This is the main goal of GOYA, as no other single experiment will provide such rapid follow-up observations.
We have mentioned that GRBs will be localized to better than 1 degree by WIFICAM. However only smaller error boxes will allow deep searches.
That is the reason of including a cluster of narrow field-of-view moving telescopes in the payload. In less than 10 s, the GOYA X-ray telescope (XTEL) will point to the 1 degree error box given by WIFICAM, so most of the bursts will be observed while they are still going on. This will make possible to reduce the error box to about 1' after final on-ground processing. For a fraction of bursts (those with -20 < b < +20), the spectra obtained by the X-ray telescope (0.5-10 keV) will allow to derive the value of the H column towards the source. This is an importante indicator of the distance. For instance, if a particular burst arises from the direction of the Galactic Centre, and N(H) is very low, we can conclude that the burster is pretty much closer, about 1-2 kpc. Therefore, we will distinguish whether they are produced in nearby sources or not. In the latter case, we cannot distinguish whether they will be located far in the Galaxy or beyond.