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We investigate what one can hope to learn about the parameters that describethe neutrino fluxes emitted by the explosion of a galactic supernova using theobservations of a megaton-size Water-Cherenkov detector. We calculate theallowed regions that can be obtained by fitting these parameters to a simulatedobservation of events by such a detector. All four available detection channels(inverse beta decay, charge and neutral current on oxygen and elasticscattering on electrons) are included in the fit and we use a ten dimensionalparameters space. Nine parameters describe the initial neutrino fluxes and arereferred to as the supernova parameters. Furthermore, we include the dependenceon the Chooz mixing angle $\theta_{13}$, which controls the matter effects thatthe neutrino undergoes in the outer-parts of the supernova. If we do not makeany extra assumption on these parameters, we show that one can hope todetermine $\theta_{13}$ quite well whereas, except for the parametersdescribing the $\bar\nu_e$ flux, most of the supernova parameters are ratherdifficult to constrain, even if the four detection channels could be completelyseparated.

Learning more about what can be concluded from the observation of neutrinos from a galactic supernova