This is a list of fast radio bursts . Items are listed here if information about the fast radio burst has been published. Although there could be thousands of detectable events per day, only detected ones are listed.
Name | Date and time (UTC) for 1581.804688 MHz | RA (J2000) | Decl. (J2000) | DM (pc.cm−3) [note 1] | Width (ms) | Peak flux (Jy) | Maximum estimated comoving distance (Gly) [note 1] | Observed comoving distance (Gly) [note 1] | Notes |
---|---|---|---|---|---|---|---|---|---|
FRB 010312 | 2001-03-12 11:06:47.98 | 05h 27m | −64° 56′ | 1187±14 | 24.3±1.3 | 0.2±0.05 | 10.14±0.15 | — | |
FRB 010621 [1] | 2001-06-21 13:02:11.30 | 18h 52m | −08° 30′ | 748±3 | 8+4 −2.3 | 0.53+0.26 −0.09 | 2.41±0.03 | — | |
FRB 010724 [2] | 2001-07-24 19:50:01.69 | 01h 18m | −75° 12′ | 375±3 | 13+5 −11 | 30+10 −10 | 3.42±0.05 | — | "Lorimer Burst" |
FRB 011025 [3] | 2001-01-25 00:29:15.79 | 19h 07m | −40° 37′ | 790.3±3 | 9.4±0.2 | 0.54+0.11 −0.07 | 6.62±0.10 | — | Announced in 2014 as FRB 011025 (from data archived in 2001). |
FRB 090625 [4] | 2009-06-25 21:53:52.85 | 03h 07m | −29° 55′ | 899.55±0.01 | 1.9+0 −1.9 | 1.14+0.42 −0.21 | 8.22±0.12 | — | |
FRB 110214 | 2011-02-14 07:14:10.353 | 01h 21m | −49° 47′ | 168.9±0.5 | 1.9±0.9 | 27+1028 −0 | 1.79±0.02 | — | |
FRB 110220 [5] | 2011-02-20 01:55:48.096 | 22h 35m | −12° 24′ | 944.38±0.05 | 5.6±0.1 | 1.3 | 8.48±0.12 | — | |
FRB 110523 [6] [7] [8] | 2011-05-23 15:06:19.7 | 21h 45m | −00° 10′ | 623.30±0.06 | 1.73±0.17 | 0.6 | 5.77±0.09 | — | 700–900 MHz at Green Bank radio telescope, detection of both circular and linear polarization. |
FRB 110626 [5] | 2011-06-26 21:33:17.477 | 21h 04m | −44° 44′ | 723.0±0.3 | 1.41+1.22 −0.45 | 0.63+1.22 −0.12 | 6.62±0.10 | — | |
FRB 110703 [5] | 2011-07-03 18:59:40.607 | 23h 31m | −02° 52′ | 1103.6±0.7 | 3.9+2.24 −1.85 | 0.48+0.28 −0.10 | 9.72±0.14 | — | |
FRB 120127 [5] | 2012-01-27 08:11:21.725 | 23h 15m | −18° 26′ | 553.3±0.3 | 1.21+0.64 −0.25 | 0.62+0.35 −0.10 | 5.25±0.09 | — | |
FRB 121002.1 [9] [4] | 2012-10-02 13:09:18.402 | 18h 15m | −85° 12′ | 1629.18±0.02 | 5.44+3.5 −1.2 | 0.39 | 12.82±0.17 | — | double burst 5.1 ms apart |
FRB 121002.2 [4] | 2012-10-02 13:09:18.46 | 0.43+0.33 −0.06 | |||||||
FRB 121029 | 2012-10-29 16:06:26.0 | 00h 12m | +42° 04′ | 732±5 | 320±40 | 0.34 | 6.46±0.10 | — | |
FRB 121102 [10] | 2012-11-02 06:35:53.244 | 05h 31m 58.7s | +33° 08′ 52.6″ | 557±2 | 3.0±0.5 | 0.4+0.4 −0.1 | 3.85±0.06 | — | by Arecibo radio telescope |
FRB 130626 [4] | 2013-06-26 14:55:59.771 | 16h 27m | −07° 28′ | 952.4±0.1 | 1.98+1.2 −0.44 | 0.74+0.49 −0.11 | 8.22±0.12 | — | |
FRB 130628 [4] | 2013-06-28 03:58:00.178 | 09h 03m | +03° 26′ | 469.88±0.01 | 0.64±0.13 | 1.91+0.29 −0.23 | 4.30±0.08 | — | |
FRB 130729 [4] | 2013-07-29 09:01:51.19 | 13h 41m | −06° 00′ | 861±2 | 15.61+9.98 −6.27 | 0.22+0.17 −0.046 | 7.80±0.11 | — | |
FRB 131030 | 2013-10-30 16:13:15.00 | 00h 25m | +39° 59′ | 203±4 | 530±40 | 0.24 | 1.50±0.02 | — | |
FRB 131104 [11] | 2013-11-04 18:04:01.2 | 06h 44m | −51° 17′ | 779±1 | 2.37+0.89 −0.45 | 1.16+0.35 −0.126 | 6.88±0.10 | — | 'near' Carina Dwarf Spheroidal Galaxy |
FRB 140212 | 2014-02-12 10:31:14.00 | 01h 31m | +30° 32′ | 910±4 | 390±40 | 0.26 | 8.15±0.12 | — | |
