Issue 
A&A
Volume 525, January 2011



Article Number  A18  
Number of page(s)  26  
Section  Extragalactic astronomy  
DOI  https://doi.org/10.1051/00046361/200912723  
Published online  26 November 2010 
Online material
Fig. 1
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^{h}36^{m}49.8^{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. 

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Fig. 5
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^{h}56^{m}43.76^{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. 

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Fig. 16
Likelihood of all possible (R_{21}, R_{32}) pairs on a R_{32}vs.R_{21} grid for different values of X_{CO}/(dV/dR). The contours of the R_{32}vs.R_{21} 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). 

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Fig. 17
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 1σ 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 densitytemperature 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). 

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Fig. 18
LVG result maps for NGC 4569. Upper left: H_{2} number density averaged over the 90% confidence interval of each LVG model. The black contours are at 5 × 10^{2}, 10^{3}, 3 × 10^{3} cm^{3} and the white contours at 5.5 × 10^{3}, 10^{4}, and 5 × 10^{4} 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 10^{5}, 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. 

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Fig. 19
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. 

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Fig. 20
LVG result maps for NGC 4826. Upper left: H_{2} number density averaged over the 90% confidence interval of each LVG model. The black contours are at 10^{3} and 5 × 10^{3} cm^{3} and the white contours at 10^{4} and 5 × 10^{4} 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: goodnessoffit with the same contours as in Fig. 18. 

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Fig. 23
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 R_{21} and R_{32} maps, respectively. 

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Fig. 24
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 R_{21} and R_{32} maps, respectively. 

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© ESO, 2010
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