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Astron. Astrophys. Suppl. Ser. 138, 449-450

Optical observations of GRB afterglows: GRB 970508 and
GRB 980326 revisited[*][*]

A.J. Castro-Tirado1,2 - J. Gorosabel1

Send offprint request: J. Gorosabel (

1 - Laboratorio de Astrofísica Espacial y Física Fundamental (LAEFF-INTA), P.O. Box 50727, E-28080 Madrid, Spain
2 - Instituto de Astrofísica de Andalucía (IAA-CSIC), P.O. Box 03004, E-18080 Granada, Spain

Received January 21; accepted March 17, 1999


Since January 1997, we have monitored 15 GRB fields, detecting 6 optical/IR afterglows. We have revisited GRB 970508 and GRB 980326. For GRB 970508, we derive a power-law decay exponent $\alpha=-1.19$ (R-band). The luminosity of the host galaxy L relative to the characteristic luminosity $L^{\star}$ is in the range 0.06-0.15, i.e. a dwarf galaxy. For GRB 980326, we derive a power-law decay exponent $\alpha=-1.7$, taking into account the new upper limit for the host as $R \geq 27.3$ provided by Bloom & Kulkarni (1998). This implies one of the fastest GRB optical decays ever measured. The fact that only about 50% of optical transients have been found within the $\gamma$/X-ray error boxes, suggest that either considerable intrinsic absorption is present or that some optical transients display a very fast decline. We also propose that the "secondary maximum" detected on 17 Apr. 1998 could be explained in the context of the "SN-like" light curves 2-3 weeks after the GRB, as recently suggested by Woosley (1999).

Key words: methods: observational -- gamma-rays: bursts

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