440:
125:
64:
44:
161:
288:, an Italian–Dutch satellite originally designed to study X-rays. The burst lasted around 80 seconds and had multiple peaks in its light curve. Gamma-ray bursts have very diverse time profiles, and it is not fully understood why some bursts have multiple peaks and some have only one. One possible explanation is that multiple peaks are formed when the source of the gamma-ray burst undergoes
1125:
Costa, E.; Frontera, F.; Heise, J.; Feroci, M.; In 't Zand, J.; Fiore, F.; Cinti, M. N.; Dal Fiume, D.; Nicastro, L.; Orlandini, M.; Palazzi, E.; Rapisarda, M.; Zavattini, G.; Jager, R.; Parmar, A.; Owens, A.; Molendi, S.; Cusumano, G.; MacCarone, M. C.; Giarrusso, S.; Coletta, A.; Antonelli, L. A.;
1272:
Galama, T. J.; Tanvir, N.; Vreeswijk, P. M.; Wijers, R. A. M. J.; Groot, P. J.; Rol, E.; Van
Paradijs, J.; Kouveliotou, C.; Fruchter, A. S.; Masetti, N.; Pedersen, H.; Margon, B.; Deutsch, E. W.; Metzger, M.; Armus, L.; Klose, S.; Stecklum, B. (10 June 2000). "Evidence for a Supernova in Reanalyzed
1814:
van
Paradijs, J.; Groot, P. J.; Galama, T.; Kouveliotou, C.; Strom, R. G.; Telting, J.; Rutten, R. G. M.; Fishman, G. J.; Meegan, C. A.; Pettini, M.; Tanvir, N.; Bloom, J.; Pedersen, H.; Nørdgaard-Nielsen, H. U.; Linden-Vørnle, M.; Melnick, J.; Van Der Steene, G.; Bremer, M.; Naber, R.; Heise, J.;
476:
Galama analyzed the light curve of the burst and found that its luminosity decayed at different rates at different times. The luminosity decayed more slowly between March 6 and April 7 than it did before and after these dates. Galama concluded that the earlier light curve had been dominated by the
1060:
Butler, Nathaniel R.; Marshall, Herman L.; Ricker, George R.; Vanderspek, Roland K.; Ford, Peter G.; Crew, Geoffrey B.; Lamb, Donald Q.; Jernigan, J. Garrett (10 November 2003). "The X-ray
Afterglows of GRB 020813 and GRB 021004 with Chandra HETGS: Possible Evidence for a Supernova prior to GRB
1012:
Bloom, J. S.; Kulkarni, S. R.; Djorgovski, S. G.; Eichelberger, A. C.; Côté, P.; Blakeslee, J. P.; Odewahn, S. C.; Harrison, F. A.; Frail, D. A.; Filippenko, A. V.; Leonard, D. C.; Riess, A. G.; Spinrad, H.; Stern, D.; Bunker, A.; Dey, A.; Grossan, B.; Perlmutter, S.; Knop, R. A.; Hook, I. M.;
501:. Although GRB 980326 did not provide enough information to definitively rule out this explanation, Reichart showed that the light curve of GRB 970228 could only have been caused by a supernova. Definitive evidence linking gamma-ray bursts and supernovae was eventually found in the
27:
326:
Later images after the point source faded revealed a faint galaxy at almost the same position, the presumed host galaxy of the burst; a chance position coincidence was unlikely but possible, so the cosmological origin of GRBs was not conclusive until observations of
533:
patch at the burst's position, almost certainly a distant galaxy. Although there was a remote chance that the burst and this galaxy were unrelated, their positional coincidence provided strong evidence that GRBs occur in distant galaxies rather than within the
406:
showed that the afterglow coincided with a distant, small galaxy: the first evidence of the extragalactic, cosmological nature of Gamma-ray bursts. After the gamma-ray bursts itself had faded away, very deep observations taken with the
1765:
Stanek, Krzysztof Z.; Matheson, T.; Garnavich, P. M.; Martini, P.; Berlind, P.; Caldwell, N.; Challis, P.; Brown, W. R.; et al. (12 June 2003). "Spectroscopic
Discovery of the Supernova 2003dh Associated with GRB0303291".
