80:
47:
651:
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642:. Further analysis by Frail and his colleagues indicated that the total energy released by the burst was approximately 5Ă10 ergs (5Ă10 J), and Rhoads determined that the total gamma-ray energy was approximately 3Ă10 erg (3Ă10 J). This implied that the gamma-ray and kinetic energy of the burst's ejecta were comparable, effectively ruling out those GRB models which are relatively inefficient at producing gamma rays.
1220:
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174:
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631:(the ultraviolet region of the spectrum) and 21.2 ± 0.1 in the R-band (the red region of the spectrum). The afterglow reached its peak luminosity in both bands approximately 2 days after the burst was first detectedâ19.6 ± 0.3 in the U-band at 02:13 UTC on May 11, and 19.8 ± 0.2 in the R-band at 20:55 UTC on May 10.
27:
1697:
Pederson, H.; Jaunsen, A. O.; Grav, T.; Ostensen, R.; Andersen, M. I.; Wold, M.; Kristen, H.; Broeils, A.; Naslund, M.; Fransson, C.; Lacy, M.; CastroâTirado, A. J.; Gorosabel, J.; Rodriguez
Espinosa, J. M.; Perez, A. M.; Wolf, C.; Fockenbrock, R.; Hjorth, J.; Muhli, P.; Hakala, P.; Piro, L.; Feroci,
1332:
Castro-Tirado, A. J.; Gorosabel, Javier; Benitez, Narciso; Wolf, Christian; Fockenbrock, Ralf; Martinez-Gonzalez, Enrique; Kristen, Helmuth; Broeils, Adrick; Pedersen, Holger; Greiner, Jochen; Costa, Enrico; Feroci, Marco; Piro, Luigi; Frontera, Filippo; Nicastro, Luciano; Palazzi, Eliana; Bartolini,
491:
After discovering the burst's X-ray afterglow, the BeppoSAX team provided a more accurate localization, and what
Metzger had assumed to be a variable star was still present in this smaller error box. Both the Caltech team and the Amsterdam team were hesitant to publish any conclusions on the variable
1370:
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.;
1745:
Pian, E.; Fruchter, A. S.; Bergeron, L. E.; Thorsett, S. E.; Frontera, F.; Tavani, M.; Costa, E.; Feroci, M.; Halpern, J.; Lucas, R. A.; Nicastro, L.; Palazzi, E.; Piro, L.; Sparks, W.; Castro-Tirado, A. J.; Gull, T.; Hurley, K.; Pedersen, H. (1998-01-10). "Hubble Space
Telescope Imaging of the
575:
On May 13, five days after the first detection of GRB 970508, Frail resumed his observations with the Very Large Array. He made observations of the burst's position at a wavelength of 3.5 cm and immediately detected a strong signal. After 24 hours, the 3.5 cm signal became
678:
Throughout the month of May the radio scintillations became less noticeable until they ceased altogether. This implies that the radio source significantly expanded in the time that had passed since the burst was detected. Using the known distance to the source and the elapsed time before the
459:
The following evening
Djorgovski again observed the region. He compared the images from both nights but the error box contained no objects that had decreased in luminosity between May 8 and May 9. Metzger noticed one object that had increased in luminosity, but he assumed it was a
620:/m), and the Wide Field Camera (2â26 keV) recorded a fluence of (0.7 ± 0.1) Ă 10 erg/cm (0.7 ± 0.1 nJ/m). BATSE (20â1000 keV) recorded a fluence of (3.1 ± 0.2) Ă 10 erg/cm (3.1 ± 0.2 nJ/m).
313:
1513:
Galama, T. J.; Groot, P. J.; Van
Paradijs, J.; Kouveliotou, C.; Strom, R. G.; Wijers, R. A. M. J.; Tanvir, N.; Bloom, J.; Centurion, M.; Telting, J.; Rutten, R. G. M.; Smith, P.; MacKey, C.; Smartt, S.; Benn, C.; Heise, J.; In't Zand, J. (1998-04-10).
1333:
Corrado; Guarnieri, Adriano; Masetti, Nicola; Piccioni, Adalberto; Mignoli, Marco; Wold, Magrethe; Lacy, Mark; Birkle, Kurt; Broadhurst, Tom; Brandt, Soen; Lund, Niels (1998-02-13). "Photometry and
Spectroscopy of the GRB 970508 Optical Counterpart".
674:
distances and that they can be detected because they are extremely energetic. The distance measurement and the calculations of the burst's total energy release unequivocally supported the latter theory, effectively ending the debate.
579:
Over the next month, Frail observed that the luminosity of the radio source fluctuated significantly from day to day but increased on average. The fluctuations did not occur simultaneously along all of the observed wavelengths, which
539:
from Earth. Although the redshift of the burst itself had not been determined, the absorbent matter was necessarily located between the burst and the Earth, implying that the burst itself was at least as far away. The absence of
280:
distances and are extremely energetic. Although the possibility of multiple types of GRBs meant that the two theories were not mutually exclusive, the distance measurement unequivocally placed the source of the GRB outside the
1210:
1208:
367:
On
Thursday May 8, 1997, at 21:42 UTC, BeppoSAX's Gamma Ray Burst Monitor registered a gamma-ray burst that lasted approximately 15 seconds. It was also detected by
336:(a series of spacecraft designed to detect nuclear explosions in space). The initial burst is often followed by a longer-lived "afterglow" emitted at longer wavelengths (
211:) with a detected afterglow at other wavelengths, the first to have a direct redshift measurement of the afterglow, and the first to be detected at radio wavelengths.
