local universe with multiwavelength observations spanning the ultraviolet to the radio. The LVL is leveraged by ancillary data including H$\alpha$ [@kennicutt08] and UV [@jlee11] imaging from the 11 Mpc H$\alpha$ and Ultraviolet Galaxy Survey [11HUGS; @jlee11] and the Nearby Galaxy Survey [NGS; @gildepaz07]. A subsample of the LVL also contains stellar population mapping from the ACS Nearby Galaxy Survey Treasury [ANGST; @dalcanton09], HI mapping from the VLA and GMRT, and optical broad-band imaging [@cook12; @vanzee12] and spectroscopy. However, many of the faintest objects are missing the high-quality optical spectroscopy needed to determine “direct" oxygen-abundance metallicity estimates.

As the L-Z relationship provides both a very strong constraint on theories of galaxy evolution and a tool to better understand galaxies at higher redshifts [@kobulnicky03], we are motivated to better characterize the low-luminosity end of the L-Z relationship. Thus, we obtained high-resolution MMT spectroscopy of 42 low luminosity star-forming galaxies in the Local Volume with the goal of detecting the \[\] $\lambda$4363 line in order to constrain electron temperature measurements.

We present our low-luminosity sample in § \[sec:Sample\], with spectral observations obtained from the MMT in § \[sec:mmt\] and IRAC photometry in § \[sec:phot\]. Section \[sec:data\] describes the data reduction, followed by the 