List of fast radio bursts

Last updated

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.

NameDate 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 0103122001-03-12 11:06:47.9805h 27m−64° 561187±1424.3±1.30.2±0.0510.14±0.15
FRB 010621 [1] 2001-06-21 13:02:11.3018h 52m−08° 30748±38+4
−2.3
0.53+0.26
−0.09
2.41±0.03
FRB 010724 [2] 2001-07-24 19:50:01.6901h 18m−75° 12375±313+5
−11
30+10
−10
3.42±0.05"Lorimer Burst"
FRB 011025 [3] 2001-01-25 00:29:15.7919h 07m−40° 37790.3±39.4±0.20.54+0.11
−0.07
6.62±0.10Announced in 2014 as FRB 011025 (from data archived in 2001).
FRB 090625 [4] 2009-06-25 21:53:52.8503h 07m−29° 55899.55±0.011.9+0
−1.9
1.14+0.42
−0.21
8.22±0.12
FRB 1102142011-02-14 07:14:10.35301h 21m−49° 47168.9±0.51.9±0.927+1028
−0
1.79±0.02
FRB 110220 [5] 2011-02-20 01:55:48.09622h 35m−12° 24944.38±0.055.6±0.11.38.48±0.12
FRB 110523 [6] [7] [8] 2011-05-23 15:06:19.721h 45m−00° 10623.30±0.061.73±0.170.65.77±0.09700–900 MHz at Green Bank radio telescope, detection of both circular and linear polarization.
FRB 110626 [5] 2011-06-26 21:33:17.47721h 04m−44° 44723.0±0.31.41+1.22
−0.45
0.63+1.22
−0.12
6.62±0.10
FRB 110703 [5] 2011-07-03 18:59:40.60723h 31m−02° 521103.6±0.73.9+2.24
−1.85
0.48+0.28
−0.10
9.72±0.14
FRB 120127 [5] 2012-01-27 08:11:21.72523h 15m−18° 26553.3±0.31.21+0.64
−0.25
0.62+0.35
−0.10
5.25±0.09
FRB 121002.1 [9] [4] 2012-10-02 13:09:18.40218h 15m−85° 121629.18±0.025.44+3.5
−1.2
0.3912.82±0.17double burst 5.1 ms apart
FRB 121002.2 [4] 2012-10-02 13:09:18.460.43+0.33
−0.06
FRB 1210292012-10-29 16:06:26.000h 12m+42° 04732±5320±400.346.46±0.10
FRB 121102 [10] 2012-11-02 06:35:53.24405h 31m 58.7s+33° 08 52.6557±23.0±0.50.4+0.4
−0.1
3.85±0.06by Arecibo radio telescope
FRB 130626 [4] 2013-06-26 14:55:59.77116h 27m−07° 28952.4±0.11.98+1.2
−0.44
0.74+0.49
−0.11
8.22±0.12
FRB 130628 [4] 2013-06-28 03:58:00.17809h 03m+03° 26469.88±0.010.64±0.131.91+0.29
−0.23
4.30±0.08
FRB 130729 [4] 2013-07-29 09:01:51.1913h 41m−06° 00861±215.61+9.98
−6.27
0.22+0.17
−0.046
7.80±0.11
FRB 1310302013-10-30 16:13:15.0000h 25m+39° 59203±4530±400.241.50±0.02
FRB 131104 [11] 2013-11-04 18:04:01.206h 44m−51° 17779±12.37+0.89
−0.45
1.16+0.35
−0.126
6.88±0.10'near' Carina Dwarf Spheroidal Galaxy
FRB 1402122014-02-12 10:31:14.0001h 31m+30° 32910±4390±400.268.15±0.12
FRB 140514 [12] 2014-05-14 17:14:11.0622h 34m−12° 19562.7±0.62.8+3.5
−0.7
0.47+0.099
−0.136
5.32±0.0821 ± 7 per cent (3σ) circular polarization
FRB 1411132014-11-13 07:42:55.2206h 13m+18° 47400.320.0391.96±0.02
FRB 1412162014-12-16 13:03:24.0000h 14m+41° 38545±5870±400.234.83±0.09
FRB 150215 [13] 2015-02-15 20:41:41.71418h 17m−04° 541105.6±0.82.88+1.2
−0.57
0.7+0.28
−0.095
6.72±0.1043% linear 3% circular polarized
FRB 1504182015-04-18 04:29:06.65707h 17m−19° 01776.2±0.50.8±0.32.2+0.6
