  We study the contribution of thermal and non-thermal processes to the inverse
Compton emission of the radio galaxy M 87 by modelling its broad-band emission.
Through this we aim to derive insight into where within the AGN the X-ray,
gamma-ray, and VHE emission is produced. We have analysed all available
INTEGRAL IBIS/ISGRI data on M 87, spanning almost 10 years, to set an upper
limit to the average hard X-ray flux of $f(20 - 60 \rm \, keV) < 3\times
10^{-12}$ $\rm \, erg \, cm^{-2} \, s^{-1}$, using several techniques beyond
the standard analysis which are also presented here. We also analysed hard
X-ray data from Suzaku/PIN taken late November 2006, and we report the first
hard X-ray detection of M 87 with a flux of $f(20 - 60 \rm \, keV) =
10^{-11}\rm \, erg \, cm^{-2} \, s^{-1} $. In addition we analyse data from
Fermi/LAT, INTEGRAL/JEM-X, and Suzaku/XIS. We collected historical
radio/IR/optical and VHE data and combined them with the X-ray and gamma-ray
data, to create broad-band spectral energy distributions for the average
low-flux state and the flaring state. The resulting spectral energy
distributions are modelled by applying a single-zone SSC model with a jet angle
of theta = 15 degrees. We also show that modelling the core emission of M 87
using a single-zone synchrotron self-Compton model does represent the SED,
suggesting that the core emission is dominated by a BL Lac type AGN core. Using
SED modelling we also show that the hard X-ray emission detected in 2006 is
likely due to a flare of the jet knot HST-1, rather than being related to the
core.
