be different for galaxies with luminosities greater than that of the LMC. However, the similarity of the slopes of the optical and near-IR L-Z relationships for our sample probably reflects little influence by dust extinction in the low luminosity galaxies. For this sample, we derive a mass-metallicity relationship of 12 + log(O/H) = (5.61$\pm0.24) + (0.29\pm0.03) \log(\mbox{M}_{\star})$, which agrees with previous studies; however, the dispersion ($\sigma$ = 0.15) is not significantly lower than that of the L-Z relationships. Because of the low dispersions in these relationships, if an accurate distance is available, the luminosity of a low luminosity galaxy is often a better indicator of metallicity than that derived using certain “strong-line” methods, so significant departures from the L-Z relationships may indicate that caution is prudent in such cases. With these new “direct" metallicities we also revisit the 70/160 $\mu$m color metallicity relationship.

    Additionally, we examine N/O abundance trends with respect to oxygen abundance and B-V color. We find a positive correlation between N/O ratio and B-V color for 0.05 $\lesssim B-V \lesssim$ 0.75: $\log(\mbox{N/O})$ = (1.18$\pm$0.9)$\times$(B-V) + ($-$1.92$\pm$0.08), with a dispersion of $\sigma$ = 0.14, that is in agreement with previous studies.
author:
- 'Danielle A. Berg, Evan D. 