List of gravitational wave observations
![](http://upload.wikimedia.org/wikipedia/commons/thumb/d/db/LIGO_measurement_of_gravitational_waves.svg/220px-LIGO_measurement_of_gravitational_waves.svg.png)
This is a list of observed/candidate gravitational wave events. Direct observation of gravitational waves,[n 1] which commenced with the detection of an event by LIGO in 2015, constitutes part of gravitational wave astronomy. LIGO has played a role in all subsequent detections to date, with Virgo joining in August 2017.
Nomenclature[]
Gravitational wave events are named starting with the prefix GW, while observations that trigger an event alert but have not (yet) been confirmed are named starting with the prefix S.[2] The next two digits indicate the year the event was observed, the middle two digits are the month of observation and the final two digits are the day of the month on which the event was observed. This is similar to the systematic naming for other kinds of astronomical event observations, such as those of gamma-ray bursts. Probable detections that are not confidently identified as gravitational wave events are designated LVT ("LIGO-Virgo trigger"). 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).[3][4] Some objects are in the mass gap between the largest predicted neutron star masses (Tolman–Oppenheimer–Volkoff limit) and the smallest known black holes.
Observations are made in "runs", three of them so far, with maintenance and upgrades of the detectors made between runs. The first run, O1, ran from 12 September 2015 to 19 January 2016, with O2 from 30 November 2016 to 25 August 2017.[5] O3 began on 1 April 2019; it is divided (so far) into O3a, from 1 April to 30 September 2019, and O3b, from 1 November 2019 to 27 March 2020.[6] Suspension of observation during October 2019 was for instrument upgrades and fixes, and cessation in March 2020 was due to the COVID-19 pandemic.[7][8]
List of gravitational wave events[]
![](http://upload.wikimedia.org/wikipedia/commons/thumb/5/50/O1%26O2.svg/500px-O1%26O2.svg.png)
![](http://upload.wikimedia.org/wikipedia/commons/thumb/0/05/O3_Alerts.svg/554px-O3_Alerts.svg.png)
GW event and time (UTC)[n 2] |
Date published |
Location area[n 3] (deg2) |
Luminosity distance (Mpc)[n 4] |
Energy radiated (c2M☉) [n 5] |
Chirp mass (M☉) [n 6] |
Effective spin[n 7] | Primary | Secondary | Remnant | Notes | Ref. | ||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
Type | Mass (M☉) | Type | Mass (M☉) | Type | Mass (M☉) | Spin[n 8] | |||||||||
GW150914 09:50:45 |
2016-02-11 | −170 |
−0.4 |
−1.5 |
−0.13 |
[n 9] |
−3.0 |
[n 10] |
−4.4 |
−3.0 |
−0.04 |
First GW detection; first BH merger observed |
[16][17][15] | ||
09∶54:43 |
2016-06-15 | −480 |
−0.5 |
−1.1 |
−0.19 |
−5.5 |
−4.8 |
−3.8 |
−0.11 |
Formerly candidate LVT151012; accepted as astrophysical since February 2019 |
[18][10][9] | ||||
GW151226 03:38:53 |
2016-06-15 | −190 |
−0.2 |
−0.3 |
−0.12 |
−3.2 |
−2.6 |
