O4, random noise is expected to be as significant as this event 44 times; 13 times by this point in the run.
During O4, random noise is expected to be as significant as this event 17 times; 5 times by this point in the run.

References

"GW150914 - The First Direct Detection of Gravitational Waves". www.ligo.org. Retrieved 2023-03-15.
"LSC News". www.ligo.org. Retrieved 2023-03-15.
The LIGO Scientific Collaboration; the Virgo Collaboration; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abraham, S.; Acernese, F.; Ackley, K.; Adams, C.; Adhikari, R. X.; Adya, V. B. (2019-09-04). "GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs". Physical Review X. 9 (3): 031040. arXiv:1811.12907. Bibcode:2019PhRvX...9c1040A. doi:10.1103/PhysRevX.9.031040. ISSN 2160-3308. S2CID 119366083.
Burtnyk, Kimberly (2019-10-01). "LIGO's Commissioning Break Commences". LIGO Lab | Caltech. Retrieved 2020-07-01.
"LIGO Suspends Third Observing Run (O3)". LIGO Lab. Caltech. Retrieved 20 April 2020.
Ligo, Virgo and Kagra Observing Run Plans
"GCN/LVC Notices". Goddard Space Flight Center. Retrieved 2019-11-11.
Fragione, Giacomo; et al. (2019). "Black Hole and Neutron Star Mergers in Galactic Nuclei". Monthly Notices of the Royal Astronomical Society. 488 (1): 47–63. arXiv:1811.10627. Bibcode:2019MNRAS.488...47F. doi:10.1093/mnras/stz1651. S2CID 85459844.
Strickland, Ashley (3 May 2019). "Scientists may have detected violent collision between neutron star, black hole". CNN. Retrieved 3 May 2019.
Nitz, Alexander H. (25 February 2019). "1-OGC: The first open gravitational-wave catalog of binary mergers from analysis of public Advanced LIGO data". Astrophysical Journal. 872 (2): 195. arXiv:1811.01921. Bibcode:2019ApJ...872..195N. doi:10.3847/1538-4357/ab0108. S2CID 119389481.
Abbott, B.P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (2019). "GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs". Physical Review X. 9 (3): 031040. arXiv:1811.12907. Bibcode:2019PhRvX...9c1040A. doi:10.1103/PhysRevX.9.031040. S2CID 119366083.
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 (22): 221101. arXiv:1706.01812. Bibcode:2017PhRvL.118v1101A. doi:10.1103/PhysRevLett.118.221101. PMID 28621973. S2CID 206291714.
Farr, W. M.; Stevenson, S.; Miller, M. C.; Mandel, I.; F arr, B.; Vecchio, A. (2017). "Distinguishing spin-aligned and isotropic black hole populations with gravitational waves". Nature. 548 (7667): 426–429. arXiv:1706.01385. Bibcode:2017Natur.548..426F. doi:10.1038/nature23453. PMID 28836595. S2CID 4411726.
Vitale, S.; Lynch, R.; Raymond, V.; Sturani, R.; Veitch, J.; Graff, P. (2017). "Parameter estimation for heavy binary-black holes with networks of second-generation gravitational-wave detectors". Physical Review D. 95 (6): 064053. arXiv:1611.01122. Bibcode:2017PhRvD..95f4053V. doi:10.1103/PhysRevD.95.064053. hdl:1721.1/109575. S2CID 118511535.
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): 161101. arXiv:1710.05832. Bibcode:2017PhRvL.119p1101A. doi:10.1103/PhysRevLett.119.161101. PMID 29099225. S2CID 217163611.
The LIGO Scientific Collaboration and The Virgo Collaboration (3 June 2016). "An improved analysis of GW150914 using a fully spin-precessing waveform model". Physical Review X. 6 (4): 041014. arXiv:1606.01210. Bibcode:2016PhRvX...6d1014A. doi:10.1103/PhysRevX.6.041014. S2CID 18217435.
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. S2CID 124959784.
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 (4): 041015. arXiv:1606.04856. Bibcode:2016PhRvX...6d1015A. doi:10.1103/PhysRevX.6.041015. S2CID 31926886.
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. S2CID 118651851.
Nemiroff, R.; Bonnell, J., eds. (15 June 2016). "GW151226: A Second Confirmed Source of Gravitational Radiation". Astronomy Picture of the Day. NASA.
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, B.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): L35. arXiv:1711.05578. Bibcode:2017ApJ...851L..35A. doi:10.3847/2041-8213/aa9f0c. S2CID 9030576.
Abbott, B.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. PMID 29053306. S2CID 46829350.
- "Gravitational waves from a binary black hole merger observed by LIGO and Virgo" (PDF). LIGO Scientific Collaboration (Press release).
Overbye, Dennis (27 September 2017). "New Gravitational Wave Detection From Colliding Black Holes". The New York Times. Retrieved 28 September 2017.
van Putten, Maurice H.P.M.; Della Valle, Massimo (January 2019). "Observational evidence for extended emission to GW170817". Monthly Notices of the Royal Astronomical Society: Letters. 482 (1): L46–L49. arXiv:1806.02165. Bibcode:2019MNRAS.482L..46V. doi:10.1093/mnrasl/sly166.
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". Science. 358 (6370): 1570–1574. arXiv:1710.05443. Bibcode:2017Sci...358.1570D. doi:10.1126/science.aaq0049. PMID 29038375.
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. Bibcode:2017ApJ...848L..12A. doi:10.3847/2041-8213/aa91c9.
Cho, Adrian (16 October 2017). "Merging neutron stars generate gravitational waves and a celestial light show". Science. Retrieved 16 October 2017.
The LIGO Scientific Collaboration; the Virgo Collaboration (2021). "GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo during the First Half of the Third Observing Run". Physical Review X. 11 (2): 021053. arXiv:2010.14527. Bibcode:2021PhRvX..11b1053A. doi:10.1103/PhysRevX.11.021053. S2CID 225094244.
"Superevent info - S190412m". LIGO. Retrieved 12 April 2019.
The LIGO Scientific Collaboration; the Virgo Collaboration; Abbott, R.; et al. (17 April 2020). "GW190412: Observation of a Binary-Black-Hole Coalescence with Asymmetric Masses". Physical Review D. 102 (4): 043015. arXiv:2004.08342. Bibcode:2020PhRvD.102d3015A. doi:10.1103/PhysRevD.102.043015. S2CID 215814461.
Позаненко, А. С.; Минаев, П. Ю.; Гребенев, С. А.; Человеков, И. В. (2019). "Наблюдение в гамма-диапазоне второго связанного со слиянием нейтронных звезд события LIGO/Virgo S190425z". Письма В Астрономический Журнал: Астрономия И Космическая Астрофизика (in Russian). 45 (11): 768–786. arXiv:1912.13112. doi:10.1134/S032001081911007X. S2CID 239427905.
"Gravitational waves reveal a second neutron star collision". 8 January 2020.
"Superevent info - S190425z". LIGO. Retrieved 25 April 2019.
The LIGO Scientific Collaboration; the Virgo Collaboration; et al. (6 January 2020). "GW190425: Observation of a Compact Binary Coalescence with Total Mass ~ 3.4 M_☉". The Astrophysical Journal. 892 (1): L3. arXiv:2001.01761. Bibcode:2020ApJ...892L...3A. doi:10.3847/2041-8213/ab75f5. S2CID 210023687.
