GRBOX GRBOX : Gamma-Ray Burst Online Index

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v 0.6 (BETA)

Greiner
GRB T90 commentsRA Decz XOR refs
021219 4 18:50:30 +31:54:00       1
021211 5.7 Bright, long burst. Early color variation. Possible supernova. 08:08:59.883 +06:43:37.88 1.006   y   19
021206 20 Brightest GRB in 15 years. High energy emission limits quantum gravity, but redshift unknown. Extreme polarization claimed; discredited. High-energy hardening. 16:00:46.85 -09:42:33.5     y 8
021204 No optical afterglow detected. 06:20:33 +32:06:13      
021201 0.3 Short, hard burst. Simultaneous images (optical/gamma ray), no afterglow detected. 08:07:46.09 +21:14:17.73      
021125A 20 First INTEGRAL burst. 19:47:56 +28:23:28       1
021125B 10 00:08:56.88 -35:15:28.80
021113 20 Long, dark burst. 00:04:24.96 -35:12:36      
021112 5 Long, possibly dark burst. 02:36:52 +48:50:56      
021104 26 Long, X-ray rich burst. 00:00:10.08 -35:19:51.6      
021023 15 IPN burst; small error box 07:24:55.03 -16:16:51.55      
021021 13 XRF. 00:17:23 -01:37:00      
021020 20 21:29:10.92 51:55:00.43      
021016 90 00:33:43.62 46:47:16      
021013 100 14:51:55.41 -56:13:55.57      
021008B 10 11:42:42 +36:48:43.2
021008A 30 Very high fluence. 12:45:47.73 44:10:59.79      
021004 100 Intrinsically brightest late-time afterglow. Complicated light curve - energy reinjections, density variations? 00:26:54.68 +18:55:41.6 2.323 y y y 45
020923 5 Two possible position regions; only one is listed. 14:06:07.54 50:31:18.25      
020910 25 13:56:00.57 -44:43:36.34      
020904 15 00:44:28.95 -68:57:38.48      
020903 3.3 Extremely soft spectrum. First XRF afterglow. Low-z host; Possible supernova association. 22:48:42.34 -20:46:09.30 0.251   y y 6
020819 20 AKA 020819B. Dark GRB with optical afterglow at large offset from spiral host galaxy w/super-solar metallicity. 23:27:19.47 +06:15:55.95 0.41 6
020813A 125 Long, bright burst. Early break; smooth light curve. 19:46:41.87 -19:36:04.81 1.2545 y y y 15
020812 20 Possible bright OT detection; not confirmed. 20:38:48 -05:23:34      
020801 300 21:02:14 -53:46:13      
020715 10 Relatively small error box; no afterglow detected. 13:50:12.66 61:50:43.79      
020714 20 12:09:04.48 83:06:44.26      
020708 150 07:58:05.36 41:35:38.95      
020706 20 14:21:35.25 -55:45:41.76      
020625B XRF; unreleased in GCNs. 20:44:13.9 +07:10:11      
020625 125 Long burst. First phase very hard, second phase very soft (XRB, 86s later). 20:44:14 +07:10:12
020604 10 IPN burst, crowded field. OT not confirmed. 16:27:38.28 -29:47:38      
020603 1.5 Short, hard burst. 15:46:35.53 -22:15:12.95      
020531 1 Short-hard burst. Difficulties localizing. Possible host galaxy (z=1). 15:15:11.18 -19:24:27.8       5
020525 25 11:29:32.93 -20:21:05.28      
020427 66 Bright XRF. Redshift less than 2.3. 22:09:28.26 -65:19:31.78 y     5
020418 15 08:00:17.58 -48:38:43.64
020413 10 00:59:39 -07:06:25.23      
020410 1600 Ultra-long (>1600s). Faint afterglow; HST supernova. 22:06:31.87 -83:49:28.3 ~0.5? y y   3
020409 Dark burst? 08:45:14.33 +66:41:16.08      
020405 40 Source in star-forming region. Polarization; radio flare. Associated supernova. 13:58:03.12 -31:22:21.90 0.695   y y 11
020331 20 Long burst. Possible host galaxy identified. Rebrightening. 13:16:09.54 -17:55:15.9   y  
020322 Bright X-ray afterglow. 18:01:04.2 +81:06:28.17 y y   1
020321 90 Faint burst; faint (probable) afterglow. 16:12:43.7 -83:43:13.9       2
020317 10 Low fluence, strong spectral evolution. 10:23:21 +12:44:38      
020305 280 Possible rebrightening. Faint host. 12:42:27.94 -14:18:11.8   y   2
020127 8.2 Extremely luminous, red host galaxy (ERO). Optical AG limits are shallow. 08:15:01.42 +36:46:33.9 1.9 y   y 2
020124 70 Extremely faint host galaxy (mag>29.5). Dark burst; not obscured. 09:32:50.81 -11:31:10.6 3.198   y   2

Returned 49 GRBs: Show raw XML for these GRBs | Save GRBs as Google KML | Save GRBs as starlist | Display this table as text file


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T90:
short (<1.5s)
intermediate (1.5-4.0s)
long (>4s)

 

Position:
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Redshift:
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Site created and maintained by Daniel Perley (now at Caltech).
This work was initially supported by NASA/Swift Guest Investigator grant NNG06GH50G, the Sloan Foundation Fellows program and Hellman Faculty Fund.

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