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The metal content of a galaxy is a key property for distinguishing betweenviable galaxy evolutionary scenarios, and it strongly influences many of thephysical processes in the interstellar medium. An absolute and robustdetermination of extragalactic metallicities is essential in constrainingmodels of chemical enrichment and chemical evolution, however, current gasphase abundance determinations from optical fine-structure lines are uncertainto 0.8 dex as conversion of these optical line fluxes to abundances is stronglydependent on the electron temperature of the ionized gas. In contrast, thefar-IR emission lines can be used to derive an O++ abundance that is relativelyinsensitive to temperature, while the ratio of the optical to far-IR linesprovides a consistent temperature to be used in the derivation of an O$^+$abundance. We present observations of the [O III] 88 \micron\ fine-structureline in NGC 628 that were obtained as part of the KINGFISH program. These dataare combined with optical IFU data to derive oxygen abundances for seven HIIregions. We find the abundance of these regions to all lie between the high andlow values of strong line calibrations and in agreement with estimates thatassume temperature fluctuations are present in the HII regions.

Towards A Removal of Temperature Dependencies from Abundance Determinations