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 ∼89 Active Galactic Nuclei (AGN). At VHE, in contrast to the dominant blazar population, very few radio galaxies are detected. NGC 1275 (3C 84) is a radio galaxy in the nearby Perseus cluster (z∼0.0176). Extensive observations of NGC 1275 across all wavebands reveal a complex morphology that has evolved with time. The origin of the VHE emission in both flaring and non-flaring states of NGC 1275 is still not entirely understood. In the current study, we present the low-state spectral energy distribution of NGC 1275 constructed with multi-wavelength observations from ALMA, ATLAS, Swift-UVOT, Swift-XRT, Fermi-LAT, and VERITAS over the period 2012-2017. We find that the low-state emission is well explained by a single-zone Synchrotron self-Compton model which favors a large emission region.