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The galaxy M 87 harbors a kiloparsec-scale relativistic jet, whose origincoincides with a supermassive black hole. Observational mm-VLBI campaigns arecapable of resolving the jet-launching region at the scale of the eventhorizon. In order to provide a context for interpreting these observations,realistic general-relativistic magnetohydrodynamical (GRMHD) models of theaccretion flow are constructed. The characteristics of the observedspectral-energy distribution (SED) depend on the shape of the electrons'energy-distribution function (eDF). The dependency on the eDF is omitted in themodeling of the first Event Horizon Telescope results. In this work, we aim tomodel the M 87 SED from radio up to NIR/optical frequencies using athermal-relativistic Maxwell- J\"uttner distribution, as well as a relativistic$\kappa$-distribution function. The electrons are injected based on sub-grid,particle-in-cell parametrizations for sub-relativistic reconnection. A GRMHDsimulation in Cartesian-Kerr-Schild coordinates, using eight levels of adaptivemesh refinement (AMR), forms the basis of our model. To obtain spectra andimages, the GRMHD data is post-processed with the ray-tracing code RAPTOR,which is capable of ray tracing through AMR GRMHD simulation data. We obtainradio spectra in both the thermal-jet and $\kappa$-jet models consistent withradio observations. Additionally, the $\kappa$-jet models also recover theNIR/optical emission. The models recover the observed source sizes and coreshifts and obtain a jet power of $\approx 10^{43}$ ergs/s. In the $\kappa$-jetmodels, both the accretion rates and jet powers are approximately two timeslower than the thermal-jet model. The frequency cut-off observed at $\nu\approx 10^{15}$ Hz is recovered when the accelerator size is $10^6$ - $10^8$cm, this could potentially point to an upper limit for plasmoid sizes in thejet of M 87.

Modeling non-thermal emission from the jet-launching region of M 87 with adaptive mesh refinement