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