Abbott, R.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (2 September 2020). "GW190521: A Binary Black Hole Merger with a Total Mass of 150 M ⊙". Physical Review Letters. 125 (10): 101102. arXiv:2009.01075. Bibcode:2020PhRvL.125j1102A. doi:10.1103/PhysRevLett.125.101102. PMID 32955328. S2CID 221447506.
Abbott, R.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (2 September 2020). "Properties and Astrophysical Implications of the 150 M ⊙ Binary Black Hole Merger GW190521". The Astrophysical Journal. 900 (1): L13. arXiv:2009.01190. Bibcode:2020ApJ...900L..13A. doi:10.3847/2041-8213/aba493. hdl:11343/273616. S2CID 221447444.
"Black hole or neutron star?". June 23, 2020.
"Superevent info - S190814bv". LIGO. Retrieved 15 August 2019.
Starr, Michelle (16 August 2019). "Early Reports Indicate We May Have Detected a Black Hole And Neutron Star Collision". ScienceAlert.com. Retrieved 16 August 2019.
Mandelbum, Ryan F. (26 August 2019). "Mystery Deepens Around Newly Detected Ripples in Space-Time". Gizmodo. Retrieved 26 August 2019.
Starr, Michelle (11 February 2020). "First Papers on The Black Hole-Neutron Star Merger Are In. Here's What We Didn't See". ScienceAlert.com. Retrieved 11 February 2020.
Ackley, K.; et al. (5 February 2020). "Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger S190814bv". arXiv:2002.01950v1 [astro-ph.SR].
Overbye, Dennis (24 June 2020). "A Black Hole's Lunch Provides a Treat for Astronomers - Scientists have discovered the heaviest known neutron star, or maybe the lightest known black hole: "Either way it breaks a record."". The New York Times. Retrieved 24 June 2020.
Starr, Michelle (24 June 2020). "Astronomers Detect First-Ever Mystery Object in The 'Mass Gap' of Cosmic Collisions". ScienceAlert.com. Retrieved 24 June 2020.
University of Birmingham (23 June 2020). "Gravitational wave scientists grapple with the cosmic mystery of GW190814". EurekAlert!. Retrieved 24 June 2020.
Abbott, R.; et al. (23 June 2020). "GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object". The Astrophysical Journal Letters. 896 (2): L44. arXiv:2006.12611. Bibcode:2020ApJ...896L..44A. doi:10.3847/2041-8213/ab960f.
The LIGO Scientific Collaboration; et al. (17 November 2021). "GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run". arXiv:2111.03606. {{cite journal}}: Cite journal requires |journal= (help)
Abbott, R.; et al. (2021). "Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences". The Astrophysical Journal Letters. 915 (1): L5. arXiv:2106.15163. Bibcode:2021ApJ...915L...5A. doi:10.3847/2041-8213/ac082e. S2CID 235670241.
"Superevent info - S200105ae". LIGO. Retrieved 6 January 2020.
Bustillo, Juan Calderon; Sanchis-Gual, Nicolas; Leong, Samson H. W.; Chandra, Koustav; Torres-Forne, Alejandro; Font, Jose A.; Herdeiro, Carlos; Radu, Eugen; Wong, Isaac C. F.; Li, T. G. F. (2022). "Searching for vector boson-star mergers within LIGO-Virgo intermediate-mass black-hole merger candidates". arXiv:2206.02551 [gr-qc].
Hourihane, Sophie; Chatziioannou, Katerina; Wijngaarden, Marcella; Davis, Derek; Littenberg, Tyson; Cornish, Neil (15 August 2022). "Accurate modeling and mitigation of overlapping signals and glitches in gravitational-wave data". Physical Review D. 106 (4): 042006. arXiv:2205.13580. Bibcode:2022PhRvD.106d2006H. doi:10.1103/PhysRevD.106.042006. S2CID 249152318.
"Superevent info - S200115j". LIGO. Retrieved 15 January 2020.
Hartono, Naomi (29 June 2023). "15 Years of Radio Data Reveals Evidence of Space-Time Murmur". NASA. Retrieved 3 July 2023.
Nitz, Alexander H.; Dent, Thomas; Davies, Gareth S.; Kumar, Sumit; Capano, Collin D.; Harry, Ian; Mozzon, Simone; Nuttall, Laura; Lundgren, Andrew; Tápai, Márton (12 March 2020). "2-OGC: Open Gravitational-wave Catalog of Binary Mergers from Analysis of Public Advanced LIGO and Virgo Data". The Astrophysical Journal. 891 (2): 123. arXiv:1910.05331. Bibcode:2020ApJ...891..123N. doi:10.3847/1538-4357/ab733f. S2CID 204403263.
Venumadhav, Tejaswi; Zackay, Barak; Roulet, Javier; Dai, Liang; Zaldarriaga, Matias (2020). "New Binary Black Hole Mergers in the Second Observing Run of Advanced LIGO and Advanced Virgo". Physical Review D. 101 (8): 083030. arXiv:1904.07214. Bibcode:2020PhRvD.101h3030V. doi:10.1103/PhysRevD.101.083030. S2CID 119188594.
Zackay, Barak; Dai, Liang; Venumadhav, Tejaswi; Roulet, Javier; Zaldarriaga, Matias (2021). "Detecting Gravitational Waves With Disparate Detector Responses: Two New Binary Black Hole Mergers". Phys. Rev. D. 104 (8): 063030. arXiv:1910.09528. Bibcode:2020PhRvD.101h3030V. doi:10.1103/PhysRevD.101.083030. S2CID 119188594.
"Real-time alerts and circulars tracker" – via nasa.gov.
"Observing Plans and Public Alerts". www.ligo.org. LIGO Scientific Collaboration. October 2018. Retrieved 2018-10-28.
Singer, Leo P. (16 March 2017). "What constitutes an open, public alert?" (PDF). LSC (LIGO Scientific Collaboration). Retrieved 30 October 2018 – via gw-astronomy.org.
"GraceDB — Gravitational Wave Candidate Event Database" – via ligo.org.
"Real-time alerts and circulars tracker" – via nasa.gov.
"LIGO Announces Commissioning Break". LIGO Lab | Caltech. Retrieved 7 November 2019.
"KAGRA Gravitational-wave Telescope Starts Observation « KAGRA Large-scale Cryogenic Graviationai wave Telescope Project" (in Japanese). Retrieved 2020-02-27.
"KAGRA to Join LIGO and Virgo in Hunt for Gravitational Waves". LIGO Lab | Caltech. Retrieved 2019-10-06.
"LIGO Laboratory's Response to COVID-19". LIGO Lab. Caltech. Retrieved 24 March 2020.
"Superevent info - S190901ap". LIGO. Retrieved 6 September 2019.
"Superevent info - S190910d". LIGO. Retrieved 10 September 2019.
"Superevent info - S190910h". LIGO. Retrieved 10 September 2019.
"Superevent info - S190923y". LIGO. Retrieved 24 September 2019.
"Superevent info - S190930t". LIGO. Retrieved 30 September 2019.
"Superevent info - S191205ah". LIGO. Retrieved 5 December 2019.
"Superevent info - S191213g". LIGO. Retrieved 14 December 2019.
"Superevent info - S200213t". LIGO. Retrieved 13 February 2020.
"LIGO, Virgo and Kagra Observing Run Plans". LIGO Lab. Caltech. Retrieved 16 July 2022.
Burtnyk, Kimberly. "Latest Update on Start of Next Observing Run (O4)". LIGO. Caltech. Retrieved 18 May 2023.
"Detector status - 29 April 2023". gwosc.org. Retrieved 18 May 2023.
"Detector status - 5 May 2023". gwosc.org.
