CO(3–2) channel maps of the galaxy NGC 4569. The velocity relative to the systemic velocity of the galaxy (v_hel = −235 km s^-1) is given at the top left of each map. The phase center indicated by the large cross is at the AGN position α_J2000 = 12^h36^m49.8^s, δ_J2000 = 13°09′46.3″. The beam (represented at the bottom left of each map) is 2.6″ × 2.1″ and the rms is 115 mJy beam^-1. The only contour line overlaid corresponds to the 4σ level. The maps are not corrected for the primary beam attenuation.

CO(3–2) channel maps of the galaxy NGC 4826. The velocity relative to the systemic velocity of the galaxy (v_hel = 402 km s^-1) is given at the top left of each map. The phase center indicated by the large cross is at α_J2000 = 12^h56^m43.76^s, δ_J2000 = 21°40′51.9″. The galactic nucleus is marked by the small cross. The beam (represented at the bottom left of each map) is 2.6″ × 1.9″ and the rms is 75 mJy beam^-1. The only contour line overlaid corresponds to the 4σ level.

Likelihood of all possible (R₂₁, R₃₂) pairs on a R₃₂-vs.-R₂₁ grid for different values of X_CO/(dV/dR). The contours of the R₃₂-vs.-R₂₁ diagrams of NGC 4569 (blue) and NGC 4826 (magenta) are overlaid. The contours are smoothed and their levels correspond to 3 and 9 pixels per grid bin. (see Fig. 11).

LVG best fits to the line ratios measured in the central region of NGC 4569 at the eight positions marked in Fig. 2. The measured line ratios are represented with the 1-σ error bars and the best fit model ratios are linked with a straight line. The inset in each plot shows the 90% confidence interval (light grey shaded area) and the 50% confidence interval (dark grey) in the density-temperature plane assuming a normal probability distribution for each ratio; the best fit solution is marked with a cross. The best fit temperature and density as well as the averages over the 90% confidence interval are given at the top right of each plot. The normalized likelihood of the best fit, P/P_max is also given (1 means the measured values are exactly reproduced by the model).

LVG result maps for NGC 4569. Upper left: H₂ number density averaged over the 90% confidence interval of each LVG model. The black contours are at 5 × 10², 10³, 3 × 10³ cm^-3 and the white contours at 5.5 × 10³, 10⁴, and 5 × 10⁴ cm^-3. Upper right: kinetic temperature averaged over the 90% confidence interval of each model. The black contours are at 5, 10, 15, 20, 25 K and the white contours at 30, 35, 40 K. Lower left: pressure averaged over the 90% confidence interval of each model. The black contours are at 10^4.1, 10^4.4, and 10^4.7 K cm^-3 and the white contours at 10⁵, 10^5.3 and 10^5.6 K cm^-3. Lower right: the normalized likelihood (or merit), P/P_max, of the best fit with black contours at 0.35 and 0.55 and white contours at 0.75 and 0.95.

LVG best fits to the line ratios measured in the central region of NGC 4826 at the eight positions marked in Fig. 6. See caption of Fig. 17 for more details.

LVG result maps for NGC 4826. Upper left: H₂ number density averaged over the 90% confidence interval of each LVG model. The black contours are at 10³ and 5 × 10³ cm^-3 and the white contours at 10⁴ and 5 × 10⁴ cm^-3. Upper right: kinetic temperature averaged over the 90% confidence interval of each model. The black contours are at 5, 10, 20 K and the white contours at 40 and 60 K. Lower left: pressure averaged over the 90% confidence interval of each model. The black contours are at 10^4.7, 10^4.9, 10^5.1 and 10^5.3 K cm^-3 and the white contours at 10^5.5 and 10^5.7 K cm^-3. Lower right: goodness-of-fit with the same contours as in Fig. 18.

The upper panels show the CO integrated maps produced by the flared disk toy model described in Appendix A.1. The CO(3–2) emission is shown in greyscale, and the CO(1–0) (left panel) and CO(2–1) emission (right panel) are contours. The lower left and right panels show the resulting R₂₁ and R₃₂ maps, respectively.

The upper panels show the CO integrated maps produced by the clumpy flared disk toy model described in Appendix A.2. The CO(3–2) emission is shown in greyscale, and the CO(1–0) (left panel) and CO(2–1) emission (right panel) are contours. The lower left and right panels show the resulting R₂₁ and R₃₂ maps, respectively.