485:
than the early afterglow, an observation which conflicted with the then-preferred relativistic fireball model for the gamma-ray burst emission mechanism. He also observed that the only GRB with a similar temporal profile was
382:
was the first GRB afterglow ever detected. Power-law decays have since been recognized as a common feature in GRB afterglows, although most afterglows decay at differing rates during different phases of their lifetimes.
363:, a phenomenon that would later be referred to as a radio afterglow. Jonathan Katz later concluded that this lower-energy emission would not be limited to radio waves, but should range in frequency from radio waves to
411:
showed the underlying galaxy to have a redshift of 0.695. The predicted radio afterglow was never detected for this burst. At the time of this burst's discovery, GRBs were believed to emit radiation
374:
The Narrow Field
Instruments on board BeppoSAX began making observations of the GRB 970228's position within eight hours of its detection. A transient x-ray source was detected which faded with a
343:
and James E. Rhoads published an article arguing that, regardless of the type of explosion that causes GRBs, the extreme energetics of GRBs meant that matter from the host body must be ejected at
513:. However, supernova-like features only become apparent in the weeks following a burst, leaving the possibility that very early luminosity variations could be explained by dust echoes.
1697:
Reichart, Daniel E. (2001). "Light Curves and
Spectra of Dust Echoes from Gamma-Ray Bursts and Their Afterglows: Continued Evidence That GRB 970228 Is Associated with a Supernova".
292:. Within a few hours, the BeppoSAX team used the X-ray detection to determine the burst's position with an error box—a small area around the specific position to account for the
617:"GRB" indicates that the event was a gamma-ray burst, and the numbers follow a YYMMDD format corresponding to the date on which the burst occurred: 28 February 1997.
1650:
Reichart, Daniel E. (1999). "GRB 970228 Revisited: Evidence for a
Supernova in the Light Curve and Late Spectral Energy Distribution of the Afterglow".
1889:
1974:
1126:
Giommi, P.; Muller, J. M.; Piro, L.; Butler, R. C. (1997b). "Discovery of an X-ray afterglow associated with the γ-ray burst of 28 February 1997".
522:
462:
487:
1815:
In't Zand, J.; Costa, E.; Feroci, M.; Piro, L.; Frontera, F.; Zavattini, G.; Nicastro, L.; Palazzi, E.; Bennet, K.; et al. (1997).
1354:
Huang, Yong-feng; Tan, Chang-yi; Dai, Zi-gao; Lu, Tan (2002). "Are Gamma-ray Bursts Due to
Isotropic Fireballs or Cylindrical Jets?".
1013:
Feroci, M. (30 September 1999). "The unusual afterglow of the γ-ray burst of 26 March 1998 as evidence for a supernova connection".
1953:
1979:
557:. The redshift of the galaxy was later determined to be z = 0.695, which corresponds to a distance of approximately
1873:
1447:
Moran, Jane A.; Reichart, Daniel E. (10 October 2005). "Gamma-Ray Burst Dust Echoes
Revisited: Expectations at Early Times".
323:
of +11° 46′ 53.0″, providing the first arcsecond-accuracy localization of any Gamma-ray burst.
1755:
965:
Bloom, J. S.; Djorgovski, S. G.; Kulkarni, S. R. (2001). "The redshift and the ordinary host galaxy of GRB 970228".
