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In this contribution, we test our previously published one-dimensional PDRmodel for deriving total hydrogen volume densities from HI column densitymeasurements in extragalactic regions by applying it to the Taurus molecularcloud, where its predictions can be compared to available data. Also, we makethe first direct detailed comparison of our model to CO(1-0) and far-infraredemission. Using an incident UV flux G0 of 4.25 ({\chi} = 5) throughout the mainbody of the cloud, we derive total hydrogen volume densities of \approx 430cm-3, consistent with the extensive literature available on Taurus. Thedistribution of the volume densities shows a log-normal shape with a hint of apower-law shape on the high density end. We convert our volume densities to H2column densities assuming a cloud depth of 5 parsec and compare these columndensities to observed CO emission. We find a slope equivalent to a COconversion factor relation that is on the low end of reported values for thisfactor in the literature (0.9 x 1020 cm-2 (K km s-1)-1), although this value isdirectly proportional to our assumed value of G0 as well as the cloud depth. Weseem to under-predict the total hydrogen gas as compared to 100 {\mu}m dustemission, which we speculate may be caused by a higher actual G0 incident onthe Taurus cloud than is generally assumed.

Applying a one-dimensional PDR model to the Taurus molecular cloud and its atomic envelope