may have omitted many valuable contributions.

The very closeness of Taurus means that available instrumentation, particularly at radio frequencies, has faced a challenge to cover the entire region with angular resolution sufficient to reveal the morphology of the gas. The result has been that previous large–scale surveys of molecular line emission at millimeter wavelengths have been limited to quite low angular resolution [@ungerechts1987]. The survey of [@ungerechts1987] covers essentially all of Taurus and part of Perseus, but the 30 angular resolution of the map (obtained by averaging multiple telescope pointings to obtain a larger effective beam size) yields only 3000 pixels in the 750 square degree region mapped. The pixel size corresponds to a linear size of 1.2 pc at a distance of 140 pc, which is sufficiently large to blur out structure at important astrophysical scales. In fact, the maps of [@ungerechts1987], while delineating the large–scale structure quite well, show an almost complete absence of fine detail. This is in part due to the use exclusively of , which is sufficiently optically thick that significant variations in column densities can be entirely hidden, as well as to the low angular resolution.

There have been a number of investigations of 