FRB 140514 [12] | 2014-05-14 17:14:11.06 | 22h 34m | −12° 19′ | 562.7±0.6 | 2.8+3.5 −0.7 | 0.47+0.099 −0.136 | 5.32±0.08 | — | 21 ± 7 per cent (3σ) circular polarization |
FRB 141113 | 2014-11-13 07:42:55.22 | 06h 13m | +18° 47′ | 400.3 | 2 | 0.039 | 1.96±0.02 | — | |
FRB 141216 | 2014-12-16 13:03:24.00 | 00h 14m | +41° 38′ | 545±5 | 870±40 | 0.23 | 4.83±0.09 | — | |
FRB 150215 [13] | 2015-02-15 20:41:41.714 | 18h 17m | −04° 54′ | 1105.6±0.8 | 2.88+1.2 −0.57 | 0.7+0.28 −0.095 | 6.72±0.10 | — | 43% linear 3% circular polarized |
FRB 150418 | 2015-04-18 04:29:06.657 | 07h 17m | −19° 01′ | 776.2±0.5 | 0.8±0.3 | 2.2+0.6 −0.3 | 5.84±0.09 | — | Detection of linear polarization. The origin of the burst is disputed. [14] [15] [16] [17] |
FRB 150517.1 | 2015-05-17 17:42:08.712 | 05h 31m 58.7s | +33° 08′ 52.6″ | 560±4 | 3.8±0.4 | 0.03 | 3.85±0.06 | — | 10 repeat bursts at FRB 121102 location: 2 bursts on May 17 and 8 bursts on June 2 [18] [19] |
FRB 150517.2 | 2015-05-17 17:51:40.921 | 566±10 | 3.3±0.4 | 0.03 | |||||
FRB 150602.1 | 2015-06-02 16:38:07.575 | 555±3 | 4.6±0.3 | 0.04 | |||||
FRB 150602.2 | 2015-06-02 16:47:36.484 | 558±10 | 8.7±1.5 | 0.02 | |||||
FRB 150602.3 | 2015-06-02 17:49:18.627 | 559±10 | 2.8±0.4 | 0.02 | |||||
FRB 150602.4 | 2015-06-02 17:49:41.319 | — | 6.1±1.4 | 0.02 | |||||
FRB 150602.5 | 2015-06-02 17:50:39.298 | 556.5±3.7 | 6.6±0.1 | 0.14 | |||||
FRB 150602.6 | 2015-06-02 17:53:45.528 | 557.4±3.7 | 6.0±0.3 | 0.05 | |||||
FRB 150602.7 | 2015-06-02 17:56:34.787 | 558.7±4.9 | 8.0±0.5 | 0.05 | |||||
FRB 150602.8 | 2015-06-02 17:57:32.020 | 556.5±1.1 | 3.06±0.04 | 0.31 | |||||
FRB 150610 | 2015-06-10 05:26:59.396 | 10h 44m | −40° 05′ | 1593.9±0.6 | 2±1 | 0.7±0.2 | 12.17±0.16 | — | |
FRB 150807 | 2015-08-07 17:53:55.83 | 22h 43m | −55° 05′ | 266.5±0.1 | 0.35±0.05 | 128±5 | 2.45±0.03 | — | |
FRB 151018.1 | 2015-10-18 01:05:48.00 | 05h 31m 58.7s | +33° 08′ 52.6″ | 570±5 | 650+0 −650 | 1.4 | 3.85±0.06 | — | double burst 2.5 seconds apart at FRB121102 location |
FRB 151018.2 | 2015-10-18 01:05:50.50 | 400+0 −400 | |||||||
FRB 151113 | 2015-11-13 08:32:42.375 | 559.9±7.1 | 6.73±1.12 | 0.04 | 5 repeat bursts at FRB121102 location: 1 burst on November 13 and 4 bursts on November 19 | ||||
FRB 151119.1 | 2015-11-19 10:44:40.524 | 565.1±5.2 | 6.1±0.57 | 0.06 | |||||
FRB 151119.2 | 2015-11-19 10:51:34.957 | 568.8±6.6 | 6.14±1 | 0.04 | |||||
FRB 151119.3 | 2015-11-19 10:58:56.234 | — | 4.3±1.4 | 0.02 | |||||
FRB 151119.4 | 2015-11-19 11:05:52.492 | 560.0±6.4 | 5.97±0.35 | 0.09 | |||||
FRB 151125 | 2015-11-25 15:42:36.00 | 01h 32m | +30° 59′ | 273±4 | 1680±40 | 0.54 | 2.38±0.03 | — | |
FRB 151206 | 2015-12-06 06:17:52.78 | 19h 21m | −04° 08′ | 1909.8±0.6 | 3±0.6 | 0.3±0.04 | 14.29±0.20 | — | |
FRB 151208 | 2015-12-08 04:54:40.26 | 05h 31m 58.7s | +33° 08′ 52.6″ | 558.6±1.7 | 2.5±0.23 | 0.03 | 3.85±0.06 | — | at FRB121102 location |
FRB 151230 | 2015-12-30 16:15:46.525 | 09h 41m | −03° 27′ | 960.4±0.5 | 4.4±0.5 | 0.42±0.03 | 8.90±0.13 | — | |
FRB 160102 | 2016-01-02 08:28:39.374 | 22h 39m | −30° 11′ | 2596.1±0.3 | 3.4±0.8 | 0.5±0.1 | 17.81±0.27 | — | |
FRB 160206 | 2016-02-06 10:26:50.00 | 01h 01m | +41° 38′ | 1262±5 | 1590±40 | 0.26 | 10.67±0.15 | — | |
