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The possibility of observing supernova (SN) neutrinos through the process ofcoherent elastic neutrino-nucleus scattering (CENNS) in future ton scaledetectors designed primarily for direct detection of dark matter isinvestigated. In particular, we focus on the possibility of distinguishing thevarious phases of the SN neutrino emission. The neutrino emission rates fromthe recent long term Basel/Darmstadt simulations are used to calculate theexpected event rates. The recent state-of-the-art SN simulations predict closerfluxes among different neutrino flavors and lower average energies compared tothe earlier simulation models. We find that our estimated total event rates aretypically a factor of two lower than those predicted using older simulationmodels. We further find that, with optimistic assumptions on the detector'stime resolution (~ 10 ms) and energy threshold (~ 0.1 keV), the neutrinosassociated with the accretion phase of the SN can in principle be demarcatedout with, for example, a 10-ton Xe detector, although distinguishing theneutrinos associated with the neutronization burst phase of the explosion wouldtypically require several tens of ton detectors. We also comment on thepossibility of studying the properties of non-electron flavor neutrinos fromthe CENNS of SN neutrinos.

Observing supernova neutrino light curve in future dark matter detectors