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We use the public code ebhlight to carry out 3D radiative generalrelativistic magnetohydrodynamics (GRMHD) simulations of accretion onto thesupermassive black hole in M87. The simulations self-consistently evolve afrequency-dependent Monte Carlo description of the radiation field produced bythe accretion flow. We explore two limits of accumulated magnetic flux at theblack hole (SANE and MAD), each coupled to several sub-grid prescriptions forelectron heating that are motivated by models of turbulence and magneticreconnection. We present convergence studies for the radiation field and studyits properties. We find that the near-horizon photon energy density is an orderof magnitude higher than is predicted by simple isotropic estimates from theobserved luminosity. The radially dependent photon momentum distribution isanisotropic and can be modeled by a set of point-sources near the equatorialplane. We draw properties of the radiation and magnetic field from thesimulation and feed them into an analytic model of gap acceleration to estimatethe very high energy (VHE) gamma-ray luminosity from the magnetized jet funnel,assuming that a gap is able to form. We find luminosities of $\rm \sim 10^{41}\, erg \, s^{-1}$ for MAD models and $\rm \sim 2\times 10^{40} \, erg \,s^{-1}$ for SANE models, which are comparable to measurements of M87's VHEflares. The time-dependence seen in our calculations is insufficient to explainthe flaring behavior. Our results provide a step towards bridging theoreticalmodels of near-horizon properties seen in black hole images with the VHEactivity of M87.

Radiation GRMHD simulations of M87: funnel properties and prospects for gap acceleration