  The possibility of observing supernova (SN) neutrinos through the process of
coherent elastic neutrino-nucleus scattering (CENNS) in future ton scale
detectors designed primarily for direct detection of dark matter is
investigated. In particular, we focus on the possibility of distinguishing the
various phases of the SN neutrino emission. The neutrino emission rates from
the recent long term Basel/Darmstadt simulations are used to calculate the
expected event rates. The recent state-of-the-art SN simulations predict closer
fluxes among different neutrino flavors and lower average energies compared to
the earlier simulation models. We find that our estimated total event rates are
typically a factor of two lower than those predicted using older simulation
models. We further find that, with optimistic assumptions on the detector's
time resolution (~ 10 ms) and energy threshold (~ 0.1 keV), the neutrinos
associated with the accretion phase of the SN can in principle be demarcated
out with, for example, a 10-ton Xe detector, although distinguishing the
neutrinos associated with the neutronization burst phase of the explosion would
typically require several tens of ton detectors. We also comment on the
possibility of studying the properties of non-electron flavor neutrinos from
the CENNS of SN neutrinos.
