  The next supernova in our galaxy will be detected by a variety of neutrino
detectors. In this lecture I discuss the set of observables needed to constrain
the models of supernova neutrino emission. They are the flux normalizations,
and average energies, of each of the three expected components of the neutrino
flux: $\nu_e$, $\bar{\nu}_e$, and $\nu_x$ (all the other four flavors
combined). I show how the existing, or soon to be operational, neutrino
detectors will be able to determine the magnitude of these observables, and
estimate the corresponding rates.
