  Neutrinos from a future Galactic supernova will be detected by several large
underground detectors, in particular by SuperKamiokande (SK) and the Sudbury
Neutrino Observatory (SNO). If, as expected, the $\nu_{\mu}$ and $\nu_{\tau}$
neutrinos have somewhat higher energy on average that the electron neutrinos,
they will dominate the neutral current response. The ways to separate the
neutral and charged current signals will be discussed, and the best strategy to
measure the possible time delay of the neutral current events will be outlined.
Given the expected count rates, one will be able to measure in this way the
$\nu_{\tau}$ mass down to about 30 eV in SNO and to 50 eV in SuperKamiokande.
  Another application to be discussed is the supernova localization by the
neutrino signal, prior to or independently of the electromagnetic signal. The
accuracy with which this can be accomplished using the angular distributions of
the reactions will be estimated. With two or more detectors one can, in
principle, attempt triangulation based on the arrival time of the neutrinos. It
will be argued that for realistic parameters this method will be very difficult
and likely leads only to crude localization.
