methods is reported in Appendix \[sec:strong\].

Reddening Corrections {#sec:redcor}
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The relative intensities of the Balmer lines are nearly independent of both density and temperature, so they can be used to solve for the reddening. The MMT spectra were de-reddened using the reddening law of @cardelli89, parameterized by $A_{V}=3.1\ E(B-V)$, where the extinction, $A_{1}(\lambda)$ was calculated using the York Extinction Solver [@mccall04][^5]. With these values, the reddening, $E(B-V)$, can be derived using $$\log{\frac{I(H\alpha)}{I(H\beta)}\ } = \log{\frac{F(H\alpha)}{F(H\beta)}\ } + 0.4\ E(B-V)\ [A_{1}(H\alpha)-A_{1}(H\beta)],
    \label{eq:dered}$$ where $F$(H$\alpha)/F$(H$\beta$) is the observed flux ratio and $I$(H$\alpha)/I$(H$\beta$) is the de-reddened line intensity ratio using case B from @storey87, assuming an electron temperature calculated from the \[\] line ratio and $n_{\rm e}=10^{2}$ cm$^{-3}$. For our sample, the electron temperature range is 9,500 K - 19,500 K, with an average of 13,300 K. This range agrees with the typical electron temperatures of 10,000 K - 20,000 K for metal-poor regions. This same process can be carried out for the H$\gamma$/H$\beta$ and H$\delta$/H$\beta$ ratios observed. When all the necessary Balmer lines were present, which is true of all of the objects in our “Select" sample, we used a minimized chi squared approach to find the best estimate of E(B-V) 