molecular gas in the Taurus region with higher angular resolution, but these have typically been limited to small subregions within the overall gas distribution. These studies, with $\simeq$1 to 2 angular resolution include a few thousand to $\simeq$ 30,000 spatial pixels [@schloerb1984; @duvert1986; @heyer1987; @mizuno1995]. These studies, with the combination of higher angular resolution and use of the J = 1$\rightarrow$0 transition of do reveal considerable structure in the molecular gas, but have not elucidated its relationship to larger–scale features in the molecular gas distribution.

A number of other studies have utilized yet higher angular resolution and different tracers to probe gas having different characteristic properties over limited regions. Some examples include [@langer1995] employing CCS, [@onishi1996] and [@onishi1998] using , [@onishi2002] using H$^{13}$CO$^+$, and [@tatematsu2004] employing N$_2$H$^+$. Many individual cores have been observed in ammonia, a tracer in which they appear relatively well–defined, as indicated by compilation of @jijina1999. Most of the regions covered by these studies have been pre-selected based on the large–scale surveys discussed above. In these maps, we see indications of finer–scale structure, but the emission is generally quite spatially restricted compared to that seen in the more abundant isotopologues of carbon monoxide.

In this paper we 