This interval encompasses almost all of the emission in the Taurus region, with the exception of some isolated areas with gas at $\simeq$ 10 , which may well not be associated with Taurus, and a limited amount of emission in the velocity range 1  to 2 . Figure \[12co\_tmax\] displays the  J = 1$\rightarrow$0 peak emission within this same velocity interval. Note that in both of these figures, the emission is not corrected for the antenna efficiency. [@narayanan2007] present images of the emission of both isotopologues in 1  bins covering the range 0  to 13 .

It is evident that the  is detectable over a significantly larger area than is the . Particularly in the northeast portion of the map, we see very extended  emission, where there is relatively little . There are also two interesting regions of quite strong  emission, at 422+2830 and 448+2940, which are among the warmest regions observed, and yet which do not show up as significant local maxima in the  (and hence column density). In general, the warmer gas as traced by  is seen in regions of high column density, but the amount of structure seen in the optically thick  with our angular resolution, sampling, 