576:
significantly stronger, and he also detected signals at the 6 and 21 cm wavelengths. This was the first confirmed observation of a radio afterglow of a GRB.
1209:
560: â 1.09. This was the first instance in which scientists were able to measure the redshift of a GRB. Several optical spectra were also obtained at the
441:
1698:
M.; Costa, E.; Nicastro, L.; Palazzi, E.; Frontera, F.; Monaldi, L.; Heise, J. (1998). "Evidence for
Diverse Optical Emission from Gamma-Ray Burst Sources".
385:
Wide Field
Cameras. Within a few hours, the BeppoSAX team localized the burst to an error boxâa small area around the specific position to account for the
272:
Until this burst, astronomers had not reached a consensus regarding how far away GRBs occur from Earth. Some supported the idea that GRBs occur within the
1371:
Giommi, P.; Muller, J. M.; Piro, L.; Butler, R. C. (1997-06-19). "Discovery of an X-ray afterglow associated with the Îł-ray burst of 28 February 1997".
708:
3162:
1515:
1254:
581:
596:(rapid variations in the radio luminosity of an object) occur only when the source has an apparent diameter of less than 3 microarcseconds.
699:
slope over about 100 days. The afterglow eventually disappeared, revealing the burst's host, an actively star-forming dwarf galaxy with an
465:
258:
670:, concluding that the bursts are visibly faint because they are not highly energetic. Others concluded that GRBs occur in other galaxies at
469:
1418:
Djorgovski, S. G.; Metzger, M. R.; Odewahn, S. C.; Gal, R. R.; Kulkarni, S. R.; Pahre, M. A.; Frail, D. A.; Costa, E.; Feroci, M. (1997).
627:
of the objectâa logarithmic measure of its brightness with a higher number indicating a fainter objectâwas 20.3 ± 0.3 in the
1956:
Waxman, E.; Kulkarni, S. R.; Frail, D. A. (1998-04-10). "Implications of the Radio
Afterglow from the Gamma-Ray Burst of 1997 May 8".
1635:
Metzger, M. R.; Djorgovski, S. G.; Kulkarni, S. R.; Steidel, C. C.; Adelberger, K. L.; Frail, D. A.; Costa, E.; Frontera, F. (1997b).
695:
The afterglow of GRB 970508 reached a peak total luminosity 19.82 days after the burst was detected. It then faded with a
2024:
3157:
535: = 0.8349 ± 0.0002, indicating that light from the burst had been absorbed by matter roughly 6 billion
1946:
1927:
1587:
425:
2044:
1456:; Frontera, F.; Kouveliotou, C.; MacChetto, D.; Palazzi, E.; Pedersen, H.; Tavani, M.; Van Paradijs, J. (2000-12-20).
658:
Prior to this burst, astronomers had not reached consensus regarding how far away GRBs occur from Earth. Although the
1810:
1802:
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1679:
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456:
observatory, conducted a more extensive analysis of the data, but was also unable to identify any new light sources.
276:, but are visibly faint because they are not highly energetic. Others concluded that GRBs occur in other galaxies at
723: = 0.83, suggesting that, unlike previously observed bursts, GRB 970508 may have been associated with an
2049:
2033:
635:
378:
1616:
Metzger, M. R.; Djorgovski, S. G.; Steidel, C. C.; Kulkarni, S. R.; Adelberger, K. L.; Frail, D. A. (1997).
452:, but he found no new sources of light within the error box. Mark Metzger, a colleague of Djorgovski at the
440:, less than four hours after the discovery. While preparing for his observations Frail contacted astronomer
3177:
3023:
2017:
1452:
Fruchter, A. S.; Pian, E.; Gibbons, R.; Thorsett, S. E.; Ferguson, H.; Petro, L.; Sahu, K. C.; Livio, M.;
177:
3077:
485:
2304:
1867:
Rhoads, James E. (1999-03-25). "The Dynamics and Light Curves of Beamed Gamma Ray Burst Afterglows".
1244:
329:
223:
1457:
3167:
2679:
736:
417:
1637:"Spectral constraints on the redshift of the optical counterpart to the Îł-ray burst of 8 May 1997"
79:
46:
3172:
3066:
2010:
1597:
Kouveliotou, C.; Briggs, M. S.; Preece, R.; Fishman, G. J.; Meegan, C. A.; Harmon, B. A. (1997).
724:
488:
on May 9. They were also unable to find any light sources which had faded during that time.
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31:
Image of the optical afterglow of GRB 970508 taken one month after the burst was detected
1979:
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published his discovery, which was later confirmed to be the burst's optical afterglow.
3127:
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1991:
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scintillation ended, Frail calculated that the radio source had expanded at almost the
671:
628:
624:
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277:
137:
448:. Djorgovski immediately compared his images of the region with older images from the
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572:) and 3,500â8,000 Ă
(350â800 nm), but no emission lines were identified.
