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Fig. 10

image

a) Radial distribution of the spectral line intensities (normalized using the number of H i spaxels in each RG-bin as measure of the sampled volume) of H i, [C ii] and its gas components (upper panel) and CO and its gas components (lower panel). b) Galactic distributions of warm H2 gas fraction, f(warm-H2): a) with respect to the total H2 gas (solid line); b) with respect to the total H i+H2 gas (dashed line); τ(H i) = 0 and 1.0 represent f(warm-H2) for optically thin and thick cases used for H i column densities, respectively. The variation of the H2 fractions as a functions of Galactocentric radius RG are representative of the star formation rate (SFR) and star formation efficiency (SFE).

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