Portion of the spectrum of the nine Ap stars with resolved magnetically split lines that were not studied in M24. The wavelengths are in the laboratory reference frame. The main lines are Nd III λ 6145.1 Å, Cr II λ 6147.2 Å, Fe II λ 6147.6 Å, and Fe II λ 6149.2 Å; their Zeeman patterns were shown in Fig. 3 of M24. The doublet pattern of the Fe II λ 6149.2 Å line is of particular interest as it lends itself to mostly approximation-free and model-independent determination of the mean magnetic field modulus ⟨B⟩. However, in a fraction of the stars, its blue wing is affected to some extent by blends that may include contributions from the Sm II λ 6149.06 Å line and/or from an unidentified line. This blend is exceptionally strong in HD 143487, which also features the strongest Nd III λ 6145.2 Å line of all the stars shown here. The benefit of the higher resolving power of HARPS-N over the lower one of SALT-HRS for separation of the magnetically split components of the Fe II λ 6149.2 Å line is also apparent in this figure.