−1.5 |
−0.05 |
[19][20] | |||||
GW170104 10∶11:58 |
2017-06-01 | −410 |
−0.5 |
−1.7 |
−0.20 |
−5.6 |
−4.5 |
−3.5 |
−0.10 |
[11][21] | |||||
GW170608 02:01:16 |
2017-11-16 | −110 |
−0.1 |
−0.2 |
−0.07 |
−1.7 |
−2.1 |
−0.7 |
−0.04 |
Smallest BH progenitor masses to date |
[22] | ||||
18:56:29 |
2018-11-30 | −1320 |
−1.7 |
−4.7 |
−0.25 |
−10.2 |
−10.1 |
−10.2 |
−0.13 |
Largest progenitor masses until GW190521 | [10] | ||||
08:28:21 |
2018-11-30 | −380 |
−0.6 |
−1.6 |
−0.16 |
−6.0 |
−5.1 |
−3.7 |
−0.09 |
[10] | |||||
GW170814 10∶30:43 |
2017-09-27 | −210 |
−0.3 |
−1.1 |
−0.11 |
−3.0 |
−4.1 |
−2.4 |
−0.05 |
First announced detection by three observatories; first polarization measurement |
[23][24] | ||||
GW170817 12∶41:04 |
2017-10-16 | −0.001 |
−0.01 |
−0.10 |
−0.09 |
[n 11] |
First NS merger observed in GW; first detection of EM counterpart (GRB 170817A; AT 2017gfo); nearest event to date |
[14][27][28] | |||||||
02:25:09 |
2018-11-30 | −360 |
−0.5 |
−1.7 |
−0.21 |
−4.7 |
−5.2 |
−3.8 |
−0.08 |
[10] | |||||
13:13:58 |
2018-11-30 | −0.8 |
−3.2 |
−0.22 |
−6.6 |
−7.1 |
−6.6 |
−0.10 |
[10] | ||||||
GW190408_181802 2019-04-08 |
2020-10-27 | −590 |
−1.2 |
−0.19 |
−3.4 |
−3.5 |
−2.7 |
−0.07 |
[29] | ||||||
GW190412 2019-04-12 05:30:44 |
2020-04-17 | −170 |
−0.3 |
−0.11 |
−5.3 |
−1.0 |
−3.9 |
−0.07 |
First possible observation of a merger of two black holes of very different masses | [30][31] | |||||
GW190413_052954 2019-04-13 |
2020-10-27 | −1890 |
−3.7 |
−0.33 |
−7.4 |
−6.3 |
−8.4 |
−0.13 |
[29] | ||||||
GW190413_134308 2019-04-13 |
2020-10-27 | −2340 |
−4.6 |
−0.28 |
−9.6 |
−9.6 |
−10.3 |
−0.12 |
[29] | ||||||
GW190421_213856 2019-04-21 |
2020-10-27 | −1420 |
−6.6 |
−0.26 |
−6.6 |
−8.2 |
−8.1 |
−0.11 |
[29] | ||||||
GW190424_180648 2019-04-21 |
2020-10-27 | −1330 |
−4.2 |
−0.22 |
−6.9 |
−7.3 |
−9.2 |
−0.09 |
[29] | ||||||
2019-04-25 08:18:05 |
2020-01-06 | −72 |
−0.02 |
−0.01 |
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.[33]
It was published in 2020 that a gamma-ray burst was detected () ~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.[32] |
[34][35] | |||||||||
GW190521 2019-05-21 03:02:29 |
2020-09-02 | −2600 |
−1.9 |
−8 |
−0.36 |
−14 |
−18 |
−16 |
−0.12 |
Originally designated S190521g. Largest progenitor masses to date. | [36][37] | ||||
GW190814 2019-08-14 21:11:18 | 2020-06-23 | −45 |
−0.06 |
−0.061 |
−1.0 |
−0.09 |
−0.9 |
−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.[38] | [39][40][41][42][43] [44][45][46][47] | |||||
GW200105 2020-01-05 16:24:26 |
2021-06-29 | −0.07 |
−0.15 |
−1.5 |
−0.2 |
First event confirmed to be a black hole and neutron star merger. Originally designated S200105ae. | [48][49] | ||||||||
GW200115 2020-01-15 04:23:09 |
2021-06-29 | −100 |
−0.07 |
−0.35 |
−2.1 |
−0.3 |
Second event confirmed to be a black hole and neutron star merger. Originally designated S200115j. | [48][50] |
![](http://upload.wikimedia.org/wikipedia/commons/thumb/2/27/Gravitational_Wave_Transient_Catalog_1.png/950px-Gravitational_Wave_Transient_Catalog_1.png)
