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A supernova event in our own galaxy will result in a large number ofneutrinos detected on Earth within the time-frame of a few seconds. Theseneutrinos will have been produced thermally with, in principle, three distincttemperatures for the electron, anti-electron and remaining heavy flavoursrespectively. We revisit the possibility that new MeV-mass particles $\chi$ arealso produced thermally during the event, which scatter with the neutrinos andalter their temperatures. Our main emphasis is on the detectability of thiseffect using the neutrino spectrum, given the large uncertainty on thetemperature and density profiles of the stellar matter. By marginalising overthe parameters of a simple analytic model for the stellar profile, we find thatSuper Kamiokande could place an upper limit on the scattering cross section atthe level of $\sigma_{\chi \nu} \sim 10^{-40} \cdot (T / \mathrm{MeV})^2$cm$^2$ for 10 MeV mass particles at 90% confidence. A direct-detection-likeexperiment would be less susceptible to systematic uncertainties in theneutrino production and mixing, but this would need a target mass around 100tonnes in order to acquire enough statistics to compete with Super Kamiokande.

How well can new particles interacting with neutrinos be constrained after a galactic supernova?