350 Å, large enough that the underlying absorption was not a concern. Even for those H$\alpha$ emission lines with lower EWs, the underlying absorption was negligible. This was often not the case for H$\beta$ and the lower equivalent width Balmer lines. The H$\beta$ absorption EWs for our sample range from 1-8 Å. These values are typical of local low-luminosity galaxies, with the majority having H$\beta$ absorption EWs between 0 Å and 5 Å [see, e.g., Figure 6 in @berg11]. For the bluer Balmer lines, a multiple component fit was used in which the absorption was fit by a broad, negative Lorentzian profile and the emission was fit by a narrow, positive Gaussian profile. To ensure a proper fit of the \[\] $\lambda4363$ line, H$\gamma$ was first fit by a Gaussian profile, then \[\] $\lambda4363$ was forced to be fit to the same line profile with the assumption that the profile widths of these two neighboring lines should be the same.

Note that we chose to fit the underlying Balmer absorption with Lorentzian profiles, as opposed to using stellar population synthesis continuum fitting common in many studies [e.g., @tremonti04]. Given the large equivalent widths of the Balmer emission lines, the differences 