description of the method used to determine “direct" oxygen abundances in § \[sec:metallicity\]. Our “Select" sample, compiled from objects with “direct" oxygen abundances and secure distance estimates, is defined in § \[sec:Gold\]. Using this sample, metallicity is compared to expected trends with *B*-band luminosity, 4.5 $\mu$m luminosity, and stellar mass in § \[sec:Lb-Z\], § \[sec:L-Z\], and § \[sec:M-Z\] respectively. N/O relative abundances are discussed in § \[sec:N/O\]. In § \[sec:discussion\] we discuss the results of the relationships found in § \[sec:Lb-Z\]-§ \[sec:M-Z\], the “young galaxy" hypothesis, and the quality of abundance estimators. Finally, we summarize our conclusions in § \[sec:conclusion\]. Appendix \[sec:strong\] presents the strong-line abundances for the low-luminosity LVL galaxies for which we were unable to determine “direct” abundances. and Appendix \[sec:outlier\] presents our new “direct" abundances in comparison to the color-temperature metallicity relationship of @engelbracht08.

Sample Selection
================

*Spitzer* LVL Survey {#sec:LVL}
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LVL is a *Spitzer Space Telescope* legacy program that combines IRAC (Infrared Array Camera) and MIPS (Multiband Imaging Photometer) infrared imaging for a complete sample of 258 galaxies for the nearest 11 Mpc of our local universe. These data build upon recent Local Volume galaxy surveys: narrowband H$\alpha$ [@kennicutt08], *GALEX* ultraviolet [@jlee11], and *Hubble Space 