included 2.4$\times$10$^8$ voxels.

As discussed in detail by [@narayanan2007], the overall quality of the data was excellent. After calibration and combination of the 30 by 30 submaps which were the units in which the data was taken, the data were resampled onto a uniform grid of 20 spacing, which is very close to the Nyquist sampling interval $\lambda/2D$ for the 13.7 m diameter telescope operating at a wavelength of 2.6 mm. The images produced by the combination of the submaps and regridding were 2069 pixels in RA by 1529 pixels in decl., thus comprising 3,163,501 spatial pixels resampled onto a uniform 20 grid. The final data set has a well–behaved distribution of noise with a mean rms antenna temperature equal to 0.125 K for  and 0.28 K for  in channel widths of 0.27 and 0.26 , respectively.

![\[13co\_tint\] Antenna temperature of the  J = 1$\rightarrow$0 transition integrated over the velocity range 2 to 9 . The scale is shown in the bar at the right; values have not been corrected for antenna efficiency.](f1.pdf)

We show the basic  data in Figure \[13co\_tint\], which gives the intensity of the  J = 1$\rightarrow$0 transition integrated over the velocity range 2  to 9 . 