FRB 160317 [20] | 2016-03-17 09:00:36.53 | 07h 54m | −29° 37′ | 1165±11 | 21±7 | 3 | 8.09±0.11 | — | First FRB observed by the interferometer UTMOST |
FRB 160410 [20] | 2016-04-10 08:33:39.68 | 08h 41m | +06° 05′ | 278±3 | 4±1 | 7 | 2.35±0.03 | — | |
FRB 160608 [20] | 2016-06-08 03:53:01.088 | 07h 37m | −40° 48′ | 682±7 | 9±6 | 4.3 | 4.60±0.09 | — | |
FRB 160823 | 2016-08-23 17:51:23.921 | 05h 31m 58.7s | +33° 08′ 52.6″ | 567±2 | 2 | — | 3.85±0.06 | — | at FRB121102 location |
FRB 160920 | 2016-09-20 03:05:43.00 | 05h 34m | +41° 45′ | 1767±4 | 5000 | 0.22 | 12.23±0.16 | — | |
FRB 161202 | 2016-12-02 13:24:54.00 | 23h 44m | +40° 48′ | 291±4 | 810±40 | 0.29 | 2.38±0.03 | — | |
FRB 170107 [21] | 2017-01-07 20:05:08.139 | 11h 23m | −05° 00′ | 609.5±0.5 | 2.4±0.2 | 24.1 | 5.81±0.09 | — | first by ASKAP, high fluence ~58 Jy ms. In Leo. Galactic latitude 51°, Distance 3.1 Gpc, isotropic energy ~3 x 1034 J [21] |
FRB 170416 | 2017-04-16 23:11:12.799 | 22h 13m | −55° 02′ | 523.2±0.2 | 5±0.6 | 19.4 | 4.92±0.09 | — | |
FRB 170428 | 2017-04-28 18:02:34.700 | 21h 47m | −41° 51′ | 991.7±0.9 | 4.4±0.5 | 7.7 | 8.84±0.13 | — | |
FRB 170606 | 2017-06-06 10:03:27.00 | 05h 34m | +41° 45′ | 247±5 | 3300 | 0.54 | — | — | |
FRB 170707 | 2017-07-07 06:17:34.354 | 02h 59m | −57° 16′ | 235.2±0.6 | 3.5±0.5 | 14.8 | 2.15±0.02 | — | |
FRB 170712 | 2017-07-12 13:22:17.394 | 22h 36m | −60° 57′ | 312.79±0.07 | 1.4±0.3 | 37.8 | 2.94±0.04 | — | |
FRB 170826.1-15 | 2017-08-26 13:52:01.252 | 05h 31m 58.7s | +33° 08′ 52.6″ | 565±5 | 1.74 | 0.38 | 3.85±0.06 | — | 15 more bursts at the location of FRB 121102 detected by Green Bank Telescope over a 24-minute interval, bringing the total received bursts from this location to 34. [22] |
FRB 170827 [23] | 2017-08-27 16:20:18 | 00h 49m | −65° 33′ | 176.80±0.04 | 0.40±0.01 | 60±20 | 1.57±0.02 | — | low DM |
FRB 170906 | 2017-09-06 13:06:56.488 | 22h 00m | −19° 57′ | 390.3±0.4 | 2.5±0.3 | 29.6 | 3.69±0.05 | — | |
FRB 170922 [24] | 2017-09-22 11:23:33.4 | 21h 30m | −08° 00′ | 1111±1 | 34.1+2.6 −2.8 | 2.3±0.5 | 9.03±0.13 | — | extreme scattering (long pulse) |
FRB 171003 | 2017-10-03 04:07:23.781 | 12h 30m | −14° 07′ | 463.2±1.2 | 2.0±0.2 | 40.5 | 4.37±0.08 | — | |
FRB 171004 | 2017-10-04 03:23:39.250 | 11h 58m | −11° 54′ | 304.0±0.3 | 2.0±0.3 | 22 | 2.84±0.04 | — | |
FRB 171019 | 2017-10-19 13:26:40.097 | 22h 18m | −08° 35′ | 460.8±1.1 | 5.4±0.3 | 40.5 | 4.37±0.08 | — | repeating FRB |
FRB 171020 | 2017-10-20 10:27:58.598 | 22h 15m | −19° 40′ | 114.1±0.2 | 3.2±0.5 | 117.6 | 0.85±0.01 | — | |
FRB 171116 | 2017-11-16 14:59:33.305 | 03h 31m | −17° 14′ | 618.5±0.5 | 3.2±0.5 | 19.6 | 5.87±0.09 | — | |
FRB 171209 [25] | 2017-12-09 20:34:23.5 | 15h 50m | −46° 10′ | 1457.4±0.03 | 2.5 | 1.48 | 14.71±0.21 | — | |
FRB 171213 | 2017-12-13 14:22:40.467 | 03h 39m | −10° 56′ | 158.6±0.2 | 1.5±0.2 | 88.6 | 1.34±0.02 | — | |
FRB 171216 | 2017-12-16 17:59:10.822 | 03h 28m | −57° 04′ | 203.1±0.5 | 1.9±0.3 | 21 | 1.79±0.02 | — | |
FRB 180110 | 2018-01-10 07:34:34.959 | 21h 53m | −35° 27′ | 715.7±0.2 | 3.2±0.2 | 128.1 | 6.69±0.10 | — | |
FRB 180119 | 2018-01-19 12:24:40.747 | 03h 29m | −12° 44′ | 402.7±0.7 | 2.7±0.5 | 40.7 | 3.85±0.06 | — | |