"Superevent info - S230518h". LIGO. Retrieved 18 May 2023.
"Superevent info - S230520ae". LIGO. Retrieved 21 May 2023.
"Superevent info - S230522a". LIGO. Retrieved 22 May 2023.
"Superevent info - S230522n". LIGO. Retrieved 22 May 2023.
"Superevent info - S230524b". LIGO. Retrieved 24 May 2023.
"Superevent info - S230525a". LIGO. Retrieved 25 May 2023.
"Superevent info - S230527bv". LIGO. Retrieved 27 May 2023.
"Superevent info - S230528a". LIGO. Retrieved 28 May 2023.
"Superevent info - S230528ay". LIGO. Retrieved 28 May 2023.
"Superevent info - S230528bt". LIGO. Retrieved 28 May 2023.
"Superevent info - S230529ay". LIGO. Retrieved 29 May 2023.
"Superevent info - S230531f". LIGO. Retrieved 31 May 2023.
"Superevent info - S230601bf". LIGO. Retrieved 1 June 2023.
"Superevent info - S230604z". LIGO. Retrieved 4 June 2023.
"Superevent info - S230605o". LIGO. Retrieved 5 June 2023.
"Superevent info - S230606d". LIGO. Retrieved 6 June 2023.
"Superevent info - S230606z". LIGO. Retrieved 6 June 2023.
"Superevent info - S230608as". LIGO. Retrieved 8 June 2023.
"Superevent info - S230609a". LIGO. Retrieved 9 June 2023.
"Superevent info - S230609u". LIGO. Retrieved 9 June 2023.
"Superevent info - S230615av". LIGO. Retrieved 15 June 2023.
"Superevent info - S230615ax". LIGO. Retrieved 15 June 2023.
"Superevent info - S230615az". LIGO. Retrieved 15 June 2023.
"Superevent info - S230623at". LIGO. Retrieved 23 June 2023.
"Superevent info - S230624av". LIGO. Retrieved 24 June 2023.
"Superevent info - S230627c". LIGO. Retrieved 27 June 2023.
"Superevent info - S230628aj". LIGO. Retrieved 28 June 2023.
"Superevent info - S230628ax". LIGO. Retrieved 28 June 2023.
"Superevent info - S230630am". LIGO. Retrieved 30 June 2023.
"Superevent info - S230630bq". LIGO. Retrieved 30 June 2023.
"Superevent info - S230702an". LIGO. Retrieved 2 July 2023.
"Superevent info - S230704f". LIGO. Retrieved 4 July 2023.
"Superevent info - S230704bd". LIGO. Retrieved 4 July 2023.
"Superevent info - S230706ah". LIGO. Retrieved 6 July 2023.
"Superevent info - S230707ai". LIGO. Retrieved 7 July 2023.
"Superevent info - S230708t". LIGO. Retrieved 8 July 2023.
"Superevent info - S230708z". LIGO. Retrieved 8 July 2023.
"Superevent info - S230708cf". LIGO. Retrieved 8 July 2023.
"Superevent info - S230709i". LIGO. Retrieved 9 July 2023.
"Superevent info - S230709bi". LIGO. Retrieved 9 July 2023.
"Superevent info - S230711b". LIGO. Retrieved 11 July 2023.
"Superevent info - S230712d". LIGO. Retrieved 12 July 2023.
"Superevent info - S230712ak". LIGO. Retrieved 12 July 2023.
"Superevent info - S230713ar". LIGO. Retrieved 13 July 2023.
"Superevent info - S230716j". LIGO. Retrieved 16 July 2023.
"Superevent info - S230716o". LIGO. Retrieved 16 July 2023.
"Superevent info - S230723ac". LIGO. Retrieved 23 July 2023.
"Superevent info - S230725am". LIGO. Retrieved 25 July 2023.
"Superevent info - S230726a". LIGO. Retrieved 26 July 2023.
"Superevent info - S230728ap". LIGO. Retrieved 28 July 2023.
"Superevent info - S230729z". LIGO. Retrieved 29 July 2023.
"Superevent info - S230731an". LIGO. Retrieved 31 July 2023.
"Superevent info - S230802aq". LIGO. Retrieved 2 August 2023.
"Superevent info - S230805x". LIGO. Retrieved 5 August 2023.
"Superevent info - S230805bm". LIGO. Retrieved 5 August 2023.
"Superevent info - S230806ak". LIGO. Retrieved 6 August 2023.
"Superevent info - S230807f". LIGO. Retrieved 7 August 2023.
"Superevent info - S230811n". LIGO. Retrieved 11 August 2023.
"Superevent info - S230814r". LIGO. Retrieved 14 August 2023.
"Superevent info - S230814ah". LIGO. Retrieved 14 August 2023.
"Superevent info - S230819ax". LIGO. Retrieved 19 August 2023.
"Superevent info - S230820bq". LIGO. Retrieved 20 August 2023.
"Superevent info - S230822ac". LIGO. Retrieved 22 August 2023.
"Superevent info - S230822bm". LIGO. Retrieved 22 August 2023.
"Superevent info - S230824r". LIGO. Retrieved 24 August 2023.
"Superevent info - S230824bp". LIGO. Retrieved 24 August 2023.
"Superevent info - S230825k". LIGO. Retrieved 25 August 2023.
"Superevent info - S230825aq". LIGO. Retrieved 25 August 2023.
"Superevent info - S230828aq". LIGO. Retrieved 28 August 2023.
"Superevent info - S230830q". LIGO. Retrieved 30 August 2023.
"Superevent info - S230831e". LIGO. Retrieved 31 August 2023.
"Superevent info - S230902af". LIGO. Retrieved 2 September 2023.
"Superevent info - S230904n". LIGO. Retrieved 4 September 2023.
"Superevent info - S230904bg". LIGO. Retrieved 4 September 2023.
"Superevent info - S230908aa". LIGO. Retrieved 8 September 2023.
"Superevent info - S230911ae". LIGO. Retrieved 11 September 2023.
"Superevent info - S230911ar". LIGO. Retrieved 12 September 2023.
"Superevent info - S230914ak". LIGO. Retrieved 14 September 2023.
"Superevent info - S230916bm". LIGO. Retrieved 16 September 2023.
"Superevent info - S230917af". LIGO. Retrieved 17 September 2023.
"Superevent info - S230919bj". LIGO. Retrieved 19 September 2023.
"Superevent info - S230920al". LIGO. Retrieved 20 September 2023.
"Superevent info - S230922g". LIGO. Retrieved 22 September 2023.
"Superevent info - S230922q". LIGO. Retrieved 22 September 2023.
"Superevent info - S230924an". LIGO. Retrieved 24 September 2023.
"Superevent info - S230925cj". LIGO. Retrieved 26 September 2023.
"Superevent info - S230927g". LIGO. Retrieved 27 September 2023.
"Superevent info - S230927l". LIGO. Retrieved 27 September 2023.
"Superevent info - S230927be". LIGO. Retrieved 27 September 2023.
"Superevent info - S230928cb". LIGO. Retrieved 28 September 2023.
"Superevent info - S230930al". LIGO. Retrieved 30 September 2023.
"Superevent info - S231001aq". LIGO. Retrieved 1 October 2023.
"Superevent info - S231004bq". LIGO. Retrieved 4 October 2023.
"Superevent info - S231005j". LIGO. Retrieved 5 October 2023.
"Superevent info - S231005ah". LIGO. Retrieved 5 October 2023.
"Superevent info - S231007w". LIGO. Retrieved 7 October 2023.
"Superevent info - S231007am". LIGO. Retrieved 7 October 2023.
"Superevent info - S231008ap". LIGO. Retrieved 8 October 2023.
"Superevent info - S231014r". LIGO. Retrieved 14 October 2023.
"Superevent info - S231017e". LIGO. Retrieved 17 October 2023.
"Superevent info - S231018br". LIGO. Retrieved 18 October 2023.
"Superevent info - S231020ba". LIGO. Retrieved 20 October 2023.
"Superevent info - S231020bw". LIGO. Retrieved 20 October 2023.
"Superevent info - S231025a". LIGO. Retrieved 25 October 2023.
"Superevent info - S231025ap". LIGO. Retrieved 25 October 2023.

