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The indirect search for dark matter is typically restricted to individualphoton bands and instruments. In the context of multiwavelength observations,finding a weak signal in large fore- and backgrounds at only one wavelengthband is hampered by systematic uncertainties dominating the signal strength.Dark matter particle annihilation is producing Standard Model particles ofwhich the prompt photon emission is searched for in many studies. However, alsothe secondary emission of charged particles from dark matter annihilation inthe TeV range results in comparable or even stronger fluxes in the GHz-GeVrange. In this study, we calculate the prompt and secondary emission of ascotogenic WIMP with a mass of $1\,\mathrm{TeV}$ in 27 dwarf galaxies of theMilky Way. For the secondary emission, we include Inverse Compton scattering,bremsstrahlung, and synchrotron radiation, which results in a "triple hump"structure characteristic for only dark matter and no other astrophysicalsource. In order to determine the best candidates for multi-instrumentanalyses, we estimate the diffuse emission component of the Milky Way itself,including its own dark matter halo from the same scotogenic WIMP model. We findsignal-to-background ratios of individual sources on the order of$10^{-3}$-$10^{-2}$ across X- to $\gamma$-rays assuming $J$-factors for thecold dark matter distribution inferred from observations and no additionalboosting due to small-scale clumping. We argue that a joint multi-wavelengthanalysis of all nearby galaxies as well as the extension towards the CosmicGamma-ray Background is required to disentangle possible dark matter signalsfrom astrophysical back- and foregrounds.

MHz to TeV expectations from scotogenic WIMP dark matter