Shock-accelerated fluxes of protons (solid blue line) and electrons (solid red line), secondary electron flux (long-dashed green line), interstellar electron flux (short-dashed magenta line), and Maxwellian distribution of thermal protons (dash-dotted black line) as function of energy. The solid red circle shows the energy E^* where synchrotron losses cause a break in the flux slope. The cyan-, black-, and yellow-shaded areas show the electron energy ranges mostly contributing to synchrotron emission for B  =  1 mG and frequency ranges of GMRT, SKA, and VLA telescopes, respectively (see Eq. (24)). Dotted lines show the non-relativistic part of the electron fluxes.