Techniques for detection of cosmic diffuse neutrinos and anti-neutrinos

We first indicate the energy regions where diffuse neutrinos or anti‐neutrinos are expected. Techniques for the detection of these neutrinos are described. We focus on the prospects for detecting neutrinos or anti‐neutrinos in the window between the atmospheric and solar neutrino flux, from 10–30 MeV. We also describe methods to detect neutrinos in the 100 MeV to GeV region using a lunar neutrino telescope. A brief comment is made concerning the detection of the 1.9° relic neutrinos.