External links

"Detections". LIGO.
Video (3:10): LIGO Orrey (1 Dec 2018) on YouTube

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

[12] The detection date of a GW event is indicated by its designation; i.e., event GW150914 was detected on 2015-09-14.

[13] The relatively large and distant area of the sky within which it is claimed to be possible to localize the source.

[14] 1 Mpc is approximately 3.26 Mly.

[15] 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.

[16] The chirp mass 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. It is related to, but less than, the geometric mean $(m_{geo})$ of the binary masses, according to $m_{geo}\left({\frac {m_{geo}}{m_{1}+m_{2}}}\right)^{1/5}$ , thus ranging from ~87% of $m_{geo}$ when the masses are the same to ~78% when they differ by an order of magnitude.

[20] The dimensionless effective inspiral spin parameter is: ${\frac {m_{1}a_{1}cos\theta _{LS_{1}}+m_{2}a_{2}cos\theta _{LS_{2}}}{m_{1}+m_{2}}},$ [12] where $m$ is the mass of a black hole, $a$ is its spin, and $\theta _{LS}$ is the angle between the orbital angular momentum and a merging black hole's spin (ranging from $0$ when aligned to $\pi$ when antialigned). It is the mass-weighted linear combination of the components of the black holes' spins aligned with the orbital axis[12][11] and has values ranging from −1 to 1 (the extremes correspond to situations with both black hole spins exactly antialigned and aligned, respectively, with orbital angular momentum).[13] This is the spin parameter most relevant to the evolution of the inspiral gravitational waveform, and it can be measured more accurately than those of the premerger BHs.[14]

[22] Values of the dimensionless spin parameter $a=$ c J/G M² for a black hole 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.[15]

[24] Spin estimate is 0.26+0.52
−0.24.[16]

[25] Spin estimate is 0.32+0.54
−0.29.[16]

[36] Based on a descending spin-down chirp observed in GW post-merger, a magnetar was produced that survived at least 5 seconds.[26]

[38] 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.[27]

[67] 1 Mpc is approximately 3.26 Mly.

[68] Which instruments observed the event. (H = LIGO Hanford, L=LIGO Livingston, V=Virgo)

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

[82] 1 Mpc is approximately 3.26 Mly.

[83] Which instruments observed the event. (H = LIGO Hanford, L=LIGO Livingston, V=Virgo)

[84] The chance a random signal of this significance would occur at any point in O3's 11-month run. Calculated by 1 - (1-false alarm rate in Hz)^28,512,000. This is not the chance of the given signal being 'real' or not: Background contamination (such as earthquakes) can cause statistically significant signals as well, and although four detections have a >50% chance to have occurred randomly in O3, there is only a 19.4% chance that none of these signals would be real.

[85] Probability that both components have mass < 3 M_☉

[86] Probability that one component has mass < 3 M_☉ and the other has mass > 5 M_☉

[87] Probability that both components have mass > 5 M_☉

[88] Probability that at least one component has a mass in the range 3-5 M_☉, between those of known neutron stars and black holes, a range sometimes identified as the "lower" mass gap

[89] Probability that the source is terrestrial or non-cosmological (e.g. foreground noises and signals [e.g. "noise"] or a technical/systematic error ["glitch"])

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

[103] 1 Mpc is approximately 3.26 Mly.

[104] Which instruments observed the event. (H = LIGO Hanford, L=LIGO Livingston, V=Virgo)

[105] The chance a random signal of this significance would occur at any point in O4's 20-month run. Calculated by 1 - (1-false alarm rate in Hz)^46,656,000. This is not the chance of the given signal being 'real' or not: Background contamination (such as earthquakes) can cause statistically significant signals as well.

[106] Probability that both components have mass < 3 M_☉

[107] Probability that one component has mass < 3 M_☉ and the other has mass > 5 M_☉

[108] Probability that both components have mass > 5 M_☉

[109] Probability that at least one component has a mass in the range 3-5 M_☉, between those of known neutron stars and black holes, a range sometimes identified as the "lower" mass gap

[110] Probability that the source is terrestrial or non-cosmological (e.g. foreground noises and signals [e.g. "noise"] or a technical/systematic error ["glitch"])

[115] During O4, random noise is expected to be as significant as this event 39 times; 0.5 times by this point in the run.

[117] During O4, random noise is expected to be as significant as this event 35 times; 0.5 times by this point in the run.

[119] During O4, random noise is expected to be as significant as this event 10 times; 0.2 times by this point in the run.

[121] During O4, random noise is expected to be as significant as this event 14 times; 0.3 times by this point in the run.

[123] During O4, random noise is expected to be as significant as this event 33 times; 0.7 times by this point in the run.

[125] During O4, random noise is expected to be as significant as this event 13 times; 0.3 times by this point in the run.

[128] During O4, random noise is expected to be as significant as this event 40 times; 1 time by this point in the run.

[131] During O4, random noise is expected to be as significant as this event 13 times; 0.4 times by this point in the run.

[135] During O4, random noise is expected to be as significant as this event 19 times; 0.7 times by this point in the run.

[140] During O4, random noise is expected to be as significant as this event 7 times; 0.4 times by this point in the run.

[142] During O4, random noise is expected to be as significant as this event 24 times; 1 time by this point in the run.

[144] During O4, random noise is expected to be as significant as this event 7 times; 0.4 times by this point in the run.

[146] During O4, random noise is expected to be as significant as this event 43 times; 3 times by this point in the run.

[147] During O4, random noise is expected to be as significant as this event 9 times; 0.6 times by this point in the run.

[149] During O4, random noise is expected to be as significant as this event 42 times; 3 times by this point in the run.

[151] During O4, random noise is expected to be as significant as this event 44 times; 3 times by this point in the run.

[153] During O4, random noise is expected to be as significant as this event 10 times; 0.8 times by this point in the run.

[160] During O4, random noise is expected to be as significant as this event 28 times; 2 times by this point in the run.

[167] During O4, random noise is expected to be as significant as this event 24 times; 2 times by this point in the run.

[170] During O4, random noise is expected to be as significant as this event 22 times; 2 times by this point in the run.

[172] During O4, random noise is expected to be as significant as this event 46 times; 5 times by this point in the run.

[174] During O4, random noise is expected to be as significant as this event 21 times; 2 times by this point in the run.

[176] During O4, random noise is expected to be as significant as this event 30 times; 3 times by this point in the run.