469:
independently analyzed GRB 970228's optical light curve, both concluding that the host object may have undergone a
1885:"Precessing jets interacting with interstellar material as the origin for the light curves of gamma-ray bursts"
198:. Since 1993, physicists had predicted GRBs to be followed by a lower-energy afterglow (in wavelengths such as
1984:
1989:
447:
as it goes supernova, collapses into a black hole, and emits a gamma-ray burst along its axis of rotation
229:
and lasted approximately 80 seconds. Peculiarities in the light curve of GRB 970228 suggested that a
379:
355:. Should this shock front occur in a magnetic field, accelerated electrons in it would emit long-lasting
191:
164:
387:
308:
270:
219:
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Panaitescu, A. (15 May 2007). "Decay phases of Swift X-ray afterglows and the forward-shock model".
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of the host galaxy, effectively ruling out the possibility that the burst originated in an
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222:); this resulted in large positional uncertainties which left their nature very unclear.
8:
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1912:
1835:
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1673:
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1517:
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Paczyński, Bohdan; Rhoads, James E. (1993). "Radio
Transients from Gamma-Ray Bursters".
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394:. Comparison of the images revealed an object which had decreased in luminosity in both
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by the Gamma-Ray Burst Monitor (GRBM) and one of the Wide Field Cameras (WFCs) on board
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1070:
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1022:
1000:
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344:
1817:"Transient optical emission from the error box of the γ-ray burst of 28 February 1997"
1375:
497:
An alternative explanation for the light curves of GRB 970228 and GRB 980326 involved
16:
Gamma-ray burst detected on 28 Feb 1997, the first for which an afterglow was observed
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About one and nine days later, optical images of the error box were taken with the
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jets, a characteristic which lowers the total energy output of a burst by several
402:. This was the burst's optical afterglow. Deeper follow-up observations using the
311:
on La Palma; comparison of the images revealed a fading point source located at a
245:
of z = 0.695), providing early evidence that GRBs occur well beyond the
1957:
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454:
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347:
during the explosion. They predicted that the interaction between the ejecta and
312:
274:
187:
72:
37:
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1951:
BeppoSAX follow-up observations of the region of the Gamma-ray burst GRB 970228
399:
386:
Optical images were taken of GRB 970228's position on 1 and 8 March using the
1968:
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368:
207:
52:
1945:
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burst itself, whereas the later light curve was produced by the underlying
1903:
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1461:
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1140:
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1027:
979:
444:
352:
320:
226:
199:
84:
1198:
Esin, A. A.; Blandford, R. (2000). "Dust Echoes from Gamma-Ray Bursts".
173:
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510:
506:
498:
424:
420:
416:
328:
289:
262:
250:
238:
211:
1603:
Reichart, Daniel E. (19 February 1998). "The Redshift of GRB 970508".
249:; this was proven decisively two months later with a subsequent burst
233:
may have occurred as well. The position of the burst coincided with a
1843:
580:
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The position of the burst's afterglow was measurably offset from the
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Converting of the redshift into the distance done by on-line tools:
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996:
550:
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116:
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439:
1400:
Katz, J. I. (1994). "Low-Frequency Spectra of Gamma-Ray Bursts".
277:, a series of spacecraft designed to detect nuclear explosions.
530:
234:
210:), but until this event, GRBs had only been observed in highly
203:
160:
1883:
Zwart, Simon F. Portegies; Totani, Tomonori (17 August 2001).
490:, for which a supernova relation had already been proposed by
575:
568:. At this distance, the burst would have released a total of
473:
explosion several weeks before the gamma-ray burst occurred.
364:
142:
26:
415:. The afterglows from this burst and several others—such as
194:
was observed. It was detected on 28 February 1997 at 02:58
1747:
Flash! The Hunt for the Biggest Explosions in the Universe
538:. This conclusion was later supported by observations of
281:
195:
1175:"GRB 970228: Redshift and properties of the host galaxy"
423:—provided early evidence that GRBs emit radiation in
280:
GRB 970228 was detected on 28 February 1997 at 02:58
378:slope in the days following the burst. This x-ray
1890:Monthly Notices of the Royal Astronomical Society
1543:Philosophical Transactions of the Royal Society A
1273:Optical and Near-Infrared Images of GRB 970228".
