2 Observations

All observations were carried out with the 15 m James Clerk Maxwell Telescope (JCMT) on Mauna Kea (Hawaii), mostly between 1993 and 1996. The JCMT has a pointing accuracy better than 2'' rms Observations of the ${\rm ^{3}P_{1}}{-}{\rm ^{3}P_{0}\,[CI]}$ transition at $\nu$ = 492.161 GHz were made at a resolution of 10.2'' (HPBW); those of the J= 2-1  ${\rm ^{13}CO}$ transition with a resolution of 22''. The observing conditions can be judged from the total system temperatures (including sky) which are listed in Table 1.

All observations were obtained using the Digital Autocorrelator Spectrograph as a backend. Spectra were binned to various resolutions; we applied linear baseline corrections only and scaled the spectra to main-beam brightness temperatures, $T_{\rm mb}$ = $T_{\rm A}^{*}$/ $\eta _{\rm mb}$. Line parameters were determined by Gaussian fitting and by adding channel intensities over the relevant range. For observations at 492 GHz we used $\eta _{\rm mb}$ = 0.43 up to January 1995 and $\eta _{\rm mb}$ = 0.50 for later observations. For observations at 220 GHz, we used $\eta _{\rm mb}$ = 0.69. A list of the observed galaxies and additional information is given in Table 1.