  As the largest mass concentrations in the local Universe, nearby clusters of
galaxies and their central galaxies are prime targets in searching for indirect
signatures of dark matter annihilation (DMA). We seek to constrain the dark
matter annihilation emission component from multi-frequency observations of the
central galaxy of the Virgo cluster. The annihilation emission component is
modeled by the prompt and inverse-Compton gamma rays from the hadronization of
annihilation products from generic weakly interacting dark matter particles.
This component is fitted to the excess of the observed data above the spectral
energy distribution (SED) of the jet in M87, described with a best-fit
synchrotron-self-Compton (SSC) spectrum. While this result is not sufficiently
significant to claim a detection, we emphasize that a dark matter "double hump
signature" can be used to unambiguously discriminate the dark matter emission
component from the variable jet-related emission of M87 in future, more
extended observation campaigns.
