New constraints on the gamma-ray and high energy neutrino fluxes from the circumstellar interaction of SN 2023ixf. (arXiv:2307.08744v1 [astro-ph.HE])

New constraints on the gamma-ray and high energy neutrino fluxes from the circumstellar interaction of SN 2023ixf. (arXiv:2307.08744v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sarmah_P/0/1/0/all/0/1">Prantik Sarmah</a>

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 $7.3times 10^{-2} ~rm GeV~cm^{-2}$. 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.

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 $7.3times 10^{-2} ~rm GeV~cm^{-2}$. 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.

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