[178] During O4, random noise is expected to be as significant as this event 31 times; 3 times by this point in the run.

[180] During O4, random noise is expected to be as significant as this event 23 times; 3 times by this point in the run.

[183] During O4, random noise is expected to be as significant as this event 23 times; 3 times by this point in the run.

[186] During O4, random noise is expected to be as significant as this event 5 times; 0.6 times by this point in the run.

[192] During O4, random noise is expected to be as significant as this event 13 times; 2 times by this point in the run.

[201] During O4, random noise is expected to be as significant as this event 17 times; 3 times by this point in the run.

[205] During O4, random noise is expected to be as significant as this event 23 times; 4 times by this point in the run.

[208] During O4, random noise is expected to be as significant as this event 16 times; 3 times by this point in the run.

[210] During O4, random noise is expected to be as significant as this event 24 times; 5 times by this point in the run.

[212] During O4, random noise is expected to be as significant as this event 6 times; 1 time by this point in the run.

[215] During O4, random noise is expected to be as significant as this event 19 times; 4 times by this point in the run.

[218] During O4, random noise is expected to be as significant as this event 37 times; 8 times by this point in the run.

[220] During O4, random noise is expected to be as significant as this event 42 times; 9 times by this point in the run.

[223] During O4, random noise is expected to be as significant as this event 18 times; 4 times by this point in the run.

[226] During O4, random noise is expected to be as significant as this event 41 times; 9 times by this point in the run.

[228] During O4, random noise is expected to be as significant as this event 21 times; 5 times by this point in the run.

[235] During O4, random noise is expected to be as significant as this event 10 times; 2 times by this point in the run.

[237] During O4, random noise is expected to be as significant as this event 34 times; 8 times by this point in the run.

[244] During O4, random noise is expected to be as significant as this event 36 times; 9 times by this point in the run.

[248] During O4, random noise is expected to be as significant as this event 28 times; 7 times by this point in the run.

[250] During O4, random noise is expected to be as significant as this event 10 times; 3 times by this point in the run.

[254] During O4, random noise is expected to be as significant as this event 29 times; 8 times by this point in the run.

[256] During O4, random noise is expected to be as significant as this event 38 times; 11 times by this point in the run.

[260] During O4, random noise is expected to be as significant as this event 44 times; 13 times by this point in the run.

[262] During O4, random noise is expected to be as significant as this event 17 times; 5 times by this point in the run.

[1] "GW150914 - The First Direct Detection of Gravitational Waves". www.ligo.org. Retrieved 2023-03-15.

[LSC_News-2] "LSC News". www.ligo.org. Retrieved 2023-03-15.

[3] The LIGO Scientific Collaboration; the Virgo Collaboration; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abraham, S.; Acernese, F.; Ackley, K.; Adams, C.; Adhikari, R. X.; Adya, V. B. (2019-09-04). "GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs". Physical Review X. 9 (3): 031040. arXiv:1811.12907. Bibcode:2019PhRvX...9c1040A. doi:10.1103/PhysRevX.9.031040. ISSN 2160-3308. S2CID 119366083.

[4] Burtnyk, Kimberly (2019-10-01). "LIGO's Commissioning Break Commences". LIGO Lab | Caltech. Retrieved 2020-07-01.

[:0-5] "LIGO Suspends Third Observing Run (O3)". LIGO Lab. Caltech. Retrieved 20 April 2020.

[planspage-6] Ligo, Virgo and Kagra Observing Run Plans

[7] "GCN/LVC Notices". Goddard Space Flight Center. Retrieved 2019-11-11.

[ARX-20181126-8] Fragione, Giacomo; et al. (2019). "Black Hole and Neutron Star Mergers in Galactic Nuclei". Monthly Notices of the Royal Astronomical Society. 488 (1): 47–63. arXiv:1811.10627. Bibcode:2019MNRAS.488...47F. doi:10.1093/mnras/stz1651. S2CID 85459844.

[CNN-20190503-9] Strickland, Ashley (3 May 2019). "Scientists may have detected violent collision between neutron star, black hole". CNN. Retrieved 3 May 2019.

[Nov5-10] Nitz, Alexander H. (25 February 2019). "1-OGC: The first open gravitational-wave catalog of binary mergers from analysis of public Advanced LIGO data". Astrophysical Journal. 872 (2): 195. arXiv:1811.01921. Bibcode:2019ApJ...872..195N. doi:10.3847/1538-4357/ab0108. S2CID 119389481.

[Nov30-11] Abbott, B.P.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (2019). "GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs". Physical Review X. 9 (3): 031040. arXiv:1811.12907. Bibcode:2019PhRvX...9c1040A. doi:10.1103/PhysRevX.9.031040. S2CID 119366083.

[50SM2017-17] 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 (22): 221101. arXiv:1706.01812. Bibcode:2017PhRvL.118v1101A. doi:10.1103/PhysRevLett.118.221101. PMID 28621973. S2CID 206291714.

[Farr2017-18] Farr, W. M.; Stevenson, S.; Miller, M. C.; Mandel, I.; F arr, B.; Vecchio, A. (2017). "Distinguishing spin-aligned and isotropic black hole populations with gravitational waves". Nature. 548 (7667): 426–429. arXiv:1706.01385. Bibcode:2017Natur.548..426F. doi:10.1038/nature23453. PMID 28836595. S2CID 4411726.

[Vitale2017-19] Vitale, S.; Lynch, R.; Raymond, V.; Sturani, R.; Veitch, J.; Graff, P. (2017). "Parameter estimation for heavy binary-black holes with networks of second-generation gravitational-wave detectors". Physical Review D. 95 (6): 064053. arXiv:1611.01122. Bibcode:2017PhRvD..95f4053V. doi:10.1103/PhysRevD.95.064053. hdl:1721.1/109575. S2CID 118511535.

[PRL-171016-21] 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): 161101. arXiv:1710.05832. Bibcode:2017PhRvL.119p1101A. doi:10.1103/PhysRevLett.119.161101. PMID 29099225. S2CID 217163611.

[Improved-23] The LIGO Scientific Collaboration and The Virgo Collaboration (3 June 2016). "An improved analysis of GW150914 using a fully spin-precessing waveform model". Physical Review X. 6 (4): 041014. arXiv:1606.01210. Bibcode:2016PhRvX...6d1014A. doi:10.1103/PhysRevX.6.041014. S2CID 18217435.

[PRL116-061102-26] 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. S2CID 124959784.

[PhysicsWorld-2016-02-11-27] Tushna Commissariat (11 February 2016). "LIGO detects first ever gravitational waves – from two merging black holes". Physics World.

[PRX2016-28] 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 (4): 041015. arXiv:1606.04856. Bibcode:2016PhRvX...6d1015A. doi:10.1103/PhysRevX.6.041015. S2CID 31926886.

[PRL116-241103-29] 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. S2CID 118651851.

[APOD-2016-06-15-30] Nemiroff, R.; Bonnell, J., eds. (15 June 2016). "GW151226: A Second Confirmed Source of Gravitational Radiation". Astronomy Picture of the Day. NASA.

[NYT-20170601-31] 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-32] Abbott, B.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): L35. arXiv:1711.05578. Bibcode:2017ApJ...851L..35A. doi:10.3847/2041-8213/aa9f0c. S2CID 9030576.

[PRL-20171006-33] Abbott, B.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. PMID 29053306. S2CID 46829350.
"Gravitational waves from a binary black hole merger observed by LIGO and Virgo" (PDF). LIGO Scientific Collaboration (Press release).

