  Core-collapse supernovae are one of the most energetic events in the universe
($10^{46} J$). When a massive star (M $>$ 8 M$_{\odot}$) ignites its last
fusion stage where silicon fusion makes iron, its end is then very close.
Basically, the core of the star falls inwardly and the gravitational energy is
then released in a supernova explosion. The basic picture of this explosion was
confirmed by the few neutrinos detected from the SN1987a supernova at
Kamiokande, IMB and Baksan detectors. However, there are many details that are
still unknown. Since then, a large detector network has grown with better
capabilities. Nowadays, in the case of a supernova explosion in our galaxy, the
information that we would acquire would allow us to learn much more about these
energetic events and constrain our models. Here, I present a brief summary of
this network with special emphasis in SuperK-Gd (the upgraded Super-Kamiokande
detector with efficient neutron tagging).