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477:
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2002:
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afterglow. By analyzing the fluctuating strength of the radio signals, astronomer
226:, and often followed by a longer-lived "afterglow" emitted at longer wavelengths (
3005:
604:
BeppoSAX's Gamma-Ray Burst Monitor, operating in the energy range of 40â700
504:
333:
289:
250:
249:
GRB 970508 was detected by the Gamma Ray Burst Monitor on the ItalianâDutch
200:
88:
40:
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expanding fireball, this was the first strong evidence to support such a model.
2992:
680:
481:
445:
297:
73:
650:
3151:
2694:
1253:
Bloom, J. S.; Djorgovski, S. G.; Kulkarni, S. R.; Frail, D. A. (1998-11-01).
666:, some astronomers supported the idea that they occur within the Milky Way's
605:
565:
461:
235:
68:
588:
explained as being the result of the radio waves being bent by interstellar
503:
On the night between May 10 and May 11, 1997, Metzger's colleague
381:. The burst also occurred within the field of view of one of BeppoSAX's two
3103:
2778:
1937:
Varendoff, Martin (2001). "Gamma-Ray Bursts". In Volken Schönfelder (ed.).
1799:
Supernovae and Gamma-Ray Bursts: The Greatest Explosions Since the Big Bang
1676:
Supernovae and Gamma-Ray Bursts: The Greatest Explosions Since the Big Bang
1228:
was created from a revision of this article dated 3 February 2010
401:
1362:
715:
of 0.70 ± 0.07. The redshift of GRB 970508's optical afterglow,
2964:
2750:
2704:
2689:
1970:
1881:
1834:
1760:
1712:
1535:
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calculated that the source of the radio waves had expanded almost at the
243:
231:
100:
377:, and by the Burst and Transient Source Experiment (BATSE) on board the
186:
2745:
2740:
2699:
2684:
639:
536:
433:
421:
410:
357:
356:). The first GRB afterglow to be discovered was the X-ray afterglow of
321:
293:
269:; this was the first measurement of the distance to a gamma-ray burst.
262:
215:
208:
1458:"Hubble Space Telescope Observations of the Host Galaxy of GRB 970508"
515:. He then sent the data to Metzger, who after identifying a system of
261:
determined that GRB 970508 occurred at least 6 billion
3046:
3041:
3031:
2873:
2732:
2645:
2640:
2635:
2630:
2625:
2620:
2367:
707: = 25.4 ± 0.15. The galaxy was well fitted by an
696:
663:
617:
593:
569:
520:
473:
390:
325:
282:
273:
219:
218:
flash associated with an explosion in a distant galaxy and producing
683:. While various existing models already encompassed the notion of a
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2786:
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2565:
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2515:
2510:
2505:
2500:
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2485:
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2455:
2450:
2445:
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2430:
2425:
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2415:
2410:
2405:
2400:
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1987:
1898:
1851:
1777:
1729:
1552:
1491:
1291:
659:
528:
508:
361:
349:
254:
239:
122:
1661:
1636:
1402:
662:
of bursts suggested that they do not occur within the disk of the
364:, an ItalianâDutch satellite originally designed to study X-rays.
2974:
1440:(Press release). National Radio Astronomy Observatory. 1997-05-15
609:
453:
345:
1820:
Reichart, Daniel E. (1998-02-19). "The Redshift of GRB 970508".
1670:
PaczyĆski, Bohdan (1999). M. Livio; N. Panagia; K. Sahu (eds.).
2959:
2954:
2836:
2804:
173:
1438:"Very Large Array Detects Radio Emission From Gamma-Ray Burst"
719: = 0.835, agreed with the host galaxy's redshift of
2760:
2755:
638:, analyzed the burst and determined that it was not strongly
382:
353:
337:
266:
227:
155:
2714:
2709:
2059:
524:
312:
3098:
1918:
Flash! The hunt for the biggest explosions in the universe
1793:
Piran, Tsvi (1999). M. Livio; N. Panagia; K. Sahu (eds.).
288:
GRB 970508 was also the first burst with an observed
613:
437:
416:
After a rough position of the burst had been determined,
389:
in the positionâwith a diameter of approximately 10
374:
204:
151:
59:
207:; it is historically important as the second GRB (after
26:
654:
Image of GRB 970508's host galaxy taken in August 1998
3075:
645:
544:
features in the spectra constrained the redshift to
2032:
3022:
1915:
1575:
1268:(1). California Institute of technology: L25âL28.
840:
838:
548: †2.3, while further investigation by
3149:
1746:Optical Transient Associated with GRB 970508".
924:
922:
835:
2991:
938:
936:
612:of (1.85 ± 0.3) à 10
373:, a robotic space probe designed to study the
300:. This provided strong evidence that GRBs are
2018:
203:(GRB) detected on May 8, 1997, at 21:42
2777:
919:
754:
752:
1163:
1161:
1159:
1157:
933:
2025:
2011:
1034:
1032:
420:of the BeppoSAX team contacted astronomer
332:. GRBs were first detected in 1967 by the
78:
45:
25:
2731:
1969:
1922:. Cambridge: Cambridge University Press.
1880:
1833:
1759:
1711:
1660:
1534:
1473:
1384:
1273:
1060:
1058:
1019:
1017:
1015:
1013:
1001:
999:
997:
749:
564:at wavelength ranges of 4,300â7,100
105:+79° 16′ 19.6″
1236:, and does not reflect subsequent edits.