−0.3
5.84±0.09Detection of linear polarization. The origin of the burst is disputed. [14] [15] [16] [17]
FRB 150517.12015-05-17 17:42:08.71205h 31m 58.7s+33° 08 52.6560±43.8±0.40.033.85±0.0610 repeat bursts at FRB 121102 location: 2 bursts on May 17 and 8 bursts on June 2 [18] [19]
FRB 150517.22015-05-17 17:51:40.921566±103.3±0.40.03
FRB 150602.12015-06-02 16:38:07.575555±34.6±0.30.04
FRB 150602.22015-06-02 16:47:36.484558±108.7±1.50.02
FRB 150602.32015-06-02 17:49:18.627559±102.8±0.40.02
FRB 150602.42015-06-02 17:49:41.3196.1±1.40.02
FRB 150602.52015-06-02 17:50:39.298556.5±3.76.6±0.10.14
FRB 150602.62015-06-02 17:53:45.528557.4±3.76.0±0.30.05
FRB 150602.72015-06-02 17:56:34.787558.7±4.98.0±0.50.05
FRB 150602.82015-06-02 17:57:32.020556.5±1.13.06±0.040.31
FRB 1506102015-06-10 05:26:59.39610h 44m−40° 051593.9±0.62±10.7±0.212.17±0.16
FRB 1508072015-08-07 17:53:55.8322h 43m−55° 05266.5±0.10.35±0.05128±52.45±0.03
FRB 151018.12015-10-18 01:05:48.0005h 31m 58.7s+33° 08 52.6570±5650+0
−650
1.43.85±0.06double burst 2.5 seconds apart at FRB121102 location
FRB 151018.22015-10-18 01:05:50.50400+0
−400
FRB 1511132015-11-13 08:32:42.375559.9±7.16.73±1.120.045 repeat bursts at FRB121102 location: 1 burst on November 13 and 4 bursts on November 19
FRB 151119.12015-11-19 10:44:40.524565.1±5.26.1±0.570.06
FRB 151119.22015-11-19 10:51:34.957568.8±6.66.14±10.04
FRB 151119.32015-11-19 10:58:56.2344.3±1.40.02
FRB 151119.42015-11-19 11:05:52.492560.0±6.45.97±0.350.09
FRB 1511252015-11-25 15:42:36.0001h 32m+30° 59273±41680±400.542.38±0.03
FRB 1512062015-12-06 06:17:52.7819h 21m−04° 081909.8±0.63±0.60.3±0.0414.29±0.20
FRB 1512082015-12-08 04:54:40.2605h 31m 58.7s+33° 08 52.6558.6±1.72.5±0.230.033.85±0.06at FRB121102 location
FRB 1512302015-12-30 16:15:46.52509h 41m−03° 27960.4±0.54.4±0.50.42±0.038.90±0.13
FRB 1601022016-01-02 08:28:39.37422h 39m−30° 112596.1±0.33.4±0.80.5±0.117.81±0.27
FRB 1602062016-02-06 10:26:50.0001h 01m+41° 381262±51590±400.2610.67±0.15
FRB 160317 [20] 2016-03-17 09:00:36.5307h 54m−29° 371165±1121±738.09±0.11First FRB observed by the interferometer UTMOST
FRB 160410 [20] 2016-04-10 08:33:39.6808h 41m+06° 05278±34±172.35±0.03
FRB 160608 [20] 2016-06-08 03:53:01.08807h 37m−40° 48682±79±64.34.60±0.09
FRB 1608232016-08-23 17:51:23.92105h 31m 58.7s+33° 08 52.6567±223.85±0.06at FRB121102 location
FRB 1609202016-09-20 03:05:43.0005h 34m+41° 451767±450000.2212.23±0.16
FRB 1612022016-12-02 13:24:54.0023h 44m+40° 48291±4810±400.292.38±0.03
FRB 170107 [21] 2017-01-07 20:05:08.13911h 23m−05° 00609.5±0.52.4±0.224.15.81±0.09first by ASKAP, high fluence ~58 Jy ms. In Leo. Galactic latitude 51°, Distance 3.1 Gpc, isotropic energy ~3 x 1034 J [21]
FRB 1704162017-04-16 23:11:12.79922h 13m−55° 02523.2±0.25±0.619.44.92±0.09
