We present MMT spectroscopic observations of H ii regions in 42 low luminosity galaxies in the Spitzer Local Volume Legacy ( LVL ) survey . For 31 of the 42 galaxies in our sample , we were able to measure the temperature sensitive [ O iii ] \lambda 4363 line at a strength of 4 \sigma or greater , and thus determine oxygen abundances using the “ direct ” method . Our results provide the first “ direct ” estimates of oxygen abundance for 19 of these galaxies . “ Direct ” oxygen abundances were compared to B -band luminosities , 4.5 \mu m luminosities , and stellar masses in order to characterize the luminosity-metallicity and mass-metallicity relationships at low-luminosity . We present and analyze a “ Combined Select ” sample composed of 38 objects ( drawn from a sub-set of our parent sample and the literature ) with “ direct ” oxygen abundances and reliable distance determinations ( based on the tip of the red giant branch or Cepheid variables ) . Consistent with previous studies , the B -band and 4.5 \mu m luminosity-metallicity relationships for the 38 objects were found to be 12 + log ( O/H ) = ( 6.27 \pm 0.21 ) + ( -0.11 \pm 0.01 ) M _ { B } and 12 + log ( O/H ) = ( 6.10 \pm 0.21 ) + ( -0.10 \pm 0.01 ) M _ { [ 4.5 ] } with dispersions of \sigma = 0.15 and 0.14 respectively . The slopes of the optical and near-IR L-Z relationships have been reported to 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 \pm 0.24 ) + ( 0.29 \pm 0.03 ) \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 .