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Very high energy (VHE) emission has been detected from the radio galaxyNGC1275, establishing it as a potential cosmic-ray (CR) accelerator and a highenergy neutrino source. We here study neutrino and $\gamma$-ray emission fromthe core of NGC1275 simulating the interactions of CRs assumed to beaccelerated by magnetic reconnection, with the accreting plasma environment. Todo this, we combine (i) numerical general relativistic (GR)magneto-hydrodynamics (MHD), (ii) Monte Carlo GR leptonic radiative transferand, (iii) Monte Carlo interaction of CRs. A leptonic emission model thatreproduces the SED in the [$10^3$-$10^{10.5}$] eV energy range is used as thebackground target for photo-pion interactions+electromagnetic cascading. CRsinjected with the power-law index \k{appa}=1.3 produce an emission profile thatmatches the VHE tail of NGC1275. The associated neutrino flux, below theIceCube limits, peaks at $\sim$PeV energies. However, coming from a singlesource, this neutrino flux may be an over-estimation.

Neutrino and $\gamma$-ray Emission from the Core of NGC1275 by Magnetic Reconnection: GRMHD Simulations and Radiative Transfer/Particle Calculations