FRB 1704282017-04-28 18:02:34.70021h 47m−41° 51991.7±0.94.4±0.57.78.84±0.13
FRB 1706062017-06-06 10:03:27.0005h 34m+41° 45247±533000.54
FRB 1707072017-07-07 06:17:34.35402h 59m−57° 16235.2±0.63.5±0.514.82.15±0.02
FRB 1707122017-07-12 13:22:17.39422h 36m−60° 57312.79±0.071.4±0.337.82.94±0.04
FRB 170826.1-152017-08-26 13:52:01.25205h 31m 58.7s+33° 08 52.6565±51.740.383.85±0.0615 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 16:20:1800h 49m−65° 33176.80±0.040.40±0.0160±201.57±0.02low DM
FRB 1709062017-09-06 13:06:56.48822h 00m−19° 57390.3±0.42.5±0.329.63.69±0.05
FRB 170922 [24] 2017-09-22 11:23:33.421h 30m−08° 001111±134.1+2.6
−2.8
2.3±0.59.03±0.13extreme scattering (long pulse)
FRB 1710032017-10-03 04:07:23.78112h 30m−14° 07463.2±1.22.0±0.240.54.37±0.08
FRB 1710042017-10-04 03:23:39.25011h 58m−11° 54304.0±0.32.0±0.3222.84±0.04
FRB 1710192017-10-19 13:26:40.09722h 18m−08° 35460.8±1.15.4±0.340.54.37±0.08repeating FRB
FRB 1710202017-10-20 10:27:58.59822h 15m−19° 40114.1±0.23.2±0.5117.60.85±0.01
FRB 1711162017-11-16 14:59:33.30503h 31m−17° 14618.5±0.53.2±0.519.65.87±0.09
FRB 171209 [25] 2017-12-09 20:34:23.515h 50m−46° 101457.4±0.032.51.4814.71±0.21
FRB 1712132017-12-13 14:22:40.46703h 39m−10° 56158.6±0.21.5±0.288.61.34±0.02
FRB 1712162017-12-16 17:59:10.82203h 28m−57° 04203.1±0.51.9±0.3211.79±0.02
FRB 1801102018-01-10 07:34:34.95921h 53m−35° 27715.7±0.23.2±0.2128.16.69±0.10
FRB 1801192018-01-19 12:24:40.74703h 29m−12° 44402.7±0.72.7±0.540.73.85±0.06
FRB 180128.12018-01-28 00:59:38.61713h 56m−06° 43441.4±0.22.9±0.317.54.24±0.07
FRB 180128.22018-01-28 04:53:26.79622h 22m−60° 15495.9±0.72.3±0.228.74.73±0.09
FRB 1801302018-01-30 04:55:29.99321h 52m−38° 34343.5±0.44.1±123.13.23±0.05
FRB 1801312018-01-31 05:45:04.32021h 50m−40° 41657.7±0.54.5±0.422.26.16±0.09
FRB 1802122018-02-12 23:45:04.39914h 21m−03° 35167.5±0.51.81±0.06531.47±0.02
FRB 180301 [26] 2018-03-01 07:34:19.7606h 13m+04° 3452030.5positive spectrum, from Breakthrough Listen
FRB 180309 [27] 2018-03-09 02:49:32.9921h 25m−33° 59263.42±0.010.47527.62.41±0.03
FRB 180311 [28] 2018-03-11 04:11:54.8021h 32m−57° 441570.9±0.513.40.1516.86±0.25
FRB 1803152018-03-15 05:05:30.98519h 35m−26° 50479±0.42.4±0.323.34.57±0.09
FRB 1803212018-03-21 07:05:54.0000h 33m+42° 02594±51670±400.545.35±0.09
FRB 1803242018-03-24 09:31:46.70606h 16m−34° 47431±0.44.3±0.516.53.78±0.06
FRB 1804172018-04-17 13:18:31.0012h 25m+14° 13474.82.5221.84.63±0.09
FRB 1804302018-04-30 10:00:35.7006h 51m−09° 57264.1±0.51.2147.5±3.31.08±0.01
FRB 1805152018-05-15 21:57:26.48523h 13m−42° 15355.2±0.51.9±0.424.22.58±0.04
FRB 1805252018-05-25 15:19:06.51514h 40m−02° 12388.1±0.33.8±0.178.93.72±0.05
FRB 1805282018-05-28 04:24:00.906h 39m−49° 54899.3±0.62.0±0.215.759.75±0.14
