We explore the behaviour of [C ii] λ157.74 μm forbidden fine-structure line observed in a sample of 28 galaxies selected from ∼ 50 deg² of the Herschel-Astrophysical Terahertz Large Area Survey survey. The sample is restricted to galaxies with flux densities higher than S_160 μm > 150 mJy and optical spectra from the Galaxy and Mass Assembly survey at 0.02 < z < 0.2. Far-IR spectra centred on this redshifted line were taken with the Photodetector Array Camera and Spectrometer instrument on-board the Herschel Space Observatory. The galaxies span 10 < log(L_IR/L_⊙) < 12 (where L_IR ≡ L_IR[8-1000 μm]) and $7.3<{\rm log} (L_{\rm [C\,\small {II}]}/{\rm L}_{\odot }) <9.3$, covering a variety of optical galaxy morphologies. The sample exhibits the so-called [C ii] deficit at high-IR luminosities, i.e. $L_{[{\rm C\,\small {II}}]}$/L_IR (hereafter [C ii]/IR) decreases at high L_IR. We find significant differences between those galaxies presenting [C ii]/IR >2.5 × 10⁻³ with respect to those showing lower ratios. In particular, those with high ratios tend to have: (1) L_IR <10¹¹ L_⊙; (2) cold dust temperatures, T_d < 30 K; (3) disc-like morphologies in r-band images; (4) a Wide-field Infrared Survey Explorer colour 0.5 ≲ S_12 μm/S_22 μm ≲ 1.0; (5) low surface brightness Σ_IR ≈ 10^8–9 L_⊙ kpc⁻², (6) and specific star formation rates of sSFR ≈0.05–3 Gyr⁻¹. We suggest that the strength of the far-UV radiation fields (〈G_O〉) is main parameter responsible for controlling the [C ii]/IR ratio. It is possible that relatively high 〈G_O〉 creates a positively charged dust grain distribution, impeding an efficient photoelectric extraction of electrons from these grains to then collisionally excite carbon atoms. Within the brighter IR population, 11 < log(L _IR/L_⊙) < 12, the low [C ii]/IR ratio is unlikely to be modified by [C ii] self-absorption or controlled by the presence of a moderately luminous AGN (identified via the BPT diagram).