[104] "Gravitational waves from a binary black hole merger observed by LIGO and Virgo" (PDF). LIGO Scientific Collaboration (Press release).

[NYT-20170927-34] Overbye, Dennis (27 September 2017). "New Gravitational Wave Detection From Colliding Black Holes". The New York Times. Retrieved 28 September 2017.

[van_Putten2019-35] van Putten, Maurice H.P.M.; Della Valle, Massimo (January 2019). "Observational evidence for extended emission to GW170817". Monthly Notices of the Royal Astronomical Society: Letters. 482 (1): L46–L49. arXiv:1806.02165. Bibcode:2019MNRAS.482L..46V. doi:10.1093/mnrasl/sly166.

[DroutPiro2017-37] 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". Science. 358 (6370): 1570–1574. arXiv:1710.05443. Bibcode:2017Sci...358.1570D. doi:10.1126/science.aaq0049. PMID 29038375.

[ApJ2017.10-39] 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. Bibcode:2017ApJ...848L..12A. doi:10.3847/2041-8213/aa91c9.

[SM-20171016-40] Cho, Adrian (16 October 2017). "Merging neutron stars generate gravitational waves and a celestial light show". Science. Retrieved 16 October 2017.

[GWTC-2-41] The LIGO Scientific Collaboration; the Virgo Collaboration (2021). "GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo during the First Half of the Third Observing Run". Physical Review X. 11 (2): 021053. arXiv:2010.14527. Bibcode:2021PhRvX..11b1053A. doi:10.1103/PhysRevX.11.021053. S2CID 225094244.

[S190412m-42] "Superevent info - S190412m". LIGO. Retrieved 12 April 2019.

[arxiv2004.08342-43] The LIGO Scientific Collaboration; the Virgo Collaboration; Abbott, R.; et al. (17 April 2020). "GW190412: Observation of a Binary-Black-Hole Coalescence with Asymmetric Masses". Physical Review D. 102 (4): 043015. arXiv:2004.08342. Bibcode:2020PhRvD.102d3015A. doi:10.1103/PhysRevD.102.043015. S2CID 215814461.

[Pozanenko2019-44] Позаненко, А. С.; Минаев, П. Ю.; Гребенев, С. А.; Человеков, И. В. (2019). "Наблюдение в гамма-диапазоне второго связанного со слиянием нейтронных звезд события LIGO/Virgo S190425z". Письма В Астрономический Журнал: Астрономия И Космическая Астрофизика (in Russian). 45 (11): 768–786. arXiv:1912.13112. doi:10.1134/S032001081911007X. S2CID 239427905.

[45] "Gravitational waves reveal a second neutron star collision". 8 January 2020.

[S190425z-46] "Superevent info - S190425z". LIGO. Retrieved 25 April 2019.

[arxiv2001.01761-47] The LIGO Scientific Collaboration; the Virgo Collaboration; et al. (6 January 2020). "GW190425: Observation of a Compact Binary Coalescence with Total Mass ~ 3.4 M_☉". The Astrophysical Journal. 892 (1): L3. arXiv:2001.01761. Bibcode:2020ApJ...892L...3A. doi:10.3847/2041-8213/ab75f5. S2CID 210023687.

[PhysRevLett-48] Abbott, R.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (2 September 2020). "GW190521: A Binary Black Hole Merger with a Total Mass of 150 M ⊙". Physical Review Letters. 125 (10): 101102. arXiv:2009.01075. Bibcode:2020PhRvL.125j1102A. doi:10.1103/PhysRevLett.125.101102. PMID 32955328. S2CID 221447506.

[AstroJ-49] Abbott, R.; et al. (LIGO Scientific Collaboration and Virgo Collaboration) (2 September 2020). "Properties and Astrophysical Implications of the 150 M ⊙ Binary Black Hole Merger GW190521". The Astrophysical Journal. 900 (1): L13. arXiv:2009.01190. Bibcode:2020ApJ...900L..13A. doi:10.3847/2041-8213/aba493. hdl:11343/273616. S2CID 221447444.

[50] "Black hole or neutron star?". June 23, 2020.

[S190814bv-51] "Superevent info - S190814bv". LIGO. Retrieved 15 August 2019.

[SA-20190816-52] Starr, Michelle (16 August 2019). "Early Reports Indicate We May Have Detected a Black Hole And Neutron Star Collision". ScienceAlert.com. Retrieved 16 August 2019.

[GZM-20190826-53] Mandelbum, Ryan F. (26 August 2019). "Mystery Deepens Around Newly Detected Ripples in Space-Time". Gizmodo. Retrieved 26 August 2019.

[SA-20200211-54] Starr, Michelle (11 February 2020). "First Papers on The Black Hole-Neutron Star Merger Are In. Here's What We Didn't See". ScienceAlert.com. Retrieved 11 February 2020.

[ARX-20200205-55] Ackley, K.; et al. (5 February 2020). "Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger S190814bv". arXiv:2002.01950v1 [astro-ph.SR].

[NYT-20200624-56] Overbye, Dennis (24 June 2020). "A Black Hole's Lunch Provides a Treat for Astronomers - Scientists have discovered the heaviest known neutron star, or maybe the lightest known black hole: "Either way it breaks a record."". The New York Times. Retrieved 24 June 2020.

[SA-20200624-57] Starr, Michelle (24 June 2020). "Astronomers Detect First-Ever Mystery Object in The 'Mass Gap' of Cosmic Collisions". ScienceAlert.com. Retrieved 24 June 2020.

[EA-20200623-58] University of Birmingham (23 June 2020). "Gravitational wave scientists grapple with the cosmic mystery of GW190814". EurekAlert!. Retrieved 24 June 2020.

[AJL-20200623-59] Abbott, R.; et al. (23 June 2020). "GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object". The Astrophysical Journal Letters. 896 (2): L44. arXiv:2006.12611. Bibcode:2020ApJ...896L..44A. doi:10.3847/2041-8213/ab960f.

[O3B-60] The LIGO Scientific Collaboration; et al. (17 November 2021). "GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run". arXiv:2111.03606. {{cite journal}}: Cite journal requires |journal= (help)

[BHNSmerger_June21-61] Abbott, R.; et al. (2021). "Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences". The Astrophysical Journal Letters. 915 (1): L5. arXiv:2106.15163. Bibcode:2021ApJ...915L...5A. doi:10.3847/2041-8213/ac082e. S2CID 235670241.

[S200105ae-62] "Superevent info - S200105ae". LIGO. Retrieved 6 January 2020.

[Bustillo2022-63] Bustillo, Juan Calderon; Sanchis-Gual, Nicolas; Leong, Samson H. W.; Chandra, Koustav; Torres-Forne, Alejandro; Font, Jose A.; Herdeiro, Carlos; Radu, Eugen; Wong, Isaac C. F.; Li, T. G. F. (2022). "Searching for vector boson-star mergers within LIGO-Virgo intermediate-mass black-hole merger candidates". arXiv:2206.02551 [gr-qc].

[Hourihane2022-64] Hourihane, Sophie; Chatziioannou, Katerina; Wijngaarden, Marcella; Davis, Derek; Littenberg, Tyson; Cornish, Neil (15 August 2022). "Accurate modeling and mitigation of overlapping signals and glitches in gravitational-wave data". Physical Review D. 106 (4): 042006. arXiv:2205.13580. Bibcode:2022PhRvD.106d2006H. doi:10.1103/PhysRevD.106.042006. S2CID 249152318.