1219:
1154:
871:
869:
867:
649:
400:
316:Artist's conception of BeppoSAX in orbit
311:
3163:Astronomical objects discovered in 1997
1315:"IAU Circular 6654: 1997cm; GRB 970508"
1029:
897:
895:
854:
852:
814:
812:
623:About 5 hours after the burst the
432:. Frail began making observations at a
16:Gamma-ray burst detected on May 8, 1997
3150:
2803:
1828:(2). University of Chicago: L99âL101.
1097:
1095:
1055:
1010:
994:
634:James E. Rhoads, an astronomer at the
2006:
864:
436:of 20 centimeters at 01:30
892:
849:
809:
426:National Radio Astronomy Observatory
320:A gamma-ray burst (GRB) is a highly
2045:Camelopardalis in Chinese astronomy
1092:
13:
1672:Gamma-Ray BurstâSupernova relation
1206:
599:
14:
3189:
1803:Space Telescope Science Institute
1680:Space Telescope Science Institute
1615:
1516:"Optical Follow-Up of GRB 970508"
928:
646:Distance scale and emission model
498:Space Telescope Science Institute
285:, effectively ending the debate.
3133:
3121:
3109:
3097:
3085:
3062:
3061:
1634:
1622:International Astronomical Union
1603:International Astronomical Union
1596:
1424:International Astronomical Union
1319:International Astronomical Union
1218:
942:
844:
472:, members of a research team in
172:
2050:List of stars in Camelopardalis
2034:Constellation of Camelopardalis
1618:"IAU Circular 6655: GRB 970508"
1599:"IAU Circular 6660: GRB 970508"
1420:"IAU Circular 6655: GRB 970508"
1417:
1255:"The Host Galaxy of GRB 970508"
1172:
1142:
1130:
1119:
1107:
1081:
1070:
1044:
983:
971:
959:
947:
907:
881:
758:
480:, compared images taken by the
464:rather than the GRB afterglow.
396:
3158:Long-duration gamma-ray bursts
1941:. Springer. pp. 367â396.
1936:
1913:
1136:
1113:
1064:
1023:
977:
913:
901:
875:
858:
824:
818:
798:
792:
786:
775:
769:
763:
690:
636:Kitt Peak National Observatory
511:of the variable object at the
214:A gamma-ray burst is a highly
1:
1822:Astrophysical Journal Letters
1819:
1696:
1451:
1355:10.1126/science.279.5353.1011
1187:
1167:
989:
804:
379:Compton Gamma Ray Observatory
222:, the most energetic form of
2813:IC 3568 (Lemon Slice Nebula)
328:âthe most energetic form of
307:
7:
1955:
1866:
1582:. Oxford University Press.
1512:
1331:
1125:
1087:
1076:
1005:
730:
444:, who was working with the
10:
3194:
1939:The Universe in Gamma Rays
1914:Schilling, Govert (2002).
1792:
1574:Katz, Jonathan I. (2002).
1369:
1252:
1178:
1148:
781:
616:/cm (1.85 ± 0.3
486:William Herschel Telescope
113:6,000,000,000 ly (1.8
3059:
3018:
2987:
2947:
2844:
2835:
2799:
2773:
2727:
2672:
2654:
2391:
2303:
2095:
2067:
2058:
2040:
1869:The Astrophysical Journal
1748:The Astrophysical Journal
1744:
1700:The Astrophysical Journal
1573:
1523:The Astrophysical Journal
1462:The Astrophysical Journal
1436:
1312:
1262:The Astrophysical Journal
1050:
1038:
965:
953:
887:
830:
330:electromagnetic radiation
224:electromagnetic radiation
183:
170:
162:
146:
135:
121:
109:
99:
87:
67:
54:
36:
24:
1669:
1101:
742:
737:List of gamma-ray bursts
556:suggested a redshift of
360:, which was detected by
178:Related media on Commons
2680:2MASS J05325346+8246465
725:active galactic nucleus
592:in the Milky Way. Such
492:object. On May 10
1214:
1194:Listen to this article
660:isotropic distribution
655:
562:Calar Alto Observatory
513:W. M. Keck Observatory
484:on May 8 and the
413:
317:
304:expanding explosions.
1958:Astrophysical Journal
1213:
653:
554:University of Chicago
404:
315:
1313:Bond, H. E. (1997).
1245:More spoken articles
594:radio scintillations
586:Princeton University
450:Digitized Sky Survey
442:Stanislav Djorgovski
3178:Astronomical events
3024:Astronomical events
1980:1998ApJ...497..288W
1891:1999ApJ...525..737R
1844:1998ApJ...495L..99R
1770:1998ApJ...492L.103P
1722:1998ApJ...496..311P
1653:1997Natur.387..878M
1545:1998ApJ...497L..13G
1484:2000ApJ...545..664F
1395:1997Natur.387..783C
1347:1998Sci...279.1011C
1341:(5353): 1011â1014.
1284:1998ApJ...507L..25B
147:Total energy output
21:
1805:. pp. 17â35.