FRB 1807142018-07-14 10:00:08.717h 46m−11° 461467.92±0.32.90.614.87±0.21
FRB 180725 [29] 2018-07-25 17:59:32.81306h 13m+67° 04715.98±0.020.31+0.08
−0.07
396.43±0.10first detection of an FRB at radio frequencies below 700 MHz
realtime detection by CHIME
FRB 1807272018-07-27 00:52:04.47413h 11m+26° 26642.07±0.030.78±0.16186.20±0.10
FRB 180729.12018-07-29 00:48:19.23813h 16m+55° 32109.61±0.0020.12±0.012830.85±0.01
FRB 180729.22018-07-29 17:28:18.25805h 58m+56° 30317.37±0.010.081132.38±0.03
FRB 1807302018-07-30 03:37:25.93703h 53m+87° 12849.047±0.0020.42±0.041197.66±0.11
FRB 1808012018-08-01 08:47:14.79321h 30m+72° 43656.2±0.030.51±0.09555.71±0.09
FRB 1808062018-08-06 14:13:03.10715h 15m+75° 38739.98±0.030.69356.91±0.11
FRB 180810.12018-08-10 17:28:54.61406h 46m+34° 52414.95±0.020.27413.29±0.05
FRB 180810.22018-08-10 22:40:42.49311h 59m+83° 07169.134±0.0020.28±0.03611.34±0.02
FRB 1808122018-08-12 11:45:32.87201h 12m+80° 47802.57±0.041.25+0.49
−0.47
147.08±0.11
FRB 180814.12018-08-14 14:20:14.44015h 54m+74° 01238.32±0.010.181392.12±0.02
FRB 180814.2 [30] 2018-08-14 14:49:48.02204h 22m 22s+73° 40189.38±0.092.6±0.28.11.11±0.01Detected by CHIME. Second repeating FRB to be discovered and first since 2012.
FRB 1808172018-08-17 01:49:20.20215h 33m+42° 121006.84±0.0020.37709.20±0.14
FRB 1809062018-09-06 01:17:47.38004h 22m 22s+73° 40191±33.95.41.11±0.01at FRB 180814.2 location
FRB 1809112018-09-11 12:59:13.733189.8±0.97.90.43
FRB 180916 2018-09-16 10:15:19.80301h 58m 00.75s+65° 43 00.5349.2±0.41.4±0.071.4±0.61.63±0.020.45±0.02repeating FRB localized to a nearby spiral galaxy
FRB 1809172018-09-17 00:46:35.35904h 22m 22s+73° 40189.5±0.1631.01.11±0.01at FRB 180814.2 location
FRB 1809192018-09-19 12:36:09.141190±0.1160.75
FRB 180924 [31] 2018-09-24 16:23:12.626521h 44m 25.26s−40° 54 00.1361.42±0.061.3±0.09164.26±0.073.99±0.06first non-repeating FRB whose source has been localized
FRB 1810162018-10-16 04:16:56.3015h 46m−25° 251982.8±2.88.6+0.7
−0.8
10.1917.78±0.27
FRB 181017.12018-10-17 10:24:37.4022h 06m−08° 51239.97±0.030.33902.54±0.04
FRB 181017.22018-10-17 23:26:11.8617h 05m+68° 171281.9±0.413.4±0.10.4±0.310.89±0.15repeating FRB
FRB 1810192018-10-19 08:13:22.7501h 58m 00.75s+65° 43 00.5349.0±0.64.1±0.30.6±0.31.63±0.020.45±0.02burst at FRB 180916 location
FRB 1810282018-10-28 10:12:31.47704h 22m 22s+73° 40188.9±0.5420.291.11±0.01at FRB 180814.2 location
FRB 181030.12018-10-30 04:13:13.02510h 54m+73° 44103.5±0.70.59±0.083.2±1.70.68±0.010.088±0.003repeating FRB, most likely originating from NGC 3403.
FRB 181030.22018-10-30 04:16:21.654103.5±0.31.43±0.083.1±1.4
FRB 181104.12018-11-04 06:57:18.58501h 58m 00.75s+65° 43 00.5349.5±0.31.37±0.071.4±0.51.63±0.020.45±0.02burst at FRB 180916 location
FRB 181104.22018-11-04 07:07:01.591349.6±0.26.3±1.10.4±0.2
