Journal
ASTROPHYSICAL JOURNAL
Volume 778, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/778/1/54
Keywords
gamma-ray burst: general; gamma-ray burst: individual (GRB 091024A)
Categories
Funding
- UK Science and Technology Facilities Council
- Royal Society
- Wolfson Foundation
- Sun Microsys-tems, Inc.
- Hewlett-Packard Company
- AutoScope Corporation
- Lick Observatory
- NSF
- University of California
- Sylvia and Jim Katzman Foundation
- TABASGO Foundation
- W. M. Keck Foundation
- Gary and Cynthia Bengier
- Christopher R. Redlich Fund
- Richard and Rhoda Goldman Fund
- NSF [AST-1211916]
- NASA/Swift [NNX10AI21G, NNX12AD73G]
- Science and Technology Facilities Council [ST/J001465/1, ST/K001000/1, ST/I001719/1, PP/E002064/1, ST/I505821/1] Funding Source: researchfish
- STFC [ST/I001719/1, ST/K001000/1, ST/J001465/1, ST/I505821/1, PP/E002064/1] Funding Source: UKRI
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1107973, 1211916] Funding Source: National Science Foundation
- NASA [NNX12AD73G, 53354] Funding Source: Federal RePORTER
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We present a broadband study of gamma-ray burst (GRB) 091024A within the context of other ultra-long-duration GRBs. An unusually long burst detected by Konus-Wind (KW), Swift, and Fermi, GRB 091024A has prompt emission episodes covering similar to 1300 s, accompanied by bright and highly structured optical emission captured by various rapid-response facilities, including the 2 m autonomous robotic Faulkes North and Liverpool Telescopes, KAIT, S-LOTIS, and the Sonoita Research Observatory. We also observed the burst with 8 and 10 m class telescopes and determine the redshift to be z = 1.0924 +/- 0.0004. We find no correlation between the optical and gamma-ray peaks and interpret the optical light curve as being of external origin, caused by the reverse and forward shock of a highly magnetized jet (R-B approximate to 100-200). Low-level emission is detected throughout the near-background quiescent period between the first two emission episodes of the KW data, suggesting continued central-engine activity; we discuss the implications of this ongoing emission and its impact on the afterglow evolution and predictions. We summarize the varied sample of historical GRBs with exceptionally long durations in gamma-rays ( greater than or similar to 1000 s) and discuss the likelihood of these events being from a separate population; we suggest ultra-long GRBs represent the tail of the duration distribution of the long GRB population.
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