Submitted to ApJ Sub-PeV Neutrinos from TeV Unidentified Sources in the Galaxy

The IceCube collaboration discovery of 28 high-energy neutrinos over the en-ergy range 30 TeV ∼< εν ∼< 1 PeV, a 4.3σ excess over expected backgrounds, rep-resents the first high-confidence detection of cosmic neutrinos at these energies. In light of this discovery, we explore the possibility that some of the Sub-PeV cosmic neutrinos might originate in our Galaxy’s TeV unidentified (TeV UnID) sources. While typically resolved at TeV energies, these sources lack promi-nent radio or X-ray counterparts, and so have been considered promising sites for hadron acceleration within our Galaxy. Modeling the TeV UnID sources as Galactic hypernova remnants, we predict Sub-PeV neutrino fluxes and spectra consistent with their contributing a minority of nν ∼< 2 of the observed events. This is consistent with our analysis of the spatial distribution of the Sub-PeV neutrinos and TeV UnID sources, which finds that a best-fit of one, and maxi-mum of 3.8 (at 90%-confidence), of the ≈16 non-atmospheric sub-PeV neutrinos may originate in TeV UnID sources, with the remaining 75 % to 95 % of events being drawn from an isotropic background. If our scenario is correct, we ex-pect excess Sub-PeV neutrinos to accumulate along the Galactic plane, within |` | ∼< 30 ◦ of the Galactic center and in the Cygnus region, as observations by IceCube and other high-energy neutrino facilities go forward. Our scenario also has implications for radio, X-ray, and TeV observations of the TeV UnID sources. Subject headings: neutrinos — gamma rays: general — cosmic rays — ISM: supernova remnant