The rapid follow-up observation provided by the GOYA optical camera (OCAM) will also clarify whether a flashing optical counterpart takes place simultaneously to the GRB. The limiting magnitude for 1-s integration time is V = 14.5 (and V = 20 for t = 1000 s). See figures 3.1 and 3.2. Therefore, GOYA will be able to detect objects as faint as V = 14.5 in 1 s. This is the kind of optical emition predicted when an extrapolation of the gamma-ray spectrum is done into the optical range [70]. In case that no emission will be detected, GOYA will impose severe constraints to many theoretical models. A positive detection, on the other hand, would be a very important step for the resolution of the GRB mystery, not the least because the source position would then be defined to within a few arcseconds, and very deep searches for quiescent counterpart could meaningfully be conducted from the ground, both in the optical/infrared and in the radio regime.