FRB 180128.1 | 2018-01-28 00:59:38.617 | 13h 56m | −06° 43′ | 441.4±0.2 | 2.9±0.3 | 17.5 | 4.24±0.07 | — | |
FRB 180128.2 | 2018-01-28 04:53:26.796 | 22h 22m | −60° 15′ | 495.9±0.7 | 2.3±0.2 | 28.7 | 4.73±0.09 | — | |
FRB 180130 | 2018-01-30 04:55:29.993 | 21h 52m | −38° 34′ | 343.5±0.4 | 4.1±1 | 23.1 | 3.23±0.05 | — | |
FRB 180131 | 2018-01-31 05:45:04.320 | 21h 50m | −40° 41′ | 657.7±0.5 | 4.5±0.4 | 22.2 | 6.16±0.09 | — | |
FRB 180212 | 2018-02-12 23:45:04.399 | 14h 21m | −03° 35′ | 167.5±0.5 | 1.81±0.06 | 53 | 1.47±0.02 | — | |
FRB 180301 [26] | 2018-03-01 07:34:19.76 | 06h 13m | +04° 34′ | 520 | 3 | 0.5 | — | — | positive spectrum, from Breakthrough Listen |
FRB 180309 [27] | 2018-03-09 02:49:32.99 | 21h 25m | −33° 59′ | 263.42±0.01 | 0.475 | 27.6 | 2.41±0.03 | — | |
FRB 180311 [28] | 2018-03-11 04:11:54.80 | 21h 32m | −57° 44′ | 1570.9±0.5 | 13.4 | 0.15 | 16.86±0.25 | — | |
FRB 180315 | 2018-03-15 05:05:30.985 | 19h 35m | −26° 50′ | 479±0.4 | 2.4±0.3 | 23.3 | 4.57±0.09 | — | |
FRB 180321 | 2018-03-21 07:05:54.00 | 00h 33m | +42° 02′ | 594±5 | 1670±40 | 0.54 | 5.35±0.09 | — | |
FRB 180324 | 2018-03-24 09:31:46.706 | 06h 16m | −34° 47′ | 431±0.4 | 4.3±0.5 | 16.5 | 3.78±0.06 | — | |
FRB 180417 | 2018-04-17 13:18:31.00 | 12h 25m | +14° 13′ | 474.8 | 2.52 | 21.8 | 4.63±0.09 | — | |
FRB 180430 | 2018-04-30 10:00:35.70 | 06h 51m | −09° 57′ | 264.1±0.5 | 1.2 | 147.5±3.3 | 1.08±0.01 | — | |
FRB 180515 | 2018-05-15 21:57:26.485 | 23h 13m | −42° 15′ | 355.2±0.5 | 1.9±0.4 | 24.2 | 2.58±0.04 | — | |
FRB 180525 | 2018-05-25 15:19:06.515 | 14h 40m | −02° 12′ | 388.1±0.3 | 3.8±0.1 | 78.9 | 3.72±0.05 | — | |
FRB 180528 | 2018-05-28 04:24:00.9 | 06h 39m | −49° 54′ | 899.3±0.6 | 2.0±0.2 | 15.75 | 9.75±0.14 | — | |
FRB 180714 | 2018-07-14 10:00:08.7 | 17h 46m | −11° 46′ | 1467.92±0.3 | 2.9 | 0.6 | 14.87±0.21 | — | |
FRB 180725 [29] | 2018-07-25 17:59:32.813 | 06h 13m | +67° 04′ | 715.98±0.02 | 0.31+0.08 −0.07 | 39 | 6.43±0.10 | — | first detection of an FRB at radio frequencies below 700 MHz realtime detection by CHIME |
FRB 180727 | 2018-07-27 00:52:04.474 | 13h 11m | +26° 26′ | 642.07±0.03 | 0.78±0.16 | 18 | 6.20±0.10 | — | |
FRB 180729.1 | 2018-07-29 00:48:19.238 | 13h 16m | +55° 32′ | 109.61±0.002 | 0.12±0.01 | 283 | 0.85±0.01 | — | |
FRB 180729.2 | 2018-07-29 17:28:18.258 | 05h 58m | +56° 30′ | 317.37±0.01 | 0.08 | 113 | 2.38±0.03 | — | |
FRB 180730 | 2018-07-30 03:37:25.937 | 03h 53m | +87° 12′ | 849.047±0.002 | 0.42±0.04 | 119 | 7.66±0.11 | — | |
FRB 180801 | 2018-08-01 08:47:14.793 | 21h 30m | +72° 43′ | 656.2±0.03 | 0.51±0.09 | 55 | 5.71±0.09 | — | |
FRB 180806 | 2018-08-06 14:13:03.107 | 15h 15m | +75° 38′ | 739.98±0.03 | 0.69 | 35 | 6.91±0.11 | — | |
FRB 180810.1 | 2018-08-10 17:28:54.614 | 06h 46m | +34° 52′ | 414.95±0.02 | 0.27 | 41 | 3.29±0.05 | — | |
FRB 180810.2 | 2018-08-10 22:40:42.493 | 11h 59m | +83° 07′ | 169.134±0.002 | 0.28±0.03 | 61 | 1.34±0.02 | — | |
FRB 180812 | 2018-08-12 11:45:32.872 | 01h 12m | +80° 47′ | 802.57±0.04 | 1.25+0.49 −0.47 | 14 | 7.08±0.11 | — | |
FRB 180814.1 | 2018-08-14 14:20:14.440 | 15h 54m | +74° 01′ | 238.32±0.01 | 0.18 | 139 | 2.12±0.02 | — | |
