All Tables

Table 1: Observation parameters.
Table 2: Calibrator fluxes in Jy.
Table 3: Molecular column densities and abundances at 3 different positions of the PDR named "Cloud'', "IR peak'' and "IR edge''. Equatorial offsets refer to the Mosaic 2 map center given in Table 1. $(\delta x, \delta y)$ offsets refer to the coordinate system defined in Fig. 3. H₂ column densities have been derived from the 1.2 $\ensuremath{~ \ensuremath{{\rm mm}}}$ dust continuum emission using a dust temperature range of 20 to 40 $\ensuremath{~ \ensuremath{{\rm K}}}$ for the "Cloud'' position and 40 to 80 $\ensuremath{~ \ensuremath{{\rm K}}}$ for the IR positions. Others column densities used LVG models with a representative set of densities and kinetic temperature. 1- $\sigma$ uncertainties thus reflect the systematics due to the approximate knowledge of density and kinetic temperature. Abundances are computed with respect to the number of protons, i.e. $[{\rm X}] = 0.5~N({\rm X})/N(\mbox{H$_2$ })$ .