New constraints on the gamma-ray and high energy neutrino fluxes from the circumstellar interaction of SN 2023ixf

Abstract

The recent supernova, SN 2023ixf, one of the closest observed type II SNe has revealed the presence of a dense circumstellar material (CSM). Interaction of the SN ejecta with this dense CSM may create high energy protons of PeV energies through shock acceleration. These accelerated protons then colliding with the CSM (inelastic \(pp\) collision) can produce secondaries such as high energy gamma-rays and neutrinos. However, no gamma-rays and neutrinos have been detected by Fermi-LAT and IceCube from this event. Indeed, Fermi-LAT has placed an upper limits on the gamma-ray flux above \(100\)~MeV to be \(2.6 \times 10^{-11}~\rm erg~cm^{-2}~s^{-1}\). On the other hand IceCube's upper limit on muon neutrino flux is \(7.3\times 10^{-2} ~\rm GeV~cm^{-2}\). Using these experimental constraints and shock-CSM properties derived from observations, we obtain new upper limits on the gamma-ray (\(10^{-11}~\rm erg~cm^{-2}~s^{-1}\)) and neutrino (\(10^{-3}~\rm GeV~cm^{-2}\)) fluxes from SN 2023ixf produced via the \(pp\) interaction channel. While we found the gamma-ray flux to be consistent with Fermi-LAT's upper limit, the neutrino flux is found to be about \(2\) order smaller than the IceCube's upper limit. We further analyse detection prospects of such secondary signals from future SN 2023 like events with upcoming detectors, CTA and IceCube-Gen2 and found to have great discovery potential, if any event occurs within \(7\) Mpc.