neutrinos and Fermi/LAT [$\gamma$-rays]{} are both produced in interactions of CRs which have a hard spectrum with a power-law index harder than 2.4 and a cut-off above $\sim 10$PeV. This assumes the CRs are interacting with the interstellar medium in the Norma arm and/or in the galactic bar.

The role of isolated SNRs in producing PeV CRs is uncertain. The [$\gamma$-ray]{} spectra from most shell-type galactic SNRs observed by Cherenkov telescopes show a spectral cutoff well below PeV energies [see e.g. @acero15]. While future [*Cherenkov Telescope Array*]{} observations may be needed to confirm these results [see e.g. @fa13], a population of [pevatrons]{} is needed to explain the observed spectrum of galactic CRs at and above the spectral knee region. Supernovae with transrelativistic shocks [@budnik08; @Chakraborti2011] and type IIb supernovae [@ptu10] were proposed to accelerate CRs above PeV energies but the statistics of these potential sources remain to be established. Here, we present a model of a galactic [pevatron]{} which produces hard CR spectra with a high efficiency of conversion of SN kinetic energy into the highest energy CRs. We further argue that this PeV CR source has the properties required to explain a number of the IceCube neutrinos detected from 