1966:
648:. UCLA Division of Astronomy & Astrophysics
690:
688:
686:
646:"Ned Wright's Javascript Cosmology Calculator"
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481:. Reichart noted that the late afterglow was
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443:Artist's illustration showing the life of a
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521:During the night between 12 and 13 March,
273:. GRBs were first detected in 1967 by the
123:
62:
42:
25:
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1750:. Cambridge: Cambridge University Press.
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525:made observations of the region with the
89:+11° 46′ 53.0″
1592:IAU Circular 6635: GRB 970228; C/1995 O1
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1975:Astronomical objects discovered in 1997
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1967:
1611:(2). University of Chicago: L99–L101.
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1261:IAU Circular 6643: GRB 970228; 1997by
1114:IAU Circular 6572: GRB 970228; 1997aa
803:
434:
300:. The burst was also detected by the
632:
592:
261:A gamma-ray burst (GRB) is a highly
225:The burst had multiple peaks in its
13:
1812:
1356:Chinese Astronomy and Astrophysics
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14:
2001:
1939:
1173:Djorgovski, George (3 May 1999).
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1922:10.1046/j.1365-8711.2001.04913.x
1596:International Astronomical Union
1395:. Retrieved on 23 February 2010.
1393:International Astronomical Union
1347:International Astronomical Union
1330:International Astronomical Union
1265:International Astronomical Union
1118:International Astronomical Union
644:Wright, Edward L. (9 May 2008).
449:Credit: Nicolle Rager Fuller/NSF
159:
1864:. In Volken Schönfelder (ed.).
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1980:Long-duration gamma-ray bursts
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542:, the first burst to have its
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1605:Astrophysical Journal Letters
1389:IAU Circular 6578: GRB 970228
1376:10.1016/S0275-1062(02)00092-9
1343:IAU Circular 6588: GRB 970228
1326:IAU Circular 6584: GRB 970228
957:
269:, the most energetic form of
1011:
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237:about 8.1 billion
218:(the most energetic form of
107:8,123,000,000 ly (2.491
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1868:. Berlin: Springer-Verlag.
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1866:The Universe in Gamma Rays
1860:Varendoff, Martin (2001).
1744:Schilling, Govert (2002).
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388:William Herschel Telescope
309:William Herschel Telescope
296:in the position—of 3
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1275:The Astrophysical Journal
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1063:The Astrophysical Journal
799:Van Paradijs et al., 1997
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271:electromagnetic radiation
220:electromagnetic radiation
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529:. He discovered a faint
527:New Technology Telescope
404:New Technology Telescope
331:about two months later.
165:Related media on Commons
1368:2002ChA&A..26..414H
555:active galactic nucleus
467:University of Amsterdam
1946:Gamma-ray Burst 970228
1563:10.1098/rsta.2006.1985
451:
392:Isaac Newton Telescope
214:bursts of high-energy
1768:Astrophysical Journal
1699:Astrophysical Journal
1652:Astrophysical Journal
1496:Astrophysical Journal
1449:Astrophysical Journal
1402:Astrophysical Journal
1201:Astrophysical Journal
967:Astrophysical Journal
509:and the afterglow of
459:University of Chicago
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357:synchrotron radiation
1985:February 1997 events
1990:Astronomical events
1913:2001MNRAS.328..951P
1836:1997Natur.386..686V
1790:2003ApJ...591L..17S
1721:2001ApJ...554..643R
1674:1999ApJ...521L.111R
1627:1998ApJ...495L..99R
1590:. (22 April 1997) "
1555:2007RSPTA.365.1197P
1549:(1854): 1197–1205.