[S200115j-65] "Superevent info - S200115j". LIGO. Retrieved 15 January 2020.

[66] Hartono, Naomi (29 June 2023). "15 Years of Radio Data Reveals Evidence of Space-Time Murmur". NASA. Retrieved 3 July 2023.

[Nitz2020-69] Nitz, Alexander H.; Dent, Thomas; Davies, Gareth S.; Kumar, Sumit; Capano, Collin D.; Harry, Ian; Mozzon, Simone; Nuttall, Laura; Lundgren, Andrew; Tápai, Márton (12 March 2020). "2-OGC: Open Gravitational-wave Catalog of Binary Mergers from Analysis of Public Advanced LIGO and Virgo Data". The Astrophysical Journal. 891 (2): 123. arXiv:1910.05331. Bibcode:2020ApJ...891..123N. doi:10.3847/1538-4357/ab733f. S2CID 204403263.

[Venumadhav2019b-70] Venumadhav, Tejaswi; Zackay, Barak; Roulet, Javier; Dai, Liang; Zaldarriaga, Matias (2020). "New Binary Black Hole Mergers in the Second Observing Run of Advanced LIGO and Advanced Virgo". Physical Review D. 101 (8): 083030. arXiv:1904.07214. Bibcode:2020PhRvD.101h3030V. doi:10.1103/PhysRevD.101.083030. S2CID 119188594.

[Zackay2019-71] Zackay, Barak; Dai, Liang; Venumadhav, Tejaswi; Roulet, Javier; Zaldarriaga, Matias (2021). "Detecting Gravitational Waves With Disparate Detector Responses: Two New Binary Black Hole Mergers". Phys. Rev. D. 104 (8): 063030. arXiv:1910.09528. Bibcode:2020PhRvD.101h3030V. doi:10.1103/PhysRevD.101.083030. S2CID 119188594.

[72] "Real-time alerts and circulars tracker" – via nasa.gov.

[LGS2018.10-73] "Observing Plans and Public Alerts". www.ligo.org. LIGO Scientific Collaboration. October 2018. Retrieved 2018-10-28.

[74] Singer, Leo P. (16 March 2017). "What constitutes an open, public alert?" (PDF). LSC (LIGO Scientific Collaboration). Retrieved 30 October 2018 – via gw-astronomy.org.

[75] "GraceDB — Gravitational Wave Candidate Event Database" – via ligo.org.

[76] "Real-time alerts and circulars tracker" – via nasa.gov.

[77] "LIGO Announces Commissioning Break". LIGO Lab | Caltech. Retrieved 7 November 2019.

[78] "KAGRA Gravitational-wave Telescope Starts Observation « KAGRA Large-scale Cryogenic Graviationai wave Telescope Project" (in Japanese). Retrieved 2020-02-27.

[79] "KAGRA to Join LIGO and Virgo in Hunt for Gravitational Waves". LIGO Lab | Caltech. Retrieved 2019-10-06.

[80] "LIGO Laboratory's Response to COVID-19". LIGO Lab. Caltech. Retrieved 24 March 2020.

[S190901ap-90] "Superevent info - S190901ap". LIGO. Retrieved 6 September 2019.

[S190910d-91] "Superevent info - S190910d". LIGO. Retrieved 10 September 2019.

[S190910h-92] "Superevent info - S190910h". LIGO. Retrieved 10 September 2019.

[S190923y-93] "Superevent info - S190923y". LIGO. Retrieved 24 September 2019.

[S190930t-94] "Superevent info - S190930t". LIGO. Retrieved 30 September 2019.

[S191205ah-95] "Superevent info - S191205ah". LIGO. Retrieved 5 December 2019.

[S191213g-96] "Superevent info - S191213g". LIGO. Retrieved 14 December 2019.

[S200213t-97] "Superevent info - S200213t". LIGO. Retrieved 13 February 2020.

[98] "LIGO, Virgo and Kagra Observing Run Plans". LIGO Lab. Caltech. Retrieved 16 July 2022.

[99] Burtnyk, Kimberly. "Latest Update on Start of Next Observing Run (O4)". LIGO. Caltech. Retrieved 18 May 2023.

[100] "Detector status - 29 April 2023". gwosc.org. Retrieved 18 May 2023.

[101] "Detector status - 5 May 2023". gwosc.org.

[S230518h-111] "Superevent info - S230518h". LIGO. Retrieved 18 May 2023.

[S230520ae-112] "Superevent info - S230520ae". LIGO. Retrieved 21 May 2023.

[S230522a-113] "Superevent info - S230522a". LIGO. Retrieved 22 May 2023.

[S230522n-114] "Superevent info - S230522n". LIGO. Retrieved 22 May 2023.

[S230524b-116] "Superevent info - S230524b". LIGO. Retrieved 24 May 2023.

[S230525a-118] "Superevent info - S230525a". LIGO. Retrieved 25 May 2023.

[S230527bv-120] "Superevent info - S230527bv". LIGO. Retrieved 27 May 2023.

[S230528a-122] "Superevent info - S230528a". LIGO. Retrieved 28 May 2023.

[S230528ay-124] "Superevent info - S230528ay". LIGO. Retrieved 28 May 2023.

[S230528bt-126] "Superevent info - S230528bt". LIGO. Retrieved 28 May 2023.

[S230529ay-127] "Superevent info - S230529ay". LIGO. Retrieved 29 May 2023.

[S230531f-129] "Superevent info - S230531f". LIGO. Retrieved 31 May 2023.

[S230601bf-130] "Superevent info - S230601bf". LIGO. Retrieved 1 June 2023.

[S230604z-132] "Superevent info - S230604z". LIGO. Retrieved 4 June 2023.

[S230605o-133] "Superevent info - S230605o". LIGO. Retrieved 5 June 2023.

[S230606d-134] "Superevent info - S230606d". LIGO. Retrieved 6 June 2023.

[S230606z-136] "Superevent info - S230606z". LIGO. Retrieved 6 June 2023.

[S230608as-137] "Superevent info - S230608as". LIGO. Retrieved 8 June 2023.

[S230609a-138] "Superevent info - S230609a". LIGO. Retrieved 9 June 2023.

[S230609u-139] "Superevent info - S230609u". LIGO. Retrieved 9 June 2023.

[S230615av-141] "Superevent info - S230615av". LIGO. Retrieved 15 June 2023.

[S230615ax-143] "Superevent info - S230615ax". LIGO. Retrieved 15 June 2023.

[S230615az-145] "Superevent info - S230615az". LIGO. Retrieved 15 June 2023.

[S230623at-148] "Superevent info - S230623at". LIGO. Retrieved 23 June 2023.

[S230624av-150] "Superevent info - S230624av". LIGO. Retrieved 24 June 2023.

[S230627c-152] "Superevent info - S230627c". LIGO. Retrieved 27 June 2023.

[S230628aj-154] "Superevent info - S230628aj". LIGO. Retrieved 28 June 2023.

[S230628ax-155] "Superevent info - S230628ax". LIGO. Retrieved 28 June 2023.

[S230630am-156] "Superevent info - S230630am". LIGO. Retrieved 30 June 2023.

[S230630bq-157] "Superevent info - S230630bq". LIGO. Retrieved 30 June 2023.

[S230702an-158] "Superevent info - S230702an". LIGO. Retrieved 2 July 2023.

