Ponente
Descripción
The Milky Way hosts astrophysical accelerators capable of producing high-energy cosmic rays. These cosmic rays can interact with the interstellar medium across the Galaxy to produce neutrinos and gamma rays (propagation component), while their interactions with ambient material at their acceleration sites, such as supernova remnants, can give rise to source component of the gamma-ray and neutrino flux. In this work, we estimate the neutrino flux originating from Galactic sources in the energy range of 1-100 TeV. Using simulated populations of Galactic TeV gamma-ray sources, we exploit the correlation between gamma rays and neutrinos to provide a range for the source contribution to the Galactic neutrino flux. For the upper limit, we used the full Galactic simulated gamma-ray source populations, whereas the lower limit was estimated using the hadronic component of the Galactic supernova remnant population. Finally, we compare our results with the Galactic neutrino emission measured by ANTARES and IceCube, and with the predicted propagation component of the neutrino flux.
