@Rubin_86 found that a significant fraction of the intensity of the [\[\]]{} $\lambda$5755 line can arise from recombinations of N$^{++}$. If this effect is not taken into account, the value of [$T_{\rm e}$]{}[\[\]]{} can be overestimated in those objects where N$^{++}$ is an important contributor to the total abundance of nitrogen. The contribution of recombination to [\[\]]{} $\lambda$5755 can be estimated using the expression derived by @Liu_00, which depends on the N$^{++}$ abundance. This ionic abundance can be obtained either from infrared/ultraviolet collisionally excited lines or from optical recombination lines, leading in each case to different results. Thus, the correction is somewhat uncertain and we do not apply it here. However, we estimate an upper limit of the effect it could have on our results by using the highest possible values for the N$^{++}$ abundances, which are those implied by recombination lines. We find that in many of our objects [$T_{\rm e}$]{}[\[\]]{} would change by less than 10%. The objects with the largest differences in [$T_{\rm e}$]{}[\[\]]{} are DdDm 1, IC 3568, IC 4699, M 3-32, and NGC 3242, where they reach 30–50%. For these objects, this implies values of Fe/O up to 0.4 dex lower or up to 0.2 