  Observations with the Extreme UltraViolet Explorer (EUVE) satellite have
shown that the inner region of the Virgo cluster (centered in M87 galaxy) has a
strong Extreme UltraViolet (EUV) emission (up to $13^{\prime}$) in excess to
the low-energy tail expected from the hot, diffuse IntraCluster Medium (ICM).
Detailed observations of large scale radio emission and upper limits for hard,
non-thermal X-ray emission in the $2 - 10$ keV energy band have been also
reported. Here we show that all available observations can be accounted for by
the existence of two electron Populations (indicated as I and II) in the M87
Galaxy. The mildly relativistic Population I is responsible for the EUV excess
emission via IC scattering of CBR and starlight photons. Population II
electrons (with higher energy) are instead responsible for the radio emission
through synchrotron mechanism. The same electrons also give rise to hard
non-thermal X-ray emission (via IC scattering of CBR photons), but the
resulting power is always below the upper bounds placed by present
observations. The non-negligible energy budget of the two electron populations
with respect to that associated with thermal electrons indicates that the M87
galaxy is not today in a quiescent (relaxed) phase. Nuclear activity and
merging processes could have made available this energy budget that today is
released in the form of relativistic electrons.
