HETE-2 localization and observation of the bright, X-Ray Rich Gamma-Ray Burst GRB 021211 (Articolo in rivista)

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  • HETE-2 localization and observation of the bright, X-Ray Rich Gamma-Ray Burst GRB 021211 (Articolo in rivista) (literal)
Anno
  • 2003-01-01T00:00:00+01:00 (literal)
Alternative label
  • Crew, G. B. et al. (2003)
    HETE-2 localization and observation of the bright, X-Ray Rich Gamma-Ray Burst GRB 021211
    (literal)
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  • Crew, G. B. et al. (literal)
Pagina inizio
  • 387 (literal)
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  • La determinazione della locazione di un lampo gamma a meno di 14 minuti d'arco in 22 secondi e' molto difficile da ottenere. HETE-2 distribuisce liberamente l'informazione appena possibile, in modo che tutti gli osservatori interessati possano cercare di individuare ed osservare il dopolampo. (literal)
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  • 599 (literal)
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  • Rivelazione e localizzazione, a meno di 14 arcmin in 22 secondi, da parte del satellite HETE-2, del Lampo Gamma dell'11 Dicembre 2002 e sue caratteristiche spettrali e temporali. Questo evento e' uno dei piu' noti degli ultimi tre anni. E' uno dei soli quattro Lampi Gamma finora sicuramente collegabili con un'esplosione di Supernova e, fra questi, quello a distanza maggiore. La rapidita' della localizzazione ha consentito la rivelazione del transiente ottico (dopolampo), che decade esponenzialmente ed era di tre magnitudini piu' debole degli altri eventi simili. Questo evento e' stato finora citato, in molti casi argomento principale, di quindici articoli su riviste internazionali, tredici preprints su astro-ph e trentuno comunicazioni GCN (GRB Coordinates Network, http://gcn.gsfc.nasa.gov/ (literal)
Note
  • ISI Web of Science (WOS) (literal)
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  • IASF/CNR, Bologna; MIT, Cambridge, Mass; Univ. Chicago, Ill; Univ. California, Berkeley & Santa Cruz, CA; LANL, Los Alamos, NM; NASA/GSFC, Greebelt, MD, USA; CESR/CNRS, Toulouse, France; Tokio Inst. of Technology; RIKEN; National. Astron. Obs.; Tsukuba Space Center; Miyazaki Univ. Japan; Tata Inst. Mumbai, India, INPE, Sao Jose' dos Campos, Brasil. (literal)
Titolo
  • HETE-2 localization and observation of the bright, X-Ray Rich Gamma-Ray Burst GRB 021211 (literal)
Abstract
  • ABSTRACT A bright, X-rayrich gamma-ray burst (GRB) was detected by the French Gamma Telescope (FREGATE) and localized with the Wide Field X-ray Monitor (WXM) and Soft X-ray Camera (SXC) instruments on the High Energy Transient Explorer 2 satellite (HETE-2) at 11:18:34.03 UT (40714.03 SOD) on 2002 December 11. The WXM flight software localized the burst to a 14 radius; this was relayed to the astronomical community 22 s after the start of the burst. Ground analysis of WXM and SXC data provided refined localizations; the latter can be described as a circle with a radius of 2 centered at R.A. 08h09m00s, decl. 06°4420 (J2000.0). GRB 021211 consists of a single, FRED-like pulse with a duration t90 2.3 s at high energies (85400 keV), which increases to t90 8.5 s at low energies (210 keV). The peak photon number and photon energy fluxes in the 2400 keV band are (34.0 ± 1.8) photons cm-2 s-1 and (1.68 ± 0.11) × 10-6 ergs cm-2 s-1, respectively. The energy fluences in the 230 and 30400 keV energy bands are SX = (1.36 ± 0.05) × 10-6 ergs cm-2 and S = (2.17 ± 0.15) × 10-6 ergs cm-2, respectively. Thus, GRB 021211 is an X-rayrich GRB (SX/S = 0.63 > 0.32). The average spectrum of the burst is well fitted by a Band function (low-energy power-law index = -0.805; high-energy power-law index = -2.37; and energy of the peak of the spectrum in F, E = 46.8 keV). The nearreal-time optical follow-up of GRB 021211 made possible by HETE-2 led to the detection of an optical afterglow for what otherwise would quite likely have been classified as an \"optically dark\" GRB, since the optical transient faded rapidly (from R < 14 to R 19) within the first 20 minutes, and was fainter than R 23 within 24 hr after the burst. GRB 021211 demonstrates that some fraction of burst afterglows are optically dark because their optical afterglows at times greater than 1 hr after the burst are very faint, and previously have often escaped detection. Such bursts are \"optically dim\" rather than truly optically dark. GRB 021211 also shows that even such optically dim bursts can have very bright optical afterglows at times less than 20 minutes after the burst. Subject heading: gamma rays: bursts On-line material: color figures (literal)
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