and then compared along an \[O III\] to \[O II\] line ratio contour against the best calibration data available. This classical application however treats ionization as a parameter independent of metallicity and ignores the feedback the latter has on the former. [@kd2002] solve this issue by using iterative fitting to dynamically factor the effects of the metallicity on the ionization parameter.[^2]

Distribution Analysis
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One of the most powerful tools for understanding the behavior of GRBs (and SNe) is to study the distribution of such events with respect to a physical property. [@Fruchter] compared the location distribution of LGRB and ccSNe events on their host galaxies with the distribution of the blue light in their hosts. The result was that, while core collapse supernovae follow the blue light distribution of their host galaxies, LGRBs showed a strong preference for occurring in the brightest regions of their hosts. This suggested that, while ccSNe are unbiased tracers of the available star-formation, LGRBs likely favor very massive progenitors which are concentrated in the most star forming regions of their host galaxies. [@Stanek2007] compared the metallicity distribution of LGRBs and SDSS galaxies to show that nearby LGRB hosts have low metallicities when compared to 