FRB 180814.2 [30] | 2018-08-14 14:49:48.022 | 04h 22m 22s | +73° 40′ | 189.38±0.09 | 2.6±0.2 | 8.1 | 1.11±0.01 | — | Detected by CHIME. Second repeating FRB to be discovered and first since 2012. |
FRB 180817 | 2018-08-17 01:49:20.202 | 15h 33m | +42° 12′ | 1006.84±0.002 | 0.37 | 70 | 9.20±0.14 | — | |
FRB 180906 | 2018-09-06 01:17:47.380 | 04h 22m 22s | +73° 40′ | 191±3 | 3.9 | 5.4 | 1.11±0.01 | — | at FRB 180814.2 location |
FRB 180911 | 2018-09-11 12:59:13.733 | 189.8±0.9 | 7.9 | 0.43 | |||||
FRB 180916 | 2018-09-16 10:15:19.803 | 01h 58m 00.75s | +65° 43′ 00.5″ | 349.2±0.4 | 1.4±0.07 | 1.4±0.6 | 1.63±0.02 | 0.45±0.02 | repeating FRB localized to a nearby spiral galaxy |
FRB 180917 | 2018-09-17 00:46:35.359 | 04h 22m 22s | +73° 40′ | 189.5±0.1 | 63 | 1.0 | 1.11±0.01 | — | at FRB 180814.2 location |
FRB 180919 | 2018-09-19 12:36:09.141 | 190±0.1 | 16 | 0.75 | |||||
FRB 180924 [31] | 2018-09-24 16:23:12.6265 | 21h 44m 25.26s | −40° 54′ 00.1″ | 361.42±0.06 | 1.3±0.09 | 16 | 4.26±0.07 | 3.99±0.06 | first non-repeating FRB whose source has been localized |
FRB 181016 | 2018-10-16 04:16:56.30 | 15h 46m | −25° 25′ | 1982.8±2.8 | 8.6+0.7 −0.8 | 10.19 | 17.78±0.27 | — | |
FRB 181017.1 | 2018-10-17 10:24:37.40 | 22h 06m | −08° 51′ | 239.97±0.03 | 0.33 | 90 | 2.54±0.04 | — | |
FRB 181017.2 | 2018-10-17 23:26:11.86 | 17h 05m | +68° 17′ | 1281.9±0.4 | 13.4±0.1 | 0.4±0.3 | 10.89±0.15 | — | repeating FRB |
FRB 181019 | 2018-10-19 08:13:22.75 | 01h 58m 00.75s | +65° 43′ 00.5″ | 349.0±0.6 | 4.1±0.3 | 0.6±0.3 | 1.63±0.02 | 0.45±0.02 | burst at FRB 180916 location |
FRB 181028 | 2018-10-28 10:12:31.477 | 04h 22m 22s | +73° 40′ | 188.9±0.5 | 42 | 0.29 | 1.11±0.01 | — | at FRB 180814.2 location |
FRB 181030.1 | 2018-10-30 04:13:13.025 | 10h 54m | +73° 44′ | 103.5±0.7 | 0.59±0.08 | 3.2±1.7 | 0.68±0.01 | 0.088±0.003 | repeating FRB, most likely originating from NGC 3403. |
FRB 181030.2 | 2018-10-30 04:16:21.654 | 103.5±0.3 | 1.43±0.08 | 3.1±1.4 | |||||
FRB 181104.1 | 2018-11-04 06:57:18.585 | 01h 58m 00.75s | +65° 43′ 00.5″ | 349.5±0.3 | 1.37±0.07 | 1.4±0.5 | 1.63±0.02 | 0.45±0.02 | burst at FRB 180916 location |
FRB 181104.2 | 2018-11-04 07:07:01.591 | 349.6±0.2 | 6.3±1.1 | 0.4±0.2 | |||||
FRB 181112 | 2018-11-12 17:31:15.483 | 21h 49m | −52° 58′ | 589.27±0.03 | 2.1±0.2 | 12 | 4.96±0.09 | 5.81±0.10 | localized to a small galaxy |
FRB 181119 | 2018-11-19 16:49:03.191 | 12h 42m | +65° 08′ | 364.2±1 | 6.3±0.6 | 0.3±0.2 | 3.49±0.05 | — | repeating FRB |
FRB 181120 | 2018-11-20 05:56:06.232 | 01h 58m 00.75s | +65° 43′ 00.5″ | 349.9±0.6 | 1.1±0.09 | 1.1±0.5 | 1.63±0.02 | 0.45±0.02 | burst at FRB 180916 location |
FRB 181128 | 2018-11-28 08:27:41.740 | 04h 56m | +63° 23′ | 450.2±0.3 | 2.43±0.16 | 0.5±0.3 | 3.56±0.05 | — | repeating FRB |
FRB 181219 | 2018-12-19 07:04:41.678 | 450.8±0.3 | 5.5±0.7 | 0.3±0.2 | |||||
FRB 181222 | 2018-12-22 03:59:23.208 | 01h 58m 00.75s | +65° 43′ 00.5″ | 349.1±0.1 | 4.95±0.01 | 4.9±1.8 | 1.63±0.02 | 0.45±0.02 | burst at FRB 180916 location |
FRB 181223 | 2018-12-23 03:51:28.960 | 349.7±0.7 | 1.06±0.05 | 1.7±0.6 | |||||
FRB 181225 | 2018-12-25 03:53:03.926 | 348.9±0.7 | 1.3±0.3 | 0.4±0.2 | |||||
FRB 181226 | 2018-12-26 03:43:30.107 | 348.8±0.2 | 0.87±0.03 | 1.6±0.6 | |||||
