We exploit data from the Pan-Andromeda Archaeological Survey (PAndAS) to study the extended structures of M31's dwarf elliptical companions, NGC 147 and NGC 185. Our wide-field, homogeneous photometry allows us to construct deep colour–magnitude diagrams which reach down to ∼3 mag below the red giant branch (RGB) tip. We trace the stellar components of the galaxies to surface brightness of μg ∼ 32 mag arcsec−2 and show that they have much larger extents (∼5 kpc radii) than previously recognized. While NGC 185 retains a regular shape in its peripheral regions, NGC 147 exhibits pronounced isophotal twisting due to the emergence of symmetric tidal tails. We fit single Sérsic models to composite surface brightness profiles constructed from diffuse light and star counts and find that NGC 147 has an effective radius almost three times that of NGC 185. In both cases, the effective radii that we calculate are larger by a factor of ∼2 compared to most literature values. We also calculate revised total magnitudes of M g = −15.36 ± 0.04 for NGC 185 and M g = −16.36 ± 0.04 for NGC 147. Using photometric metallicities computed for RGB stars, we find NGC 185 to exhibit a metallicity gradient of Fe/H ∼ −0.15 dex kpc−1 over the radial range 0.125–0.5 deg. On the other hand, NGC 147 exhibits almost no metallicity gradient, ∼−0.02 dex kpc−1 from 0.2 to 0.6 deg. The differences in the structure and stellar populations in the outskirts of these systems suggest that tidal influences have played an important role in governing the evolution of NGC 147.