Dependence of the derived Region 1 Bar abundances (X_ICF,Bar; log form and solar normalized) on assumed n_e and T_e. The left panel shows the effect of varying n_e = [10³, 10⁶] cm⁻³ at fixed T_e = 7500 K, and the right panel shows varying T_e = [6000, 15,000] K at fixed n_e = 10³ cm⁻³. Vertical dashed (dotted) lines in the left panel mark n_crit for the lower (higher) IP ions used to calculate X_i,Bar (Table 1). The horizontal dotted line marks solar abundance. Uncertainties are estimated via MC propagation of line flux uncertainties through PyNeb. X_ICF,Bar increases with n_e and decreases with T_e, and elements with low n_crit are the most sensitive to the chosen n_e.