Candidate events and marginal detections[]
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:
candidate event | Detection time (UTC) |
date published | Luminosity distance (Mpc)[n 13] |
Detector [n 14] |
False Alarm Rate (Yr) |
Effective spin | Primary | Secondary | probability of terrestrial noise |
Notes | Ref | ||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
Type | Mass (M☉) | Type | Mass (M☉) | ||||||||||
150928 | 2015-09-28 10:49:00 | 2018-11-05 | H,L | 0.042 | -0.70 | 2.53 | 1.02 | ~0.9 | [51] | ||||
151011 | 2015-10-11 19:27:49 | 2019-10-11 | 1560+1090 −740 |
H,L | 0.12 | 0.09+0.29 −0.27 |
51+18 −12 |
31±12 | 0.92 | [52] | |||
151019 | 2015-10-19 00:23:16 | 2018-11-05 | H,L | 0.060 | 0.11 | 14.93 | 1.27 | ~0.9 | [51] | ||||
151205 | 2015-12-05 19:55:25 | 2019-10-11 | 3000+2400 −1600 |
H,L | 0.61 | 0.14+0.40 −0.38 |
67+28 −17 |
42+16 −19 |
0.47 | [52] | |||
151213 | 2015-12-13 00:12:20 | 2018-11-05 | H,L | 0.309 | -0.79 | 11.12 | 3.30 | 0.953 | [51] | ||||
151216A | 2015-12-16 09:24:16 | 2019-10-11 | 1620+1140 −910 |
H,L | 0.10 | 0.51+0.21 −0.57 |
41+15 −17 |
14.4+7.0 −6.3 |
0.82 | [52] | |||
151216B | 2015-12-16 18:49:30 | 2019-10-11 | 500+280 −250 |
H,L | 0.03 | −0.03+0.24 −0.49 |
19.7+6.4 −7.4 |
3.25+1.32 −0.58 |
0.93 | Smaller mass could be a neutron star | [52] | ||
151217 | 2015-12-17 03:47:49 | 2019-10-11 | 1000+660 −440 |
H,L | 0.15 | 0.70+0.15 −0.50 |
46+13 −26 |
8.2+5.1 −1.7 |
0.74 | [52] | |||
151222 | 2015-12-22 05:28:26 | 2018-11-05 | H,L | 0.075 | -0.74 | 6.86 | 3.26 | 0.988 | [51] | ||||
151231 | 2015-12-31 00:40:30 | 2019-02-27 | H,L | 0.85 | [53] | ||||||||
160103 | 2016-01-03 05:48:36 | 2018-11-05 | H,L | 0.396 | 0.49 | 9.75 | 7.29 | 0.939 | [51] | ||||
170104 | 2017-01-04 21:58:40 | 2019-10-11 | 4600+4300 −3100 |
H,L | 0.03 | 0.25+0.50 −0.49 |
98+49 −40 |
44+30 −33 |
0.88 | [52] | |||
170121 | 2017-01-21 21:25:36 | 2019-04-15 | H,L | −0.3±0.3 | 29+4 −3 |
<0.01 | [54] | ||||||
170123 | 2017-01-23 20:16:42 | 2019-10-11 | 2800+2800 −1600 |
H,L | 0.04 | −0.12+0.31 −0.35 |
44+23 −12 |
28±13 | 0.92 | [52] | |||
170201 | 2017-02-01 11:03:12 | 2019-10-11 | 1530+1360 −770 |
H,L | 0.16 | 0.44+0.28 −0.54 |
48+13 −23 |
13.1+8.6 −3.7 |
0.76 | [52] | |||
170202 | 2017-02-02 13:56:57 | 2019-10-11 | 1220+980 −640 |
H,L | 0.06 | −0.06+0.27 −0.32 |
33+17 −11 |
13.8+7.0 −4.8 |
0.87 | [52] | |||
170220 | 2017-02-20 11:36:24 | 2019-10-11 | 3600+3700 −2100 |
H,L | 0.05 | 0.28+0.33 −0.37 |
69+37 −25 |
31+22 −14 |
0.90 | [52] | |||
170304 | 2017-03-04 16:37:53 | 2019-10-11 | 2300+1600 −1200 |
H,L | 2.5 | 0.11+0.29 −0.27 |
44.9+17.6 −9.4 |
31.8+9.5 −11.6 |
0.30 | [52] | |||
170402 | 2017-04-02 21:51:50 | 2019-10-21 | H,L | 0.32 | [55] | ||||||||
170403 | 2017-04-03 23:06:11 | 2019-10-11 | 2500+2100 −1300 |
H,L | 0.07 | −0.20+0.35 −0.37 |
53+23 −13 |
35+13 −15 |
0.97 | [52] | |||
170425 | 2017-04-25 05:53:34 | 2019-10-11 | 2600+2000 −1300 |
