source in the slit was used to extract the galaxy emission within apertures that encompassed $\gtrsim99\%$ of the light. Figure \[fig2\] shows a sample of four of the resulting one-dimensional spectra extracted for galaxies that had significant \[\] $\lambda$4363 detections. The inset windows display a narrower spectral range to emphasize the \[\] $\lambda$4363 strength. This sample does not feature the best spectra from our sample, but rather galaxies are ordered by ionizing radiation field strength from highest to lowest as given by the \[\] $\lambda5007$/\[\] $\lambda3727$ ratio, highlighting the variation within the sample.

Photometry {#sec:phot}
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To better characterize our low-luminosity sample, absolute magnitudes in several different bands were obtained. Here we describe their origin and reference their subsequent use. $M_B$ values were determined by @vanzee12 using photometry from apertures matched to the infrared LVL photometry (unless otherwise noted). Optical photometry for the entire LVL sample is given in @cook12, whereas @vanzee12 focuses on the analysis of colors and EW gradients of dwarf galaxies. The data are used to examine the optical luminosity-metallicity relationship (see Section \[sec:Lb-Z\]).

$M_{[4.5]}$ values from the 4.5 $\mu$m IRAC photometry presented in @dale09 were calculated using $$M_{[4.5]} = -2.5\log{\frac{F_{[4.5]} (d/10)^2}{179.7}},$$ where $F_{[4.5]}$ is the 4.5 