1215:
1006:Castro-Tirado 1998
701:apparent magnitude
656:
625:apparent magnitude
550:Daniel E. Reichart
542:Lyman-alpha forest
414:
318:
163:Other designations
154:(5 Ă 10
138:apparent magnitude
19:
3073:
3072:
3055:
3054:
3014:
3013:
3001:MACS J0647.7+7015
2983:
2982:
2831:
2830:
2795:
2794:
2769:
2768:
2723:
2722:
1948:978-3-540-67874-8
1929:978-0-521-80053-2
1647:(6636): 878â880.
1589:978-0-19-514570-0
1578:The Biggest Bangs
1379:(6635): 783â785.
1211:
194:
193:
150:5 Ă 10
3185:
3138:
3137:
3136:
3126:
3125:
3124:
3114:
3113:
3112:
3102:
3101:
3090:
3089:
3088:
3081:
3065:
3064:
3020:
3019:
2989:
2988:
2842:
2841:
2801:
2800:
2775:
2774:
2729:
2728:
2065:
2064:
2027:
2020:
2013:
2004:
2003:
1999:
1973:
1971:astro-ph/9709199
1952:
1933:
1921:
1910:
1884:
1882:astro-ph/9903399
1863:
1837:
1835:astro-ph/9712134
1816:
1789:
1763:
1761:astro-ph/9710334
1754:(2): L103âL106.
1741:
1715:
1713:astro-ph/9710322
1693:
1682:. pp. 1â8.
1666:
1664:
1631:
1629:
1628:
1612:
1610:
1609:
1593:
1581:
1570:
1568:
1567:
1538:
1536:astro-ph/9802160
1520:
1509:
1507:
1506:
1477:
1475:astro-ph/9903236
1448:
1446:
1445:
1433:
1431:
1430:
1414:
1388:
1386:astro-ph/9706065
1366:
1328:
1326:
1325:
1309:
1307:
1306:
1277:
1275:astro-ph/9807315
1259:
1235:
1233:
1222:
1221:
1212:
1202:
1200:
1195:
1181:
1176:
1170:
1165:
1152:
1146:
1140:
1134:
1128:
1123:
1117:
1111:
1105:
1099:
1090:
1085:
1079:
1074:
1068:
1062:
1053:
1048:
1042:
1036:
1027:
1021:
1008:
1003:
992:
987:
981:
975:
969:
963:
957:
951:
945:
940:
931:
926:
917:
911:
905:
899:
890:
885:
879:
873:
862:
856:
847:
845:Kouveliotou 1997
842:
833:
828:
822:
816:
807:
802:
796:
790:
784:
779:
773:
767:
761:
756:
709:exponential disk
685:relativistically
519:associated with
517:absorption lines
478:Jan van Paradijs
430:Very Large Array
407:Very Large Array
302:relativistically
187:edit on Wikidata
176:
116:
95:
83:
82:
50:
49:
29:
22:
18:
3193:
3192:
3188:
3187:
3186:
3184:
3183:
3182:
3168:May 1997 events
3148:
3147:
3144:
3134:
3132:
3122:
3120:
3110:
3108:
3096:
3086:
3084:
3076:
3074:
3069:
3051:
3010:
2993:Galaxy clusters
2979:
2943:
2827:
2791:
2765:
2719:
2668:
2650:
2621:4609 (Tonatiuh)
2387:
2299:
2091:
2054:
2036:
2031:
1949:
1930:
1813:
1690:
1626:
1624:
1607:
1605:
1590:
1565:
1563:
1518:
1504:
1502:
1443:
1441:
1428:
1426:
1323:
1321:
1304:
1302:
1257:
1249:
1248:
1237:
1231:
1229:
1226:This audio file
1223:
1216:
1207:
1204:
1198:
1197:
1193:
1190:
1185:
1184:
1177:
1173:
1166:
1155:
1147:
1143:
1135:
1131:
1124:
1120:
1112:
1108:
1100:
1093:
1086:
1082:
1075:
1071:
1063:
1056:
1049:
1045:
1037:
1030:
1022:
1011:
1004:
995:
988:
984:
976:
972:
964:
960:
952:
948:
941:
934:
927:
920:
912:
908:
900:
893:
886:
882:
874:
865:
857:
850:
843:
836:
829:
825:
817:
810:
803:
799:
791:
787:
780:
776:
768:
764:
759:Djorgovski 1997
757:
750:
745:
733:
693:
648:
602:
600:Characteristics
505:Charles Steidel
399:
334:Vela satellites
310:
290:radio frequency
251:X-ray astronomy
201:gamma-ray burst
197:GRB 970508
190:
114:
93:
89:Right ascension
77:
62:
44:
41:Gamma-ray burst
32:
17:
12:
11:
5:
3191:
3181:
3180:
3175:
3173:Camelopardalis
3170:
3165:
3160:
3143:
3142:
3130:
3118:
3106:
3094:
3071:
3070:
3060:
3057:
3056:
3053:
3052:
3050:
3049:
3044:
3039:
3034:
3028:
3026:
3016:
3015:
3012:
3011:
3009:
3008:
3006:MS 0735.6+7421
3003:
2997:
2995:
2985:
2984:
2981:
2980:
2978:
2977:
2972:
2967:
2962:
2957:
2951:
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2936:
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2916:
2911:
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2901:
2896:
2891:
2886:
2881:
2876:
2871:
2866:
2861:
2856:
2850:
2848:
2839:
2833:
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2829:
2828:
2826:
2825:
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2815:
2809:
2807:
2797:
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2792:
2790:
2789:
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2771:
2770:
2767:
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2763:
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2753:
2748:
2743:
2737:
2735:
2725:
2724:
2721:
2720:
2718:
2717:
2712:
2707:
2702:
2697:
2692:
2687:
2682:
2676:
2674:
2670:
2669:
2667:
2666:
2660:
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2652:
2651:
2649:
2648:
2643:
2638:
2633:
2628:
2623:
2618:
2613:
2608:
2603:
2598:
2593:
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2583:
2578:
2573:
2568:
2563:
2558:
2553:
2548:
2543:
2538:
2533:
2528:
2523:
2518:
2513:
2508:
2503:
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2483:
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2463:
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2267:
2262:
2257:
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2237:
2232:
2227:
2222:
2217:
2212:
2207:
2202:
2197:
2192:
2187:
2182:
2177:
2172:
2167:
2162:
2157:
2152:
2147:
2142:
2137:
2132:
2127:
2122:
2117:
2112:
2107:
2101:
2099:
2093:
2092:
2090:
2089:
2084:
2079:
2073:
2071:
2062:
2056:
2055:
2053:
2052:
2047:
2041:
2038:
2037:
2030:
2029:
2022:
2015:
2007:
2001:
2000:
1988:10.1086/305467
1964:(1): 288â293.
