Comparison of simulated profiles of vanadium lines used in Adibekyan et al. (2012), without and with HFS components,for a K dwarf (T_eff = 4800 K) and a G dwarf (T_eff = 5700 K) with a solar abundance pattern at CARMENES VIS resolution (). The red andorange solid lines are generated from the VALD3 atomic line list including the latest HFS components, for the K and G dwarf respectively. The dotted blue and green lines are simulated from a line list without HFS components. The lines are much stronger in later-type stars. While most lines show very small deviations, a few lines (notably λ567.085 nm, λ573.707 nm, and λ625.183 nm) in the K dwarf exhibit significant systematic differences when HFS is considered.