H,L | 0.20 | −0.06+0.28 −0.32 |
45+21 −11 |
30±11 | 0.79 | [52] | |||
170620 | 2017-06-20 01:14:02 | 2019-10-11 | 1710+1300 −850 |
H,L | 0.04 | 0.05±0.25 | 29.4+13.2 −6.8 |
17.9+5.4 −5.5 |
0.98 | [52] | |||
170629 | 2017-06-29 04:13:55 | 2019-10-11 | 1880+1450 −940 |
H,L | 0.06 | 0.73+0.15 −0.98 |
49+20 −30 |
7.3+4.6 −2.6 |
0.98 | [52] | |||
170721 | 2017-07-21 05:55:13 | 2019-10-11 | 1160+750 −520 |
H,L | 0.04 | −0.06+0.25 −0.29 |
31.7+9.3 −6.1 |
21.4+5.3 −5.6 |
0.94 | [52] | |||
170727 | 2017-07-27 01:04:30 | 2019-10-11 | 2200+1500 −1100 |
H,L | 180 | −0.05+0.25 −0.30 |
41.6+12.8 −7.9 |
30.4+7.9 −8.2 |
0.006 | [52] | |||
170801 | 2017-08-01 23:28:19 | 2019-10-11 | 1070+920 −580 |
L,V | 0.04 | −0.09+0.25 −0.24 |
23.9+12.6 −6.6 |
12.4+4.7 −4.0 |
0.99 | [52] | |||
170817A | 2017-08-17 03:02:46 | 2019-10-21 | H,L,V | 11.5 | 0.5±0.2 | 56+16 −10 |
40+10 −11 |
0.14 | [55] | ||||
170818 | 2017-08-18 09:34:45 | 2019-10-11 | 3100+1700 −1900 |
H,V | 0.04 | 0.06+0.48 −0.45 |
55+59 −28 |
23+43 −15 |
0.99 | [52] |
Observation candidates from O3/2019[]
From observation run O3/2019 on, observations are published as to facilitate multi-messenger observations of events.[56][57][58] Candidate event records can be directly accessed at the Gravitational Wave Candidate Event Database.[59] On 1 April 2019, the start of the third observation run was announced with a circular published in the public alerts tracker.[60] 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.[61]
The Kamioka Gravitational Wave Detector (KAGRA) in Japan became operational on 25 February 2020,[62] likely improving the detection and localization of future gravitational wave signals.[63] 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.[8][64]
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<100 Mpc
100-200 Mpc
200-500 Mpc
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2000-5000 Mpc
5000+ Mpc
|
GW event | Detection time (UTC) |
Location area[n 15] (deg2) |
Luminosity distance (Mpc)[n 16] |
Detector [n 17] |
False Alarm Rate (Hz) |
Classification | Notes | Ref | ||||
---|---|---|---|---|---|---|---|---|---|---|---|---|
NS / NS [n 18] |
NS / BH [n 19] |
BH / BH [n 20] |
Mass gap [n 21] |
Terrestrial [n 22] | ||||||||
S190408an | 2019-04-08 18:18:02 |
H,L,V | 2.8 10−18 | 0.0 | 0.0 | ~1.0 | 0.0 | 9.8e−12 | [65][66] | |||
S190421ar | 2019-04-21 21:38:56 |
H,L | 1.5 10−8 | 0.0 | 0.0 | 0.967 | 0.0 | 0.033 | Initially marked with 96% chance of having a terrestrial origin ["noise"], but later upgraded to 97% chance of being a binary black hole merger. | [67] | ||
S190426c | 2019-04-26 15:21:55 |
H,L,V | 1.9 10−8 | 0.244 | 0.064 | 0.0 | 0.117 | 0.575 | Initially marked with 49% chance of being binary neutron star merger, 13% neutron star-black hole merger, 24% mass gap merger. Later marked with a 52% chance of NS-BH, 22% mass gap, 13% BNS, and 14% terrestrial, before being revised to the current solution |
[68][69] | ||
