All Tables

Table 1: Basic properties of the sample galaxies.
Table 2: Source sizes used to convolve the data to 21.9''. For each source, we used maps (specified in Col. 5) to determine the shape of the Gaussian intensity profile (axisymmetric : a $\times$ a or elliptical: a $\times$ b) and estimate the values of the full widths at half maximum (FWHM).
Table 3: Parameters of the "best fit'' LVG and PDR models for IC 10, IC 342, NGC 4038, Overlap, M 83 and NGC 6946. For each galaxy, the same abundance ratio $\frac{^{12}C}{^{13}C}^{b}$ and the same $\Delta v^{a}$ are used for constraining both LVG and PDR models. To compare observations and predictions deduced from models, the observed CO (¹²CO and ¹³CO) and the observed C cooling rates are listed at the bottom.
Table 4: Observed and predicted ("best'' LVG model) line ratios for the studied sources.
Table 5: Observed and predicted ("best'' PDR model) line intensity ratios.
Table B.1: Results from the Gaussian fits derived from spectra of the Antennae (NGC 4038 et Overlap), Arp 220, Centaurus A, Henize 2-10, IC 10, IC 342, IRAS 10565, M 51, M 82, M 83, Mrk 231, NGC 253, NGC 891, NGC 1068, 3079, NGC 4736, NGC 6090 and NGC 6946. The observed lines (¹²CO, ¹³CO and C) are indicated in the first column. For each source, the RA(1950) and DEC(1950) positions of the center (0'',0'') is listed in Table 1. The indication ^a corresponds to the spectra shown in this article (see Figs. 1 to 16).
Table B.2: Results of the Gaussian fits derived from spectra of the Antennae (NGC 4038 et Overlap), Henize 2-10, IC 10, IC 342, M 83, NGC 253 and NGC 6946. See caption of Table B.1. Data listed in this table are either from literature or from our sample of observations.