1953:
1947:
1934:
1928:
1911:
1899:10.1086/307907
1875:(2): 737â749.
1864:
1852:10.1086/311222
1817:
1811:
1790:
1778:10.1086/311101
1742:
1730:10.1086/305385
1706:(1): 311â315.
1694:
1688:
1667:
1632:
1613:
1594:
1588:
1571:
1553:10.1086/311268
1529:(1): L13âL16.
1510:
1492:10.1086/317870
1468:(2): 664â669.
1449:
1434:
1415:
1367:
1329:
1310:
1292:10.1086/311682
1238:
1224:
1217:
1205:
1192:
1191:
1189:
1186:
1183:
1182:
1171:
1153:
1141:
1137:Schilling 2002
1129:
1118:
1114:Schilling 2002
1106:
1102:PaczyĆski 1999
1091:
1080:
1069:
1065:Schilling 2002
1054:
1043:
1028:
1024:Schilling 2002
1009:
993:
982:
978:Schilling 2002
970:
958:
946:
932:
918:
914:Varendoff 2001
906:
902:Schilling 2002
891:
880:
876:Schilling 2002
863:
859:Schilling 2002
848:
834:
823:
819:Schilling 2002
808:
797:
793:Schilling 2002
785:
774:
770:Schilling 2002
762:
747:
746:
744:
741:
740:
739:
732:
729:
692:
689:
681:speed of light
647:
644:
601:
598:
582:Jeremy Goodman
568:(430â710
482:WIYN Telescope
446:Hale Telescope
398:
395:
309:
306:
298:speed of light
192:
191:
184:
181:
180:
168:
167:
164:
160:
159:
148:
144:
143:
140:
133:
132:
125:
119:
118:
111:
107:
106:
103:
97:
96:
91:
85:
84:
74:Camelopardalis
71:
65:
64:
56:
52:
51:
38:
34:
33:
30:
15:
9:
6:
4:
3:
2:
3190:
3179:
3176:
3174:
3171:
3169:
3166:
3164:
3161:
3159:
3156:
3155:
3153:
3146:
3141:
3131:
3129:
3119:
3117:
3107:
3105:
3100:
3095:
3093:
3083:
3082:
3079:
3068:
3058:
3048:
3045:
3043:
3040:
3038:
3035:
3033:
3030:
3029:
3027:
3025:
3021:
3017:
3007:
3004:
3002:
2999:
2998:
2996:
2994:
2990:
2986:
2976:
2973:
2971:
2968:
2966:
2963:
2961:
2958:
2956:
2953:
2952:
2950:
2946:
2940:
2937:
2935:
2932:
2930:
2927:
2925:
2922:
2920:
2917:
2915:
2912:
2910:
2907:
2905:
2902:
2900:
2897:
2895:
2892:
2890:
2887:
2885:
2882:
2880:
2877:
2875:
2872:
2870:
2867:
2865:
2862:
2860:
2857:
2855:
2852:
2851:
2849:
2847:
2843:
2840:
2838:
2834:
2824:
2821:
2819:
2816:
2814:
2811:
2810:
2808:
2806:
2802:
2798:
2788:
2785:
2784:
2782:
2780:
2779:Star clusters
2776:
2772:
2762:
2759:
2757:
2754:
2752:
2749:
2747:
2744:
2742:
2739:
2738:
2736:
2734:
2730:
2726:
2716:
2713:
2711:
2708:
2706:
2703:
2701:
2698:
2696:
2693:
2691:
2688:
2686:
2683:
2681:
2678:
2677:
2675:
2671:
2665:
2662:
2661:
2659:
2657:
2653:
2647:
2644:
2642:
2639:
2637:
2634:
2632:
2629:
2627:
2624:
2622:
2619:
2617:
2614:
2612:
2609:
2607:
2604:
2602:
2599:
2597:
2594:
2592:
2589:
2587:
2584:
2582:
2579:
2577:
2574:
2572:
2569:
2567:
2564:
2562:
2559:
2557:
2554:
2552:
2549:
2547:
2544:
2542:
2539:
2537:
2534:
2532:
2529:
2527:
2524:
2522:
2519:
2517:
2514:
2512:
2509:
2507:
2504:
2502:
2499:
2497:
2494:
2492:
2489:
2487:
2484:
2482:
2479:
2477:
2474:
2472:
2469:
2467:
2464:
2462:
2459:
2457:
2454:
2452:
2449:
2447:
2444:
2442:
2439:
2437:
2434:
2432:
2429:
2427:
2424:
2422:
2419:
2417:
2414:
2412:
2409:
2407:
2404:
2402:
2399:
2398:
2396:
2394:
2390:
2384:
2381:
2379:
2376:
2374:
2371:
2369:
2366:
2364:
2361:
2359:
2356:
2354:
2351:
2349:
2346:
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2339:
2336:
2334:
2331:
2329:
2326:
2324:
2321:
2319:
2316:
2314:
2311:
2310:
2308:
2306:
2302:
2296:
2293:
2291:
2288:
2286:
2283:
2281:
2278:
2276:
2273:
2271:
2268:
2266:
2263:
2261:
2258:
2256:
2253:
2251:
2248:
