Astron. Astrophys. Suppl. Ser.
Volume 138, Number 3, September 1999Gamma-Ray Bursts in the Afterglow Era Contents Rome, November 3-6, 1998
|Page(s)||449 - 450|
|Published online||15 September 1999|
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
Send offprint request to: J. Gorosabel
Accepted: 17 March 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 (R-band). The luminosity of the host galaxy L relative to the characteristic luminosity is in the range 0.06-0.15, i.e. a dwarf galaxy. For GRB 980326, we derive a power-law decay exponent , taking into account the new upper limit for the host as 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 γ/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
Based on observations collected at the German-Spanish Astronomical Centre, Calar Alto, operated by the Max-Planck-Institut für Astronomie, Heidelberg, jointly with the Spanish National Commission for Astronomy.
© European Southern Observatory (ESO), 1999