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The recent supernova, SN 2023ixf, one of the closest observed type II SNe hasrevealed the presence of a dense circumstellar material (CSM). Interaction ofthe SN ejecta with this dense CSM may create high energy protons of PeVenergies through shock acceleration. These accelerated protons then collidingwith the CSM (inelastic $pp$ collision) can produce secondaries such as highenergy gamma-rays and neutrinos. However, no gamma-rays and neutrinos have beendetected by Fermi-LAT and IceCube from this event. Indeed, Fermi-LAT has placedan upper limits on the gamma-ray flux above $100$~MeV to be $2.6 \times10^{-11}~\rm erg~cm^{-2}~s^{-1}$. On the other hand IceCube's upper limit onmuon neutrino flux is $7.3\times 10^{-2} ~\rm GeV~cm^{-2}$. Using theseexperimental constraints and shock-CSM properties derived from observations, weobtain 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 viathe $pp$ interaction channel. While we found the gamma-ray flux to beconsistent 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 detectionprospects of such secondary signals from future SN 2023 like events withupcoming detectors, CTA and IceCube-Gen2 and found to have great discoverypotential, if any event occurs within $7$ Mpc.

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