Revisiting the contributions of supernova and hypernova remnants to the diffuse high-energy backgrounds: Constraints on very high redshift injection

Di Xiao, Peter Mészáros, Kohta Murase, Zi Gao Dai

Research output: Contribution to journalArticlepeer-review

29 Scopus citations

Abstract

Star-forming and starburst galaxies are considered one of the viable candidate sources of the high-energy cosmic neutrino background detected in IceCube. We revisit contributions of supernova remnants (SNRs) and hypernova remnants (HNRs) in such galaxies to the diffuse high-energy neutrino and gamma-ray backgrounds, in light of the latest Fermi data above 50 GeV. We also take into account possible time-dependent effects of the cosmic-ray (CR) acceleration during the SNR evolution. CRs accelerated by the SNR shocks can produce high-energy neutrinos up to ∼100 TeV energies, but CRs from HNRs can extend the spectrum up to PeV energies. We show that, only if HNRs are dominant over SNRs, the diffuse neutrino background above 100 TeV can be explained without contradicting the gamma-ray data. However, the neutrino data around 30 TeV remain unexplained, which might suggest a different population of gamma-ray dark CR sources. We also consider possible contributions of Pop-III HNRs up to z ≲ 10 and show that they are not constrained by the gamma-ray data and thus could contribute to the diffuse high-energy backgrounds if their explosion energy reaches EPOP-III ∼ a few × 1053 erg. More conservatively, our results suggest that the explosion energy of Pop-III HNRs is EPOP-III ≲ 7 × 1053 erg.

Original languageEnglish (US)
Article number133
JournalAstrophysical Journal
Volume826
Issue number2
DOIs
StatePublished - Aug 1 2016

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Fingerprint Dive into the research topics of 'Revisiting the contributions of supernova and hypernova remnants to the diffuse high-energy backgrounds: Constraints on very high redshift injection'. Together they form a unique fingerprint.

Cite this