2246:
2243:
2241:
2238:
2236:
2233:
2231:
2228:
2226:
2223:
2221:
2218:
2216:
2213:
2211:
2208:
2206:
2203:
2201:
2198:
2196:
2193:
2191:
2188:
2186:
2183:
2181:
2178:
2176:
2173:
2171:
2168:
2166:
2163:
2161:
2158:
2156:
2153:
2151:
2148:
2146:
2143:
2141:
2138:
2136:
2133:
2131:
2128:
2126:
2123:
2121:
2118:
2116:
2113:
2111:
2108:
2106:
2103:
2102:
2100:
2098:
2094:
2088:
2085:
2083:
2080:
2078:
2075:
2074:
2072:
2070:
2066:
2063:
2061:
2057:
2051:
2048:
2046:
2043:
2042:
2039:
2035:
2028:
2023:
2021:
2016:
2014:
2009:
2008:
2005:
1997:
1993:
1989:
1985:
1981:
1977:
1972:
1967:
1963:
1959:
1954:
1950:
1944:
1940:
1935:
1931:
1925:
1920:
1919:
1912:
1908:
1904:
1900:
1896:
1892:
1888:
1883:
1878:
1874:
1870:
1865:
1861:
1857:
1853:
1849:
1845:
1841:
1836:
1831:
1827:
1823:
1818:
1814:
1812:0-521-79141-3
1808:
1804:
1800:
1796:
1791:
1787:
1783:
1779:
1775:
1771:
1767:
1762:
1757:
1753:
1749:
1743:
1739:
1735:
1731:
1727:
1723:
1719:
1714:
1709:
1705:
1701:
1695:
1691:
1689:0-521-79141-3
1685:
1681:
1677:
1673:
1668:
1663:
1662:10.1038/43132
1658:
1654:
1650:
1646:
1642:
1638:
1633:
1623:
1619:
1614:
1604:
1600:
1595:
1591:
1585:
1580:
1579:
1572:
1562:
1558:
1554:
1550:
1546:
1542:
1537:
1532:
1528:
1524:
1517:
1511:
1501:
1497:
1493:
1489:
1485:
1481:
1476:
1471:
1467:
1463:
1459:
1455:
1450:
1439:
1435:
1425:
1421:
1416:
1412:
1408:
1404:
1403:10.1038/42885
1400:
1396:
1392:
1387:
1382:
1378:
1374:
1368:
1364:
1360:
1356:
1352:
1348:
1344:
1340:
1336:
1330:
1320:
1316:
1311:
1301:
1297:
1293:
1289:
1285:
1281:
1276:
1271:
1267:
1263:
1256:
1251:
1250:
1246:
1242:
1227:
1180:
1175:
1169:
1168:Fruchter 2000
1164:
1162:
1160:
1158:
1150:
1145:
1138:
1133:
1127:
1122:
1115:
1110:
1103:
1098:
1096:
1089:
1084:
1078:
1073:
1066:
1061:
1059:
1052:
1047:
1040:
1035:
1033:
1025:
1020:
1018:
1016:
1014:
1007:
1002:
1000:
998:
991:
990:Reichart 1998
986:
979:
974:
967:
962:
955:
950:
944:
943:Metzger 1997b
939:
937:
930:
929:Metzger 1997a
925:
923:
915:
910:
904:, pp. 121â123
903:
898:
896:
889:
884:
878:, pp. 118â120
877:
872:
870:
868:
861:, pp. 116â117
860:
855:
853:
846:
841:
839:
832:
827:
821:, pp. 115â116
820:
815:
813:
806:
805:Pedersen 1997
801:
794:
789:
783:
778:
771:
766:
760:
755:
753:
748:
738:
735:
734:
728:
726:
722:
718:
714:
710:
706:
702:
698:
688:
686:
682:
676:
673:
669:
665:
661:
652:
643:
641:
637:
632:
630:
626:
621:
619:
615:
611:
608:, recorded a
607:
597:
595:
591:
587:
583:
577:
573:
571:
567:
563:
559:
555:
551:
547:
543:
538:
534:
530:
527:determined a
526:
522:
518:
514:
510:
507:recorded the
506:
501:
499:
495:
489:
487:
483:
479:
475:
471:
467:
463:
462:variable star
457:
455:
451:
447:
443:
439:
435:
431:
427:
423:
419:
412:
408:
403:
394:
392:
388:
384:
380:
376:
372:
371:
365:
363:
359:
355:
351:
347:
343:
339:
335:
331:
327:
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466:Titus Galama
458:
418:Enrico Costa
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397:Observations
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278:cosmological
271:
259:Mark Metzger
248:
213:
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128:
3128:Outer space
3116:Spaceflight
2965:MACS0647-JD
2751:HD 104985 b
2705:Struve 1694
2690:NGC 2363-V1
2526:1636 (Mago)
1454:Caraveo, P.
