Astronomy & Astrophysics

All Tables

Table 1: Main parameters of the new 30 m observations ( top). Typical receiver and system temperatures are shown as $T_{\rm rec}$ and $T_{\rm sys}$ , respectively. We also show the relevant parameters for previous observations used in this work ( bottom). See original references for details.
Table 2: Parameters of gaussian fits to the SiO/H¹³CO⁺/HCO lines observed in NGC 1068. Errors (in brackets) are 1- $\sigma$ . For the non-detection of SiO(3-2) in the N position we give a 3- $\sigma$ upper limit.
Table 3: Integrated intensities of the spectra of Fig. 4 in the blue (Col. 2) and red (Col. 3) components. Column 4 = blue-to-red (east-to-west) ratio of mean temperatures. Errors (in brackets) are 1- $\sigma$ .
Table 4: Mean temperatures in the East and West knots of the CND after correction for dilution: Col. 1 = name of the line; Col. 2 = mean temperature in the East-knot; Col. 3 = idem in the West-knot.
Table 5: LVG results: Col. 1 = chemical species; Col. 2 = parameters determined from the LVG models (n: molecular gas densities in cm^-3; $N/\Delta v$ : column densities per velocity interval in cm^-2 km^-1 s; X: chemical abundances relative to H₂; we assume $X{\rm (CO)}=8\times 10^{-5}$ and compute the rest of abundances accordingly from column density ratios relative to CO); Col. 3 = solutions for the East-knot; Col. 4 = same for the West-knot; Col. 5 = east-to-west ratio of abundances.
Table 6: Abundance ratios predicted/observed in different molecular regions: the E-knot of the CND of NGC 1068, same for the West-knot; a prototypical XDR (Lepp & Dalgarno 1996; Yan & Dalgarno 1997), the Orion Extended Region (OER) (Blake et al. 1987), and the OER corrected with oxygen depletion (Ruffle et al. 1998).