FRB 1811122018-11-12 17:31:15.48321h 49m−52° 58589.27±0.032.1±0.2124.96±0.095.81±0.10localized to a small galaxy
FRB 1811192018-11-19 16:49:03.19112h 42m+65° 08364.2±16.3±0.60.3±0.23.49±0.05repeating FRB
FRB 1811202018-11-20 05:56:06.23201h 58m 00.75s+65° 43 00.5349.9±0.61.1±0.091.1±0.51.63±0.020.45±0.02burst at FRB 180916 location
FRB 1811282018-11-28 08:27:41.74004h 56m+63° 23450.2±0.32.43±0.160.5±0.33.56±0.05repeating FRB
FRB 1812192018-12-19 07:04:41.678450.8±0.35.5±0.70.3±0.2
FRB 1812222018-12-22 03:59:23.20801h 58m 00.75s+65° 43 00.5349.1±0.14.95±0.014.9±1.81.63±0.020.45±0.02burst at FRB 180916 location
FRB 1812232018-12-23 03:51:28.960349.7±0.71.06±0.051.7±0.6
FRB 1812252018-12-25 03:53:03.926348.9±0.71.3±0.30.4±0.2
FRB 1812262018-12-26 03:43:30.107348.8±0.20.87±0.031.6±0.6
FRB 1812282018-12-28 13:48:50.1006h 09m−45° 58354.2±0.91.24+0.13
−0.15
19.233.78±0.06
FRB 1901032019-01-03 13:47:23.32212h 42m+65° 08364.0±0.32.66±0.10.6±0.33.49±0.05burst at FRB 181119 location
FRB 190116.12019-01-16 13:07:33.83312h 49m+27° 09444.0±0.64.0±0.50.3±0.24.37±0.08repeating FRB
FRB 190116.22019-01-16 13:08:20.412443.6±0.81.5±0.30.4±0.2
FRB 1901262019-01-26 01:32:45.32801h 58m 00.75s+65° 43 00.5349.8±0.52.53±0.130.7±0.31.63±0.02
FRB 1902092019-02-09 08:20:20.97709h 37m+77° 40424.6±0.63.7±0.50.4±0.23.95±0.07repeating FRB
FRB 1902102019-02-10 08:17:13.907425.2±0.59.4±1.40.6±0.4
FRB 1902162019-02-16 15:26:58.02917h 05m+68° 171281.0±0.620.2±1.70.4±0.210.89±0.15burst at FRB 181017.2 location
FRB 1902222019-02-22 18:46:01.36720h 52m+69° 50460.6±0.12.97±0.901.9±0.63.91±0.07repeating FRB
FRB 1903012019-03-01 18:03:02.479459.8±0.42.44±0.81.4±0.5
FRB 1903132019-03-13 09:21:46.72512h 42m+65° 08364.2±0.61.5±0.20.4±0.23.49±0.05burst at FRB 181119 location
FRB 1905232019-05-23 06:05:55.81513h 48m 15.6s+72° 28 11760.8±0.60.42±0.056707.08±0.117.51±0.06localized to only 5 arcseconds
FRB 1907112019-07-11 01:53:41.09321h 56m−80° 23593±2
FRB 1907142019-07-14 05:17:12.90112h 16m−13° 00504±2
FRB 1908052019-08-05 09:21:0822h 18m−08° 35460.4±0.26±2burst at FRB 171019 location
FRB 1908062019-08-06 17:07:58.000h 02m−07° 35388.5
FRB 1909062019-09-06 00:08:4605h 31m 58.7s33° 08 52.6burst at FRB 121102 location
FRB 190910.1-122019-09-1212 bursts detected at FRB 121102 location in a 3-hour timespan
FRB 1910012019-10-01 16:55:35.97121h 32m−54° 40506.92±0.044.37±0.08
FRB 1911072019-11-07 18:55:36.708h 02m−13° 44714.25
FRB 1912232019-12-23 04:55:31.220h 34m−75° 09665
FRB 1912282019-12-28 09:16:16.44422h 57m−29° 46297.9±0.5
FRB 200120 [32] 2020-01-20
FRB 200428 2020-04-2819h 35m+21° 54332.8
FRB 201124 2020-11-24
08:50:41
05h 08m+26° 11413.52±0.05very 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° 53412±3
FRB 210402 2021-04-02 05:48:59.114(1)05h 08m+26° 02414±3

