We present interplanetary network localization, spectral, and time history information for four short-duration, hard spectrum gamma-ray bursts, GRB 000607, GRB 001025B, GRB 001204, and GRB 010119. All of these events were followed up with sensitive radio and optical observations (the first and only such bursts to be followed up in the radio to date), but no detections were made, demonstrating that the short bursts do not have anomalously intense afterglows. We discuss the upper limits and show that the lack of observable counterparts is consistent with both the hypothesis that the afterglow behavior of the short bursts is like that of the long-duration bursts, many of which similarly have no detectable afterglows, as well as the hypothesis that the short bursts have no detectable afterglows at all. Small number statistics do not allow a clear choice between these alternatives, but given the present detection rates of various missions, we show that progress can be expected in the near future. Partly based on observations collected at ESO, Chile; Large Program 165.H-0464.

Afterglow Upper Limits for Four Short-Duration, Hard Spectrum Gamma-Ray Bursts

FRONTERA, Filippo;GUIDORZI, Cristiano;
2002

Abstract

We present interplanetary network localization, spectral, and time history information for four short-duration, hard spectrum gamma-ray bursts, GRB 000607, GRB 001025B, GRB 001204, and GRB 010119. All of these events were followed up with sensitive radio and optical observations (the first and only such bursts to be followed up in the radio to date), but no detections were made, demonstrating that the short bursts do not have anomalously intense afterglows. We discuss the upper limits and show that the lack of observable counterparts is consistent with both the hypothesis that the afterglow behavior of the short bursts is like that of the long-duration bursts, many of which similarly have no detectable afterglows, as well as the hypothesis that the short bursts have no detectable afterglows at all. Small number statistics do not allow a clear choice between these alternatives, but given the present detection rates of various missions, we show that progress can be expected in the near future. Partly based on observations collected at ESO, Chile; Large Program 165.H-0464.
Hurley, K.; Berger, E.; Castro, Tirado; Castro, Cern; J. M., Cline; T., Feroci; M., Frail; D., A.; Frontera, Filippo; F., Masetti; Guidorzi, Cristiano; C., Montanari; E., Hartmann; D. H., Henden; A., Levine; S. E., Mazets; E., Golenetskii; S., Frederiks; D., Morrison; G., Oksanen; A., Moilanen; M., Park; H. S., Price; P. A., Prochaska; J., Trombka; J., Williams
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11392/1202251
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