  Neutrinos are guaranteed to be observable from the next galactic supernova
(SN). Optical light and gravitational waves are also observable, but may be
difficult to observe if the location of the SN in the galaxy or the details of
the explosion are unsuitable. The key to observing the next supernova is to
first use neutrinos to understand various physical quantities and then link
them to other signals. In this paper, we present Monte Carlo sampling
calculations of neutrino events from galactic supernova explosions observed
with Super-Kamiokande. The analytical solution of neutrino emission, which
represents the long-term evolution of neutrino-light curve from supernovae, is
used as a theoretical template. It gives the event rate and event spectrum
through inverse beta decay interactions with explicit model parameter
dependence. Parameter estimation is performed on these simulated sample data by
fitting least squares using the analytical solution. The results show that the
mass, radius and total energy of a remnant neutron star produced by a SN can be
determined with an accuracy of $\sim 0.1M_\odot$, $\sim 1$ km, and $\sim
10^{51}$ erg, respectively, for a galactic SN at 8 kpc.