FRB 181228 | 2018-12-28 13:48:50.10 | 06h 09m | −45° 58′ | 354.2±0.9 | 1.24+0.13 −0.15 | 19.23 | 3.78±0.06 | — | |
FRB 190103 | 2019-01-03 13:47:23.322 | 12h 42m | +65° 08′ | 364.0±0.3 | 2.66±0.1 | 0.6±0.3 | 3.49±0.05 | — | burst at FRB 181119 location |
FRB 190116.1 | 2019-01-16 13:07:33.833 | 12h 49m | +27° 09′ | 444.0±0.6 | 4.0±0.5 | 0.3±0.2 | 4.37±0.08 | — | repeating FRB |
FRB 190116.2 | 2019-01-16 13:08:20.412 | 443.6±0.8 | 1.5±0.3 | 0.4±0.2 | |||||
FRB 190126 | 2019-01-26 01:32:45.328 | 01h 58m 00.75s | +65° 43′ 00.5″ | 349.8±0.5 | 2.53±0.13 | 0.7±0.3 | 1.63±0.02 | — | |
FRB 190209 | 2019-02-09 08:20:20.977 | 09h 37m | +77° 40′ | 424.6±0.6 | 3.7±0.5 | 0.4±0.2 | 3.95±0.07 | — | repeating FRB |
FRB 190210 | 2019-02-10 08:17:13.907 | 425.2±0.5 | 9.4±1.4 | 0.6±0.4 | |||||
FRB 190216 | 2019-02-16 15:26:58.029 | 17h 05m | +68° 17′ | 1281.0±0.6 | 20.2±1.7 | 0.4±0.2 | 10.89±0.15 | — | burst at FRB 181017.2 location |
FRB 190222 | 2019-02-22 18:46:01.367 | 20h 52m | +69° 50′ | 460.6±0.1 | 2.97±0.90 | 1.9±0.6 | 3.91±0.07 | — | repeating FRB |
FRB 190301 | 2019-03-01 18:03:02.479 | 459.8±0.4 | 2.44±0.8 | 1.4±0.5 | |||||
FRB 190313 | 2019-03-13 09:21:46.725 | 12h 42m | +65° 08′ | 364.2±0.6 | 1.5±0.2 | 0.4±0.2 | 3.49±0.05 | — | burst at FRB 181119 location |
FRB 190523 | 2019-05-23 06:05:55.815 | 13h 48m 15.6s | +72° 28′ 11″ | 760.8±0.6 | 0.42±0.05 | 670 | 7.08±0.11 | 7.51±0.06 | localized to only 5 arcseconds |
FRB 190711 | 2019-07-11 01:53:41.093 | 21h 56m | −80° 23′ | 593±2 | — | — | — | — | |
FRB 190714 | 2019-07-14 05:17:12.901 | 12h 16m | −13° 00′ | 504±2 | — | — | — | — | |
FRB 190805 | 2019-08-05 09:21:08 | 22h 18m | −08° 35′ | 460.4±0.2 | 6±2 | — | — | — | burst at FRB 171019 location |
FRB 190806 | 2019-08-06 17:07:58.0 | 00h 02m | −07° 35′ | 388.5 | — | — | — | — | |
FRB 190906 | 2019-09-06 00:08:46 | 05h 31m 58.7s | 33° 08′ 52.6″ | — | — | — | — | — | burst at FRB 121102 location |
FRB 190910.1-12 | 2019-09-12 | 12 bursts detected at FRB 121102 location in a 3-hour timespan | |||||||
FRB 191001 | 2019-10-01 16:55:35.971 | 21h 32m | −54° 40′ | 506.92±0.04 | — | — | 4.37±0.08 | — | |
FRB 191107 | 2019-11-07 18:55:36.7 | 08h 02m | −13° 44′ | 714.25 | — | — | — | — | |
FRB 191223 | 2019-12-23 04:55:31.2 | 20h 34m | −75° 09′ | 665 | — | — | — | — | |
FRB 191228 | 2019-12-28 09:16:16.444 | 22h 57m | −29° 46′ | 297.9±0.5 | — | — | — | — | |
FRB 200120 [32] | 2020-01-20 | — | — | — | — | — | — | — | |
FRB 200428 | 2020-04-28 | 19h 35m | +21° 54′ | 332.8 | — | — | — | — | |
FRB 201124 | 2020-11-24 08:50:41 | 05h 08m | +26° 11′ | 413.52±0.05 | — | — | — | — | very high repeating burst activity reported to have begun 23 March 2021; includes "extremely bright" 15 April 2021 [33] [34] [35] [36] [37] [38] [39] [40] [41] |
FRB 210401 | 2021-04-01 11:33:01.66(1) | 05h 07m | +25° 53′ | 412±3 | — | — | — | — | |
FRB 210402 | 2021-04-02 05:48:59.114(1) | 05h 08m | +26° 02′ | 414±3 | — | — | — | — |
A magnetar is a type of neutron star with an extremely powerful magnetic field (~109 to 1011 T, ~1013 to 1015 G). The magnetic-field decay powers the emission of high-energy electromagnetic radiation, particularly X-rays and gamma rays.