1518:1993ApJ...418L...5P
1471:2005ApJ...632..438M
1424:1994ApJ...432L.107K
1341:. (14 March 1997) "
1324:. (12 March 1997) "
1297:2000ApJ...536..185G
1224:2000ApJ...534L.151E
1191:1999GCN...289....1D
1150:1997Natur.387..783C
1085:2003ApJ...597.1010B
1037:1999Natur.401..453B
989:2001ApJ...554..678B
788:Groot 14 March 1997
604:Groot 12 March 1997
429:orders of magnitude
349:interstellar matter
345:relativistic speeds
190:(GRB) for which an
133:Total energy output
21:
1956:2011-03-03 at the
1862:"Gamma-Ray Bursts"
1387:. (8 March 1997) "
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435:Supernova relation
150:Other designations
121:0.695, 0.695
19:
1875:978-3-540-67874-8
1830:(6626): 686–689.
1134:(6635): 783–785.
1021:(6752): 453–456.
479:Type Ic supernova
361:radio frequencies
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1658:(2): L111–L115.
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1408:(2): L107–L109.
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1259:. (6 May 1997) "
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768:
757:
754:Paczyński 1993
746:
735:
724:
710:
706:Schilling 2002
698:
682:
678:Varendoff 2001
670:
666:Schilling 2002
658:
631:
627:Schilling 2002
619:
607:
590:
588:
585:
518:
515:
436:
433:
400:infrared light
336:
333:
258:
255:
186:was the first
179:
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155:
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55:
49:
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35:
31:
30:
15:
9:
6:
4:
3:
2:
2002:
1991:
1988:
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1978:
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1337:Groot, P. J.
1335:
1331:
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1320:Groot, P. J.
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1179:GCN Circulars
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1159:
1158:10.1038/42885
1155:
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1045:10.1038/46744
1042:
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1010:
1006:
1002:
998:
994:
990:
986:
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962:
951:
946:
940:
939:Reichart 1998
935:
928:
923:
917:
912:
906:
901:
895:
890:
884:
883:Reichart 2001
879:
873:
868:
862:
857:
851:
850:Reichart 1999
846:
844:
836:
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795:
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628:
623:
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591:
584:
582:
577:
566:
556:
552:
547:
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541:
537:
532:
528:
524:
523:Jorge Melnick
514:
512:
508:
504:
500:
495:
493:
489:
484:
480:
474:
472:
468:
464:
460:
456:
450:
446:
441:
432:
430:
426:
422:
418:
414:
413:isotropically
410:
405:
401:
397:
396:visible light
393:
389:
384:
381:
377:
372:
370:
369:visible light
366:
362:
358:
354:
350:
346:
342:
332:
330:
324:
322:
314:
310:
305:
304:space probe.
303:
299:
295:
291:
287:
283:
278:
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272:
268:
264:
254:
252:
248:
244:
240:
236:
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228:
223:
221:
217:
213:
209:
208:visible light
205:
201:
197:
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189:
185:
175:
169:
166:
162:
156:
152:
148:
144:
135:
131:
126:
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118:
114:
106:
102:
98:
96:
92:
88:
86:
82:
76:
74:
70:
65:
59:
56:
54:
53:Constellation
50:
45:
39:
36:
32:
28:
23:
1962:
1894:
1888:
1865:
1827:
1823:
1771:
1767:
1746:
1702:
1698:
1655:
1651:
1608:
1604:
1595:
1587:
1546:
1542:
1499:
1495:
1452:
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1392:
1384:
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1355:
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1338:
1329:
1321:
1278:
1274:
1264:
1256:
1205:
1199:
1182:
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1131:
1127:
1117:
1109:
1066:
1062:
1018:
1014:
970:
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911:
900:
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878:
867:
856:
830:
819:
794:
783:
771:
760:
749:
738:
727:
701:
673:
661:
650:. Retrieved
622:
548:
546:determined.
520:
496:
492:Joshua Bloom
475:
463:Titus Galama
453:
448:
445:massive star
385:
373:
367:, including
338:
325:
306:
279:
260:
257:Observations
224:
183:
182:
1383:Hurley, K.
1255:Fox, D. W.
