Gamma-ray emitting radio galaxies at hard X-rays: Seyfert core or jet
  emission?
  A number of radio galaxies has been detected by Fermi/LAT in the gamma-ray
domain. In some cases, like Cen A and M 87, these objects have been seen even
in the TeV range by Cherenkov telescopes. Whereas the gamma-ray emission is
likely to be connected with the non-thermal jet emission, dominating also the
radio band, the situation is less clear at hard X-rays. While the smoothly
curved continuum emission and the overall spectral energy distribution indicate
a non-thermal emission, other features such as the iron line emission and the
low variability appear to be rather of Seyfert type, i.e. created in the
accretion disk and corona around the central black hole.
  We investigate several prominent cases using combined X-ray and gamma-ray
data in order to constrain the possible contributions of the jet and the
accretion disk to the overall spectral energy distribution in radio galaxies.
Among the three sources we study, three different origins of the hard X-ray
flux can be identified. The emission can be purely non-thermal and caused by
the jet, as in the case of M 87, or thermal inverse Compton emission from the
Seyfert type core (Cen A), or appears to be a superposition of non-thermal and
thermal inverse Compton emission, as we observe in 3C 111. Gamma-ray bright
radio galaxies host all kinds of AGN cores, Seyfert 1 and 2, BL Lac objects,
and also LINER.
