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Many abundance studies are based on spectrum synthesis and $\chi$-squareddifferences between the synthesized and an observed spectrum. Much of thespectra so compared depend only weakly on the elemental abundances. Logarithmicplots of line depths rather than relative flux make this more apparent. Wepresent simulations that illustrate a simple method for finding regions of thespectrum most sensitive to abundance, and also some caveats for using suchinformation. As expected, we find that weak features are the most sensitive.Equivalent widths of weak lines are ideal features, because of theirsensitivity to abundances, and insensitivity to factors that broaden the lineprofiles. The wings of strong lines can also be useful, but it is essentialthat the broadening mechanisms be accurately known. The very weakest features,though sensitive to abundance, should be avoided or used with great cautionbecause of uncertainty of continuum placement as well as numericaluncertainties associated with the subtraction of similar numbers.

Abundance sensitive points of line profiles in the stellar spectra