The VERITAS observatory is a ground-based imaging atmospheric Cherenkov telescope array that detects very-high-energy (VHE; E>100 GeV) gamma-ray emission from a range of astrophysical sources including more than ~40 Active Galactic Nuclei (AGN). Very few radio galaxies, AGN with relativistic jets oriented at angles offset to our line-of-sight, are detected at VHE including NGC 1275 (3C 84), the central galaxy in the Perseus cluster (z~0.0176). NGC 1275 has a long history of observations across all wavebands, and a complex morphology that has evolved with time. The origin of the TeV emission in NGC 1275 in both the flaring and non-flaring states is still not entirely understood. A VERITAS study of a January 2017 flare finds that a multi-component model is required to fit the multi-wavelength spectral energy distribution (SED). In this study, we present the EBL-corrected, Compton SED peak in the non-flaring state of NGC 1275 constructed with simultaneous VERITAS and Fermi-LAT observations over the period 2012-2017.