[S230704f-159] "Superevent info - S230704f". LIGO. Retrieved 4 July 2023.

[S230704bd-161] "Superevent info - S230704bd". LIGO. Retrieved 4 July 2023.

[S230706ah-162] "Superevent info - S230706ah". LIGO. Retrieved 6 July 2023.

[S230707ai-163] "Superevent info - S230707ai". LIGO. Retrieved 7 July 2023.

[S230708t-164] "Superevent info - S230708t". LIGO. Retrieved 8 July 2023.

[S230708z-165] "Superevent info - S230708z". LIGO. Retrieved 8 July 2023.

[S230708cf-166] "Superevent info - S230708cf". LIGO. Retrieved 8 July 2023.

[S230709i-168] "Superevent info - S230709i". LIGO. Retrieved 9 July 2023.

[S230709bi-169] "Superevent info - S230709bi". LIGO. Retrieved 9 July 2023.

[S230711b-171] "Superevent info - S230711b". LIGO. Retrieved 11 July 2023.

[S230712d-173] "Superevent info - S230712d". LIGO. Retrieved 12 July 2023.

[S230712ak-175] "Superevent info - S230712ak". LIGO. Retrieved 12 July 2023.

[S230713ar-177] "Superevent info - S230713ar". LIGO. Retrieved 13 July 2023.

[S230716j-179] "Superevent info - S230716j". LIGO. Retrieved 16 July 2023.

[S230716o-181] "Superevent info - S230716o". LIGO. Retrieved 16 July 2023.

[S230723ac-182] "Superevent info - S230723ac". LIGO. Retrieved 23 July 2023.

[S230725am-184] "Superevent info - S230725am". LIGO. Retrieved 25 July 2023.

[S230726a-185] "Superevent info - S230726a". LIGO. Retrieved 26 July 2023.

[S230728ap-187] "Superevent info - S230728ap". LIGO. Retrieved 28 July 2023.

[S230729z-188] "Superevent info - S230729z". LIGO. Retrieved 29 July 2023.

[S230731an-189] "Superevent info - S230731an". LIGO. Retrieved 31 July 2023.

[S230802aq-190] "Superevent info - S230802aq". LIGO. Retrieved 2 August 2023.

[S230805x-191] "Superevent info - S230805x". LIGO. Retrieved 5 August 2023.

[S230805bm-193] "Superevent info - S230805bm". LIGO. Retrieved 5 August 2023.

[S230806ak-194] "Superevent info - S230806ak". LIGO. Retrieved 6 August 2023.

[S230807f-195] "Superevent info - S230807f". LIGO. Retrieved 7 August 2023.

[S230811n-196] "Superevent info - S230811n". LIGO. Retrieved 11 August 2023.

[S230814r-197] "Superevent info - S230814r". LIGO. Retrieved 14 August 2023.

[S230814ah-198] "Superevent info - S230814ah". LIGO. Retrieved 14 August 2023.

[S230819ax-199] "Superevent info - S230819ax". LIGO. Retrieved 19 August 2023.

[S230820bq-200] "Superevent info - S230820bq". LIGO. Retrieved 20 August 2023.

[S230822ac-202] "Superevent info - S230822ac". LIGO. Retrieved 22 August 2023.

[S230822bm-203] "Superevent info - S230822bm". LIGO. Retrieved 22 August 2023.

[S230824r-204] "Superevent info - S230824r". LIGO. Retrieved 24 August 2023.

[S230824bp-206] "Superevent info - S230824bp". LIGO. Retrieved 24 August 2023.

[S230825k-207] "Superevent info - S230825k". LIGO. Retrieved 25 August 2023.

[S230825aq-209] "Superevent info - S230825aq". LIGO. Retrieved 25 August 2023.

[S230828aq-211] "Superevent info - S230828aq". LIGO. Retrieved 28 August 2023.

[S230830q-213] "Superevent info - S230830q". LIGO. Retrieved 30 August 2023.

[S230831e-214] "Superevent info - S230831e". LIGO. Retrieved 31 August 2023.

[S230902af-216] "Superevent info - S230902af". LIGO. Retrieved 2 September 2023.

[S230904n-217] "Superevent info - S230904n". LIGO. Retrieved 4 September 2023.

[S230904bg-219] "Superevent info - S230904bg". LIGO. Retrieved 4 September 2023.

[S230908aa-221] "Superevent info - S230908aa". LIGO. Retrieved 8 September 2023.

[S230911ae-222] "Superevent info - S230911ae". LIGO. Retrieved 11 September 2023.

[S230911ar-224] "Superevent info - S230911ar". LIGO. Retrieved 12 September 2023.

[S230914ak-225] "Superevent info - S230914ak". LIGO. Retrieved 14 September 2023.

[S230916bm-227] "Superevent info - S230916bm". LIGO. Retrieved 16 September 2023.

[S230917af-229] "Superevent info - S230917af". LIGO. Retrieved 17 September 2023.

[S230919bj-230] "Superevent info - S230919bj". LIGO. Retrieved 19 September 2023.

[S230920al-231] "Superevent info - S230920al". LIGO. Retrieved 20 September 2023.

[S230922g-232] "Superevent info - S230922g". LIGO. Retrieved 22 September 2023.

[S230922q-233] "Superevent info - S230922q". LIGO. Retrieved 22 September 2023.

[S230924an-234] "Superevent info - S230924an". LIGO. Retrieved 24 September 2023.

[S230925cj-236] "Superevent info - S230925cj". LIGO. Retrieved 26 September 2023.

[S230927g-238] "Superevent info - S230927g". LIGO. Retrieved 27 September 2023.

[S230927l-239] "Superevent info - S230927l". LIGO. Retrieved 27 September 2023.

[S230927be-240] "Superevent info - S230927be". LIGO. Retrieved 27 September 2023.

[S230928cb-241] "Superevent info - S230928cb". LIGO. Retrieved 28 September 2023.

[S230930al-242] "Superevent info - S230930al". LIGO. Retrieved 30 September 2023.

[S231001aq-243] "Superevent info - S231001aq". LIGO. Retrieved 1 October 2023.

[S231004bq-245] "Superevent info - S231004bq". LIGO. Retrieved 4 October 2023.

[S231005j-246] "Superevent info - S231005j". LIGO. Retrieved 5 October 2023.

[S231005ah-247] "Superevent info - S231005ah". LIGO. Retrieved 5 October 2023.

[S231007w-249] "Superevent info - S231007w". LIGO. Retrieved 7 October 2023.

[S231007am-251] "Superevent info - S231007am". LIGO. Retrieved 7 October 2023.

[S231008ap-252] "Superevent info - S231008ap". LIGO. Retrieved 8 October 2023.

[S231014r-253] "Superevent info - S231014r". LIGO. Retrieved 14 October 2023.

[S231017e-255] "Superevent info - S231017e". LIGO. Retrieved 17 October 2023.

[S231018br-257] "Superevent info - S231018br". LIGO. Retrieved 18 October 2023.

[S231020ba-258] "Superevent info - S231020ba". LIGO. Retrieved 20 October 2023.

[S231020bw-259] "Superevent info - S231020bw". LIGO. Retrieved 20 October 2023.

[S231025a-261] "Superevent info - S231025a". LIGO. Retrieved 25 October 2023.

[S231025ap-263] "Superevent info - S231025ap". LIGO. Retrieved 25 October 2023.