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 | — | — | — | — |
NGC 300 (also known as Caldwell 70) 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☉.
V1494 Aquilae or Nova Aquilae 1999 b was a nova which occurred during 1999 in the constellation Aquila and reached a brightness of magnitude 3.9 on 2 December 1999. making it easily visible to the naked eye. The nova was discovered with 14×100 binoculars by Alfredo Pereira of Cabo da Roca, Portugal at 18:50 UT on 1 December 1999, when it had a visual magnitude of 6.0.
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.
NGC 4725 is an intermediate barred spiral galaxy with a prominent ring structure, located in the northern constellation of Coma Berenices near the north galactic pole. It was discovered by German-born astronomer William Herschel on April 6, 1785. The galaxy lies at a distance of approximately 40 megalight-years from the Milky Way.
KT Eridani was a bright nova in the constellation Eridanus that produced an outburst in 2009. It was the first classical nova ever detected in that constellation. The nova was discovered at 12:52 UT on 25 November 2009 by K. Itagaki at Yamagata, Japan with a 21 cm patrol telescope. At the time of its discovery, it was a magnitude 8.1 object. The discovery occurred after the nova's peak brightness, but the All Sky Automated Survey system had detected the nova on three earlier occasions, allowing a more complete light curve to be produced. The peak magnitude, 5.4, was seen at 15:10 UT on 14 November 2009.
In radio astronomy, a fast radio burst (FRB) is a transient radio pulse of length ranging from a fraction of a millisecond 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. The first FRB was discovered by Duncan Lorimer and his student David Narkevic in 2007 when they were looking through archival pulsar survey data, and it is therefore commonly referred to as the Lorimer Burst. Many FRBs have since been recorded, including several that have been detected to repeat in seemingly irregular ways. Only one FRB has been detected to repeat in a regular way: FRB 180916 seems to pulse every 16.35 days.
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 in their 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.
V5856 Sagittarii, also known as Nova Sagittarii 2016 Number 4, was the 4th and brightest nova that occurred in the constellation Sagittarius during 2016. It was discovered by the All Sky Automated Survey for SuperNovae on 25.02 October 2016, at which time it had an apparent visual magnitude of 13.7. It was independently discovered by Yukio Sakurai of Mito, Ibaraki, Japan on 26.38 October 2016, by which time it had reached magnitude 10.4. It reached its peak brightness of magnitude 5.4, making it visible to the naked eye, on 8 November 2016. The nova occurred within a region of the sky monitored by the OGLE microlensing experiment, and that group reported that no star brighter than magnitude 22 was seen at the nova's position prior to its eruption.
V407 Lupi, also known as Nova Lupi 2016, was a bright nova in the constellation Lupus discovered by All Sky Automated Survey for SuperNovae (ASAS-SN) on 24.00 September 2016. At the time of its discovery, it had an apparent visual magnitude of 9.1. The ASAS-SN team reported that no object at the nova's location brighter than magnitude 17.5 was seen on images taken four days earlier. Wildly incorrect coordinates were published in the announcement telegram, but corrected in a subsequent telegram. It reached a peak brightness of magnitude 5.6, faintly visible to the naked eye, on 25 September 2016.
SN 2009ip was a supernova discovered in 2009 in the spiral galaxy NGC 7259 in the constellation of Piscis Austrinus. Since the brightness waned after days post-discovery, it was redesignated as Luminous blue variable (LBV) Supernova impostor.
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 AT2018cow was reportedly observed.
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) is an explosion event similar to supernovas and Gamma-ray bursts which presents high optical luminosity between those but rises and decays faster and has its spectra concentrated on the blue range. It is caused by some very high-energy astrophysical process not yet understood but thought to be a type of supernova with events occurring at not more than 0.1% of the typical rate.
YZ Reticuli, also known as Nova Reticuli 2020 was a naked eye nova in the constellation Reticulum discovered on July 15, 2020. Previously it was known as a VY Sculptoris type object with the designation MGAB-V207.
SN 2020oi was a supernova event in the grand design spiral galaxy known as Messier 100, or NGC 4321. It was discovered January 7, 2020 at an apparent magnitude of 17.28 by F. Forster and associates using the Zwicky Transient Facility. The position places it ~4.67″ north of the galactic nucleus. The supernova was not detected on an observation made three days before the discovery, and thus it must have begun during that brief period. The light curve peaked around January 13–18, depending on the wavelength, then declined rapidly over a period of 25 days before flattening into a more gradual decline. Observations of the spectrum made with the SOAR telescope showed this to be a type Ic supernova, with the progenitor being a massive star that had its outer envelope stripped. The initial velocity of the expanding photosphere was ~15,000 km/s.
AP Librae is a BL Lacertae object located at a distance of 700 million light years in the southern constellation of Libra. In the visual band it is one of the most active blazars known. AP Lib is surrounded by an extended source with a spectrum characteristic of a red-shifted giant elliptical galaxy. The derived visual magnitude of this region is 15.0, and it follows a radially decreasing brightness that is characteristic of an elliptical. Seven fainter galaxies are visible within an angular radius of 9′, suggesting it is the brightest member of a galactic cluster.
V4332 Sagittarii is a nova-like event in the constellation of Sagittarius. It was discovered February 24, 1994 at an apparent visual magnitude of 8.9 by Japanese amateur astronomer Minoru Yamamoto from Okazaki, Aichi, then confirmed by K. Hirosawa. Initially designated Nova Sagittarii 1994 #1, it was given the variable star designation V4332 Sgr. A spectra of the event taken March 4 lacked the characteristic features of a classical nova, with the only emission lines being of the Balmer series. Subsequent spectra showed a rapid decline in luminosity and a change of spectral type over a period of five days. By 2003, the object was ~1500 times less luminous than at peak magnitude and showed a spectrum of an M-type star.
Nova Cassiopeiae 2021, also known V1405 Cassiopeiae, was a nova in the constellation Cassiopeia. It reached a peak brightness of magnitude 5.449 on May 9, 2021, making it visible to the naked eye. It was discovered by Japanese amateur astronomer Yuji Nakamura of Kameyama, Japan, at 10:10 UT on March 18, 2021. The nova was first seen by Nakamura in four 15 second CCD exposures with a 135mm F/4 lens, when it was at magnitude 9.3. Nothing was seen brighter than magnitude 13.0 with the same equipment in exposures taken at 10:12 UT on March 14, 2021. For the first seven months after discovery, the nova's brightness stayed at a rough plateau, fading and rebrightening at least eight times; it is considered a very slow nova. After the seven month long series of peaks, Nova Cassiopeiae began a linear decline in brightness. This nova has been detected throughout the electromagnetic spectrum, from radio to gamma rays.
NGC 2617 is a Seyfert galaxy in the equatorial constellation of Hydra. It was discovered on February 12, 1885, by French astronomer Édouard Stephan. In 1888, Danish astronomer J. L. E. Dreyer described it as "extremely faint, very small, 2 very faint stars involved". It is located at an estimated distance of 202 million light years. In the infrared, the galaxy has an angular size of 0.693 by 0.652 arcminutes.