S190503bf | 2019-05-03 18:54:04 |
H,L,V | 1.6 10−9 | 0.0 | 0.0047 | 0.963 | 0.032 | 0.00012 | [71] | |||
S190510g | 2019-05-10 02:59:39 |
H,L,V | 8.8 10−9 | 0.42 | 0.0 | 0.0 | 0.0 | 0.58 | Initially reported with a 2% chance of terrestrial origin ["noise"], later downgraded to ~58% terrestrial foreground probability ["noise"]. | [72] | ||
S190512at | 2019-05-12 18:07:14 |
H,L,V | 1.9 10−9 | 0.0 | 0.0 | 0.990 | 0.0 | 0.010 | [73] | |||
S190513bm | 2019-05-13 20:54:28 |
H,L,V | 3.7 10−13 | 0.0 | 0.0052 | 0.943 | 0.052 | 6.0e−8 | [74] | |||
S190517h | 2019-05-17 05:51:01 |
H,L,V | 1.8 10−12 | 0.0 | 0.00077 | 0.983 | 0.017 | 0.000043 | [75] | |||
S190519bj | 2019-05-19 15:35:44 |
H,L,V | 5.7 10−9 | 0.0 | 0.0 | 0.956 | 0.0 | 0.044 | [76] | |||
S190521r | 2019-05-21 07:43:59 |
H,L | 3.2 10−10 | 0.0 | 0.0 | 0.9993 | 0.0 | 0.00067 | [77] | |||
S190602aq | 2019-06-02 17:59:27 |
H,L,V | 1.9 10−9 | 0.0 | 0.0 | 0.990 | 0.0 | 0.0097 | [78] | |||
S190630ag | 2019-06-30 18:52:05 |
L,V | 1.4 10−13 | 0.0 | 0.0052 | 0.943 | 0.052 | 1.8e−7 | [79] | |||
S190701ah | 2019-07-01 20:33:45 | H,L,V | 1.9 10−8 | 0.0 | 0.0 | 0.934 | 0.0 | 0.066 | [80] | |||
S190706ai | 2019-07-06 22:26:57 | H,L,V | 1.9 10−9 | 0.0 | 0.0 | 0.990 | 0.0 | 0.010 | [81] | |||
S190707q | 2019-07-07 09:33:44 | H,L | 5.3 10−12 | 0.0 | 0.0 | 0.999989 | 0.0 | 0.000011 | [82] | |||
S190718y | 2019-07-18 14:35:12 | H,L,V | 3.6 10−8 | 0.022 | 0.0 | 0.0 | 0.0 | 0.979 | Estimated to have a 98% chance to be terrestrial noise, despite passing data quality checks. | [83] | ||
S190720a | 2019-07-20 00:08:53 | H,L | 3.8 10−9 | 0.0 | 0.0 | 0.989 | 0.0 | 0.011 | Initially reported with a 71% chance of being terrestrial "noise" [non-cosmological in origin], upgraded to 1% after preliminary Virgo detector signal path inconsistency found to be insignificant. | [84] | ||
S190727h | 2019-07-27 06:03:51 | H,L,V | 1.4 10−10 | 0.0 | 0.0018 | 0.922 | 0.028 | 0.048 | [85] | |||
S190728q | 2019-07-28 06:45:27 | H,L,V | 2.5 10−23 | 0.0 | 0.144 | 0.340 | 0.516 | 3.6e-13 | Updated from an initial estimate which gave 14.4% NS/BH, 34.0% BH/BH, 51.6% mass gap, and a later estimate which gave a virtually certain BH/BH merger. | [86] | ||
S190828j | 2019-08-28 06:34:05 | H,L,V | 8.5 10−22 | 0.0 | 0.0 | ~1.0 | 0.0 | 3.8e-14 | [87] | |||
S190828l | 2019-08-28 06:55:09 | H,L,V | 4.6 10−11 | 0.0 | 0.0 | 0.9996 | 0.0 | 0.00041 | [88] | |||
S190901ap | 2019-09-01 23:31:01 |
L,V | 7.0 10−9 | 0.861 | 0.0 | 0.0 | 0.0 | 0.139 | [89] | |||
S190910d | 2019-09-10 01:26:19 |
H,L | 3.7 10−9 | 0.0 | 0.976 | 0.0 | 0.0 | 0.024 | [90] | |||
S190910h | 2019-09-10 08:29:58 |
L | 3.6 10−8 | 0.612 | 0.0 | 0.0 | 0.0 | 0.388 | Detected by only the Livingston detector, resulting in a bad sky localization. | [91] | ||
S190915ak | 2019-09-15 23:57:25 | H,L,V | 9.7 10−10 | 0.0 | 0.0 | 0.995 | 0.0 | 0.0053 | [92] | |||
S190923y | 2019-09-23 12:55:59 | H,L | 4.8 10−8 | 0.0 | 0.677 | 0.0 | 0.0 | 0.322 | [93] | |||
