  The indirect search for dark matter is typically restricted to individual
photon bands and instruments. In the context of multiwavelength observations,
finding a weak signal in large fore- and backgrounds at only one wavelength
band is hampered by systematic uncertainties dominating the signal strength.
Dark matter particle annihilation is producing Standard Model particles of
which the prompt photon emission is searched for in many studies. However, also
the secondary emission of charged particles from dark matter annihilation in
the TeV range results in comparable or even stronger fluxes in the GHz-GeV
range. In this study, we calculate the prompt and secondary emission of a
scotogenic WIMP with a mass of $1\,\mathrm{TeV}$ in 27 dwarf galaxies of the
Milky 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 astrophysical
source. In order to determine the best candidates for multi-instrument
analyses, we estimate the diffuse emission component of the Milky Way itself,
including its own dark matter halo from the same scotogenic WIMP model. We find
signal-to-background ratios of individual sources on the order of
$10^{-3}$-$10^{-2}$ across X- to $\gamma$-rays assuming $J$-factors for the
cold dark matter distribution inferred from observations and no additional
boosting due to small-scale clumping. We argue that a joint multi-wavelength
analysis of all nearby galaxies as well as the extension towards the Cosmic
Gamma-ray Background is required to disentangle possible dark matter signals
from astrophysical back- and foregrounds.