1126:Waxman 1998
1088:Rhoads 1999
1077:Galama 1998
795:, pp. 58â60
772:, pp. 12â16
713:ellipticity
691:Host galaxy
537:light-years
494:Howard Bond
342:ultraviolet
263:light years
232:ultraviolet
117:10 pc)
101:Declination
63:May 8, 1997
58:21:24
3152:Categories
3037:GRB 970508
2746:HD 33564 b
2741:HD 32518 b
2733:Exoplanets
2700:Stein 2051
2685:Gliese 445
1627:2011-07-05
1608:2011-07-05
1566:2009-04-04
1505:2009-04-01
1444:2009-04-04
1429:2011-07-05
1324:2011-07-05
1305:2009-03-15
1241:Audio help
1232:2010-02-03
1188:References
1179:Bloom 1998
1149:Piran 1999
782:Costa 1997
470:Paul Groot
434:wavelength
422:Dale Frail
411:New Mexico
391:arcminutes
358:GRB 970228
326:gamma rays
294:Dale Frail
253:satellite
220:gamma rays
209:GRB 970228
166:GRB 970508
37:Event type
20:GRB 970508
3092:Astronomy
3047:SN 2010lt
3042:SN 2004dj
3032:SN 1996ah
2097:Flamsteed
1996:119438251
1860:119394440
1795:Fireballs
1561:118998539
1051:NRAO 1997
1039:Katz 2002
966:Katz 2002
954:Katz 2002
888:Bond 1997
831:Pian 1998
697:power law
664:Milky Way
521:magnesium
474:Amsterdam
324:flash of
308:Discovery
283:Milky Way
274:Milky Way
3067:Category
2970:UGC 3730
2837:Galaxies
2823:NGC 2404
2818:NGC 1501
2787:NGC 1502
2305:Variable
1907:15557456
1786:16143935
1738:16614555
1500:14856861
1300:18107687
1243: ·
1139:, p. 126
1116:, p. 123
1067:, p. 125
1041:, p. 147
1026:, p. 124
980:, p. 120
968:, p. 149
956:, p. 148
916:, p. 383
731:See also
711:with an
529:redshift
509:spectrum
362:BeppoSAX
350:infrared
322:luminous
255:BeppoSAX
240:infrared
216:luminous
127:0.835 â€
123:Redshift
110:Distance
94:06 53 49
3078:Portals
2975:UGCA 86
2805:Nebulae
1976:Bibcode
1887:Bibcode
1840:Bibcode
1766:Bibcode
1718:Bibcode
1649:Bibcode
1541:Bibcode
1480:Bibcode
1411:4260635
1391:Bibcode
1363:9461429
1343:Bibcode
1335:Science
1280:Bibcode
1230: (
1201:minutes
1151:, p. 23
610:fluence
552:of the
496:of the
476:led by
454:Caltech
424:at the
370:Ulysses
346:optical
236:optical
2960:IC 342
2955:DDO 44
1994:
1945:
1926:
1905:
1858:
1809:
1784:
1736:
1686:
1641:Nature
1586:
1559:
1498:
1409:
1373:Nature
1361:
1298:
1104:, p. 2
640:beamed
629:U-band
590:plasma
352:, and
242:, and
199:was a
171:
76:
43:
3104:Stars
2948:Other
2874:1573A
2761:XO-6b
2756:XO-3b
2673:Other
2664:35759
2069:Bayer
2060:Stars
1992:S2CID
1966:arXiv
1903:S2CID
1877:arXiv
1856:S2CID
1830:arXiv
1782:S2CID
1756:arXiv
1734:S2CID
1708:arXiv
1557:S2CID
1531:arXiv
1519:(PDF)
1496:S2CID
1470:arXiv
1407:S2CID
1381:arXiv
1296:S2CID
1270:arXiv
1258:(PDF)
743:Notes
387:error
383:X-ray
354:radio
338:X-ray
267:Earth
265:from
244:radio
228:X-ray
185:[
136:Peak
131:†2.3
2939:5640
2934:2748
2929:2715
2924:2655
2919:2523
2914:2460
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2879:1961
2869:1573
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2859:1560
2854:1530
2715:XO-6
2710:XO-3
2646:5203
2641:5091
2636:5009
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1943:ISBN
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1584:ISBN
1359:PMID
668:halo
525:iron
523:and
468:and
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142:19.6
55:Date
2846:NGC
2401:967
1984:doi
1962:497
1895:doi
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703:of
614:erg
606:keV
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438:UTC
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