{#zd}
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Before we can explore the metallicity distribution of LGRBs as a function of redshift we need to account for completeness of our sample population. Given the nature of this sample as a completion of observations from many different observing programs, each with different sample criteria, luminosity biases, available per object observing time, and science goals, an a priori assessment is not practical. We can however annualize the effect of redshift on the completeness of the differing LGRB populations. To achieve this we cumulatively plot the redshifts of the different LGRB populations. In a typical cumulative distributions plot we would normalize the populations so as to allow for comparison of populations with different numbers of objects. Here however we are faced with some samples with a redshift range that ends far before others (and the end of the range plotted). We also have other samples with additional selection effects apparent only at high redshifts. Therefore, instead of normalizing the distributions to unity we scale each population by a unique arbitrary factor so as to produce distributions consistent with each other. As we will later focus on analyzing the LGRB metallicity distribution we thus chose to scale our populations to 