1112:. (1997a) "
905:Stanek 2003
894:Butler 2003
861:Galama 2000
743:Hurley 1997
721:Costa 1997a
708:, pp. 58–60
695:Costa 1997b
668:, pp. 12–16
517:Host galaxy
499:dust echoes
353:shock front
321:declination
239:light-years
227:light curve
206:, and even
200:radio waves
111:10 pc)
85:Declination
1969:Categories
1108:Costa, E.
958:References
916:Moran 2005
872:Bloom 1999
824:Huang 2002
813:Bloom 2001
732:Zwart 2001
652:2010-06-11
583:emission.
540:GRB 970508
511:GRB 030329
507:GRB 020813
488:GRB 980326
425:collimated
421:GRB 971214
417:GRB 970508
329:GRB 970508
317:05 01 46.7
298:arcminutes
290:precession
267:gamma rays
251:GRB 970508
216:gamma rays
184:GRB 970228
153:GRB 970228
78:05 01 46.7
34:Event type
20:GRB 970228
1643:119394440
1502:: L5–L8.
1061:020813".
1053:205058997
765:Katz 1994
581:isotropic
579:assuming
536:Milky Way
471:supernova
380:afterglow
376:power-law
339:In 1993,
335:Afterglow
265:flash of
247:Milky Way
231:supernova
192:afterglow
1954:Archived
1579:12425394
1571:17293326
1534:17567870
1440:15787149
1313:34690851
1248:14962603
1240:10813670
1005:16648604
929:, p. 102
837:, p. 173
680:, p. 381
629:, p. 101
574:10
563:10
551:centroid
544:redshift
503:spectrum
390:and the
286:BeppoSAX
263:luminous
243:redshift
241:away (a
212:luminous
141:10
117:Redshift
104:Distance
1931:9509367
1909:Bibcode
1852:4248753
1832:Bibcode
1806:2561943
1786:Bibcode
1737:7492485
1717:Bibcode
1690:7344802
1670:Bibcode
1623:Bibcode
1551:Bibcode
1514:Bibcode
1487:7506509
1467:Bibcode
1420:Bibcode
1364:Bibcode
1293:Bibcode
1220:Bibcode
1187:Bibcode
1166:9505956
1146:Bibcode
1101:6171688
1081:Bibcode
1033:Bibcode
985:Bibcode
531:nebular
465:of the
457:of the
359:in the
302:Ulysses
1929:
1872:
1850:
1824:Nature
1804:
1754:
1735:
1688:
1641:
1577:
1569:
1532:
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1438:
1311:
1246:
1238:
1164:
1128:Nature
1099:
1051:
1015:Nature
1003:
483:redder
365:x-rays
319:and a
235:galaxy
204:x-rays
158:
60:
40:
1927:S2CID
1899:arXiv
1848:S2CID
1820:(PDF)
1802:S2CID
1776:arXiv
1733:S2CID
1707:arXiv
1686:S2CID
1660:arXiv
1639:S2CID
1613:arXiv
1588:et al
1575:S2CID
1530:S2CID
1504:arXiv
1483:S2CID
1457:arXiv
1436:S2CID
1410:arXiv
1385:et al
1339:et al
1322:et al
1309:S2CID
1283:arXiv
1257:et al
1244:S2CID
1210:arXiv
1185:: 1.
1162:S2CID
1136:arXiv
1110:et al
1097:S2CID
1071:arXiv
1049:S2CID
1023:arXiv
1001:S2CID
975:arXiv
587:Notes
559:8.123
294:error
172:[
99:J2000
95:Epoch
58:Orion
1870:ISBN
1752:ISBN
1567:PMID
1236:PMID
778:, §2
461:and
419:and
398:and
1917:doi
1895:328
1840:doi
1828:386
1794:doi
1772:591
1725:doi
1703:554
1678:doi
1656:521
1631:doi
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1594:".
1559:doi
1547:365
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1475:doi
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971:554
570:5.2
505:of
315:of
282:UTC
196:UTC
137:5.2
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576:J
572:×
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176:]
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139:×
109:×
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