S190924h | 2019-09-24 02:18:46 | H,L,V | 8.9 10−19 | 0.0 | 0.0 | 0.0 | ~1.0 | 4.7e-11 | The other component of the merger has a 29.7% chance of being a neutron star, and a 70.3% chance of being either a black hole, or another object in the mass gap. | [94] | ||
S190930s | 2019-09-30 13:35:41 | H,L | 3.0 10−9 | 0.0 | 0.0 | 0.0 | 0.951 | 0.049 | The other component is either a black hole or another object in the mass gap. | [95] | ||
S190930t | 2019-09-30 14:34:07 | L | 1.5 10−8 | 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. | [96] | ||
S191105e | 2019-11-05 14:35:21 | H,L,V | 2.3 10−8 | 0.0 | 0.0 | 0.953 | 0.0 | 0.047 | First detection of the O3b run. | [97] | ||
S191109d | 2019-11-09 01:07:17 | H,L | 1.5 10−13 | 0.0 | 0.0 | 0.9999978 | 0.0 | 0.0000022 | [98] | |||
S191129u | 2019-11-29 13:40:29 | H,L | 2.7 10−35 | 0.0 | 0.0 | ~1.0 | 0.0 | 1.2e-27 | [99] | |||
S191204r | 2019-12-04 17:15:25 | H,L,V | 3.1 10−25 | 0.0 | 0.0 | ~1.0 | 0.0 | 8.7e-18 | [100] | |||
S191205ah | 2019-12-05 21:52:08 | H,L,V | 1.2 10−8 | 0.0 | 0.932 | 0.0 | 0.0 | 0.068 | [101] | |||
S191213g | 2019-12-13 04:34:08 | H,L,V | 3.5 10−8 | 0.768 | 0.0 | 0.0 | 0.0 | 0.232 | [102] | |||
S191215w | 2019-12-15 22:30:52 | H,L,V | 1.0 10−9 | 0.0 | 0.0 | 0.997 | 0.0 | 0.0028 | [103] | |||
S191216ap | 2019-12-16 21:33:38 | H,V | 1.1 10−23 | 0.0 | 0.0 | 0.9907 | 0.0093 | 8.4e-16 | Initially reported to have a ~100% chance of having a component in the mass gap. | [104] | ||
S191222n | 2019-12-22 03:35:37 | H,L | 6.5 10−12 | 0.0 | 0.0 | 0.999962 | 0.0 | 0.000038 | [105] | |||
S200112r | 2020-01-12 15:58:38 | L,V | 1.3 10−11 | 0.0 | 0.0 | 0.99966 | 0.0 | 0.00034 | [106] | |||
S200114f | 2020-01-14 02:08:18 | H,L,V | 1.2 10−9 | 0.0 | 0.0 | 0.0 | 0.0 | ? | Unidentified gravitational wave "burst" lasting 0.014 seconds at a frequency of tens of Hertz. | [107] | ||
S200128d | 2020-01-28 02:20:36 | H,L | 1.6 10−8 | 0.0 | 0.0 | 0.969 | 0.0 | 0.031 | [108] | |||
S200129m | 2020-01-29 06:54:58 | H,L,V | 6.7 10−32 | 0.0 | 0.0 | ~1.0 | 0.0 | 2.0e-24 | [109] | |||
S200208q | 2020-02-08 13:01:17 | H,L,V | 2.5 10−9 | 0.0 | 0.0 | 0.9936 | 0.0 | 0.0066 | [110] | |||
S200213t | 2020-02-13 04:10:40 | H,L,V | 1.8 10−8 | 0.629 | 0.0 | 0.0 | 0.0 | 0.371 | [111] | |||
S200219ac | 2020-02-19 09:44:15 | H,L,V | 1.3 10−8 | 0.0 | 0.0 | 0.964 | 0.0 | 0.036 | [112] | |||
S200224ca | 2020-02-24 22:22:34 | H,L,V | 1.6 10−11 | 0.0 | 0.0 | 0.999966 | 0.0 | 0.000034 | [113] | |||
S200225q | 2020-02-25 06:04:21 | H,L | 9.2 10−9 | 0.0 | 0.0 | 0.957 | 0.0 | 0.043 | [114] | |||
S200302c | 2020-03-02 01:58:11 | H,V | 9.3 10−9 | 0.0 | 0.0 | 0.890 | 0.0 | 0.110 | [115] | |||
S200311bg | 2020-03-11 11:58:53 | H,L,V | 8.9 10−26 | 0.0 | 0.0 | ~1.0 | 0.0 | 4.0e-17 | [116] | |||
S200316bj | 2020-03-16 21:57:56 | H,L,V | 7.1 10−11 | 0.0 | 0.0 | 0.0 | 0.9957 | 0.0043 | The other component is a black hole. | [117] |
See also[]