Stellar radio sources, radio source stars or radio stars are stellar objects that produce copious emissions of various radio frequencies, whether constant or pulsed. Radio emissions from stars can be produced in many varied ways.
Centaurus A is a galaxy in the constellation of Centaurus. It was discovered in 1826 by Scottish astronomer James Dunlop from his home in Parramatta, in New South Wales, Australia. There is considerable debate in the literature regarding the galaxy's fundamental properties such as its Hubble type and distance. NGC 5128 is one of the closest radio galaxies to Earth, so its active galactic nucleus has been extensively studied by professional astronomers. The galaxy is also the fifth-brightest in the sky, making it an ideal amateur astronomy target. It is only visible from the southern hemisphere and low northern latitudes.
NGC 300 (also known as Caldwell 70 or the Sculptor Pinwheel Galaxy) is a spiral galaxy in the constellation Sculptor. It is one of the closest galaxies to the Local Group, and probably lies between the latter and the Sculptor Group. It is the brightest of the five main spirals in the direction of the Sculptor Group. It is inclined at an angle of 42° when viewed from Earth and shares many characteristics of the Triangulum Galaxy. It is 94,000 light-years in diameter, somewhat smaller than the Milky Way, and has an estimated mass of (2.9 ± 0.2) × 1010M☉.
Messier 81 (also known as NGC 3031 or Bode's Galaxy) is a grand design spiral galaxy about 12 million light-years away in the constellation Ursa Major. It has a D25 isophotal diameter of 29.44 kiloparsecs (96,000 light-years). Because of its relative proximity to the Milky Way galaxy, large size, and active galactic nucleus (which harbors a 70 million M☉ supermassive black hole), Messier 81 has been studied extensively by professional astronomers. The galaxy's large size and relatively high brightness also makes it a popular target for amateur astronomers. In late February 2022, astronomers reported that M81 may be the source of FRB 20200120E, a repeating fast radio burst.
An astronomical radio source is an object in outer space that emits strong radio waves. Radio emission comes from a wide variety of sources. Such objects are among the most extreme and energetic physical processes in the universe.
YZ Ceti is a red dwarf star in the constellation Cetus. Although it is relatively close to the Sun at just 12 light years, this star cannot be seen with the naked eye. It is classified as a flare star that undergoes intermittent fluctuations in luminosity. YZ Ceti is about 13 percent the mass of the Sun and 17% of its radius.
The National Astronomical Observatories, Chinese Academy of Sciences(NAOC, Chinese: 中国科学院国家天文台; pinyin: Zhōngguó Kēxuéyuàn Guójiā Tiānwéntái) is an astronomical research institute operated by Chinese Academy of Sciences, along with Shanghai Astronomical Observatory, Purple Mountain Observatory and National Time Service Center.
In radio astronomy, a fast radio burst (FRB) is a transient radio pulse of length ranging from a fraction of a millisecond, for an ultra-fast radio burst, to 3 seconds, caused by some high-energy astrophysical process not yet understood. Astronomers estimate the average FRB releases as much energy in a millisecond as the Sun puts out in three days. While extremely energetic at their source, the strength of the signal reaching Earth has been described as 1,000 times less than from a mobile phone on the Moon.
Matthew Bailes is an astrophysicist and Professor at the Centre for Astrophysics and Supercomputing, Swinburne University of Technology and the Director of OzGrav, the ARC Centre of Excellence for Gravitational Wave Discovery. In 2015 he won an ARC Laureate Fellowship to work on Fast Radio Bursts. He is one of the most active researchers in pulsars and Fast Radio Bursts in the world. His research interests includes the birth, evolution of binary and millisecond pulsars, gravitational waves detection using an array of millisecond pulsars and radio astronomy data processing system design for Fast Radio Burst discovery. He is now leading his team to re-engineer the Molonglo Observatory Synthesis Telescope with a newly designed correlation system for observation of pulsars and Fast Radio Bursts (FRBs).
A tidal disruption event (TDE) is a transient astronomical source produced when a star passes so close to a supermassive black hole (SMBH) that it is pulled apart by the black hole's tidal force. The star undergoes spaghettification, producing a tidal stream of material that loops around the black hole. Some portion of the stellar material is captured into orbit, forming an accretion disk around the black hole, which emits electromagnetic radiation. In a small fraction of TDEs, a relativistic jet is also produced. As the material in the disk is gradually consumed by the black hole, the TDE fades over several months or years.
