Typically, three 900 second exposures[^3] were made with the slit at a fixed position angle which approximated the parallactic angle at the midpoint of the observation and laid across several H$\alpha$ bright regions when possible. This, in addition to observing the galaxies at airmasses less than 1.5, served to minimize the wavelength-dependent light loss due to differential refraction [@filippenko82]. A single slit position for each target was deemed sufficient to characterize the global oxygen abundance, as metallicity gradients are observed to be small or non-existent in low-mass galaxies [e.g., @skillman89; @ks96; @ks97; @lee06b; @croxall09]. Finally, combined helium, argon, and neon arc lamps were observed at each pointing for accurate wavelength calibration. A log of the observations is provided in Table \[tbl2\]. Figure \[fig1\] shows the R-band continuum and H$\alpha$ continuum-subtracted images for each galaxy, motivating our slit location choices. The brightest H$\alpha$ regions observed are ordered alphabetically by decreasing flux, and the slit positions on the galaxies are shown. The images scale as 60x60 arcseconds with North oriented up and East to the left.

### Spectra Reduction {#sec:mmtreduct}

The MMT observations were processed using ISPEC2D [@moustakas06], a long-slit spectroscopy data reduction package written in IDL. A master bias frame was 