  The recent 230 GHz observations of the Event Horizon Telescope (EHT) are able
to image the innermost structure of the M87 and show a ring-like structure
which is in agreement with thermal synchrotron emission generated in a torus
surrounding a supermassive black hole. However, at lower frequencies M87 is
characterised by a large-scale and edge-brightened jet with clear signatures of
non-thermal emission. In order to bridge the gap between these scales and to
provide a theoretical interpretation of these observations we perform general
relativistic magnetohydrodynamic simulations of accretion on to black holes and
jet launching.
  M87 has been the target for multiple observations across the entire
electromagnetic spectrum. Among these VLBI observations provide unique details
on the collimation profile of the jet down to several gravitational radii. In
this work we aim to model the observed broad-band spectrum of M87 from the
radio to the NIR regime and at the same time fit the jet structure as observed
with Global mm-VLBI at 86 GHz. We use general relativistic magnetohydrodynamics
and simulate the accretion of the magnetised plasma onto Kerr-black holes in
3D. The radiative signatures of these simulations are computed taking different
electron distribution functions into account and a detailed parameter survey is
performed in order to match the observations.
  The results of our simulations show that magnetically arrested disks around
fast spinning black holes ($a_\star\geq0.5$) together with a mixture of thermal
and non-thermal particle distributions are able to model simultaneously the
broad-band spectrum and the innermost jet structure of M87