In radio astronomy, perytons are short man-made radio signals of a few milliseconds resembling fast radio bursts (FRB). A peryton differs from radio frequency interference by the fact that it is a pulse of several to tens of millisecond duration which sweeps down in frequency. They are further verified by the fact that they occur at the same time in many beams, indicating that they come from Earth, whereas FRB's occur in only 1 or 2 of the beams, indicating that they are of galactic origin. The first signal occurred in 2001 but was not discovered until 2007. First detected at the Parkes Observatory, data gathered by the telescope also suggested the source was local. The signals were found to be caused by premature opening of a microwave oven door nearby.
The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is an interferometric radio telescope at the Dominion Radio Astrophysical Observatory in British Columbia, Canada which consists of four antennas consisting of 100 x 20 metre cylindrical parabolic reflectors with 1024 dual-polarization radio receivers suspended on a support above them. The antenna receives radio waves from hydrogen in space at frequencies in the 400–800 MHz range. The telescope's low-noise amplifiers are built with components adapted from the cellphone industry and its data are processed using a custom-built FPGA electronic system and 1000-processor high-performance GPGPU cluster. The telescope has no moving parts and observes half of the sky each day as the Earth turns.
GW 170817 was a gravitational wave (GW) signal observed by the LIGO and Virgo detectors on 17 August 2017, originating from the shell elliptical galaxy NGC 4993. The signal was produced by the last moments of the inspiral process of a binary pair of neutron stars, ending with their merger. It was the first GW observation to be confirmed by non-gravitational means. Unlike the five previous GW detections—which were of merging black holes and thus not expected to produce a detectable electromagnetic signal—the aftermath of this merger was seen across the electromagnetic spectrum by 70 observatories on 7 continents and in space, marking a significant breakthrough for multi-messenger astronomy. The discovery and subsequent observations of GW 170817 were given the Breakthrough of the Year award for 2017 by the journal Science.
SN 2018cow was a very powerful astronomical explosion, 10–100 times brighter than a normal supernova, spatially coincident with galaxy CGCG 137-068, approximately 200 million ly (60 million pc) distant in the Hercules constellation. It was discovered on 16 June 2018 by the ATLAS-HKO telescope, and had generated significant interest among astronomers throughout the world. Later, on 10 July 2018, and after AT 2018cow had significantly faded, astronomers, based on follow-up studies with the Nordic Optical Telescope (NOT), formally described AT 2018cow as SN 2018cow, a type Ib supernova, showing an "unprecedented spectrum for a supernova of this class"; although others, mostly at first but also more recently, have referred to it as a type Ic-BL supernova. An explanation to help better understand the unique features of AT 2018cow has been presented. AT2018cow is one of the few reported Fast Blue Optical Transients (FBOTs) observed in the Universe. In May 2020, however, a much more powerful FBOT than AT 2018cow was reportedly observed.
Ingrid Stairs is a Canadian astronomer currently based at the University of British Columbia. She studies pulsars and their companions as a way to study binary pulsar evolution, pulsar instrumentation and polarimetry, and Fast Radio Bursts (FRBs). She was awarded the 2017 Rutherford Memorial Medal for physics of the Royal Society of Canada, and was elected as a Fellow of the American Physical Society in 2018.
FRB 20180916B, is a repeating fast radio burst (FRB) discovered in 2018 by astronomers at the Canadian Hydrogen Intensity Mapping Experiment (CHIME) Telescope. According to a study published in the 9 January 2020 issue of the journal Nature, CHIME astronomers, in cooperation with the radio telescopes at European VLBI Network (VLBI) and the optical telescope Gemini North on Mauna Kea, Hawaii, were able to pinpoint the source of FRB 180916 to a location within a Milky Way-like galaxy named SDSS J015800.28+654253.0. This places the source at redshift 0.0337, approximately 457 million light-years from the Solar System.
SGR 1935+2154 is a soft gamma repeater (SGR) that is an ancient stellar remnant, in the constellation Vulpecula, originally discovered in 2014 by the Neil Gehrels Swift Observatory. Currently, the SGR-phenomena and the related anomalous X-ray pulsars (AXP) are explained as arising from magnetars. On 28 April 2020, this remnant about 30,000 light-years away in our Milky Way galaxy was observed to be associated with a very powerful radio pulse known as a fast radio burst or FRB, and a related x-ray flare. The detection is notable as the first FRB detected inside the Milky Way, and the first to be linked to a known source. Later in 2020, SGR 1935+2154 was found to be associated with repeating fast radio bursts.
In astronomy, a fast blue optical transient (FBOT), or more specifically, luminous fast blue optical transient (LFBOT), is an explosive transient event similar to supernovae and gamma-ray bursts with high optical luminosity, rapid evolution, and predominantly blue emission. The origins of such explosions are currently unclear, with events occurring at not more than 0.1% of the typical core-collapse supernova rate. This class of transients initially emerged from large sky surveys at cosmological distances, yet in recent years a small number have been discovered in the local Universe, most notably AT 2018cow.
Duncan Ross Lorimer is a British-born American astrophysicist. He is a professor of physics and astronomy at West Virginia University, known for the discovery of the first fast radio burst in 2007.