Notes

  1. 1 2 3 The dispersion measure (DM) measures how much dust a radio signal had to pass through, as higher frequencies penetrate dust more quickly than lower frequencies, creating a delayed signal across different radio frequencies.
    If one compares the DM of a radio burst to the amount of known dust in the Milky Way in that direction, as well as the density of dust in intergalactic space, a very rough distance can be inferred.
    In reality, the actual distance is usually shorter, as fast radio bursts appear to originate inside galaxies with their own concentrated dust clouds, dispersing the signal even more and making it appear much further from the Milky Way than it truly is.

Related Research Articles

<span class="mw-page-title-main">NGC 300</span> Galaxy in the constellation Sculptor

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.

<span class="mw-page-title-main">V1494 Aquilae</span> Nova seen in 1999 in the constellation of Aquila

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.

<span class="mw-page-title-main">YZ Ceti</span> Star in the constellation Cetus

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.

<span class="mw-page-title-main">NGC 4725</span> Galaxy in the constellation Coma Berenices

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.

<span class="mw-page-title-main">KT Eridani</span> Star in the constellation Eridanus

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.

<span class="mw-page-title-main">Fast radio burst</span> Astronomical high energy transient pulse

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.

<span class="mw-page-title-main">Peryton (astronomy)</span> Short man-made radio signals

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.

<span class="mw-page-title-main">V5856 Sagittarii</span> Nova that occurred in 2016

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.

<span class="mw-page-title-main">V407 Lupi</span> Nova that occurred in 2016

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.

<span class="mw-page-title-main">SN 2018cow</span> Supernova event of June 2018 in the constellation Hercules

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.

<span class="mw-page-title-main">FRB 180916.J0158+65</span>

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.

<span class="mw-page-title-main">SGR 1935+2154</span> Soft gamma repeater in the constellation Vulpecula

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.

<span class="mw-page-title-main">Fast blue optical transient</span> Astronomical observation

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.

<span class="mw-page-title-main">YZ Reticuli</span> 2020 Nova in the constellation Reticulum

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.

<span class="mw-page-title-main">SN 2020oi</span> Extragalactic supernova in 2020

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.

<span class="mw-page-title-main">AP Librae</span> Active galactic nucleus in the constellation Libra

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.

<span class="mw-page-title-main">V4332 Sagittarii</span>

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.

<span class="mw-page-title-main">Nova Cassiopeiae 2021</span> Nova in the constellation Cassiopeia seen in 2021

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.

<span class="mw-page-title-main">NGC 2617</span> Galaxy in the constellation Hydra

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.

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