similar magnitude Sloan galaxies.

These methods employ normalized cumulative evenly spaced step-functions to track the distributions of the objects. This approach works well for objects such as LGRBs and SNe whose detection is proportionate to their event rate. Galaxy samples however have massive Malmquist biases and the individual galaxies are themselves dissimilar. To allow for direct meaningful comparison between the metallicity distribution of LGRBs and galaxies [@stats_paper] first converted the SDSS to a volume limited sample with a tight redshift cut and then weighted the galaxies by their star-formation rate. The result was a weighted step-function for the galaxy population with a varying step height. The LGRBs showed a strong preference for low metallicities while the SNe populations tracked the star-formation weighted volume limited galaxy sample.

Here we are tasked with the need to compare a variety of different LGRB populations (composted of LGRB samples with different measured physical properties) to exclude redshift dependent selection biases from contaminating our further analysis. Normalized cumulative distribution plots would ordinarily be ideal for such a task except that the differing physical properties have different redshift ranges where they can be observed and different rates of observation (e.g. metallicity measurement requires spectroscopy of certain 