1999A&AS..138..449C

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 α=-1.19 (R-band). The luminosity of the host galaxy L relative to the characteristic luminosity L^* is in the range 0.06-0.15, i.e. a dwarf galaxy. For GRB 980326, we derive a power-law decay exponent α=-1.7, taking into account the new upper limit for the host as R≥27.3 provided by Bloom & Kulkarni (1998, GCN, 161). 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 (1999A&AS..138..499W).