- GRB 150101B, a weak gamma-ray burst trigger observed prior to aLIGO O1 (beginning September 12, 2015), with claimed similarities to model-supported possible neutron star merger GW170817/GRB 170817A/AT2017gfo.
Notes[]
- ^ Indirect evidence for gravitational waves was obtained by 1978 from observations of orbital decay in the neutron star binary PSR B1913+16.[1]
- ^ 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 of the binary masses, according to , thus ranging from ~87% of when the masses are the same to ~78% when they differ by an order of magnitude.
- ^ The dimensionless effective inspiral spin parameter is: [11] where is the mass of a black hole, is its spin, and is the angle between the orbital angular momentum and a merging black hole's spin (ranging from when aligned to when antialigned). It is the mass-weighted linear combination of the components of the black holes' spins aligned with the orbital axis[11][10] 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).[12] 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.[13]
- ^ Values of the dimensionless spin parameter cJ/GM2 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.[14]
- ^ Spin estimate is 0.26+0.52
−0.24.[15] - ^ Spin estimate is 0.32+0.54
−0.29.[15] - ^ Based on a descending spin-down chirp observed in GW post-merger, a magnetar was produced that survived at least 5 seconds.[25]
- ^ 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.[26]
- ^ 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)
- ^ 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"])
References[]
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- ^ 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.
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|journal=
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- ^ "Superevent info - S191213g". LIGO. Retrieved 14 December 2019.
- ^ "Superevent info - S191215w". LIGO. Retrieved 23 December 2019.
- ^ "Superevent info - S191216ap". LIGO. Retrieved 25 December 2019.
- ^ "Superevent info - S191222n". LIGO. Retrieved 22 December 2019.
- ^ "Superevent info - S200112r". LIGO. Retrieved 12 January 2020.
- ^ "Superevent info - S200114f". LIGO. Retrieved 14 January 2020.
- ^ "Superevent info - S200128d". LIGO. Retrieved 28 January 2020.
- ^ "Superevent info - S200129m". LIGO. Retrieved 29 January 2020.
- ^ "Superevent info - S200208q". LIGO. Retrieved 8 February 2020.
- ^ "Superevent info - S200213t". LIGO. Retrieved 13 February 2020.
- ^ "Superevent info - S200219ac". LIGO. Retrieved 19 February 2020.
- ^ "Superevent info - S200224ca". LIGO. Retrieved 25 February 2020.
- ^ "Superevent info - S200225q". LIGO. Retrieved 26 February 2020.
- ^ "Superevent info - S200302c". LIGO. Retrieved 2 March 2020.
- ^ "Superevent info - S200311bg". LIGO. Retrieved 11 March 2020.
- ^ "Superevent info - S200316bj". LIGO. Retrieved 17 March 2020.
External links[]
- Gravitational waves
- Physics-related lists
- Astronomy-related lists
- Observational astronomy
- Binary systems