The radial metallicity gradient and the history of elemental enrichment in M 81 through emission-line probes

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Fig. 8

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Oxygen vs. galactocentric distance in HII regions of M 81 as in Fig. 5 (bottom panel), but including the Patterson et al. (2012) weak-line abundances (diamonds). The line corresponds to the gradient for R_G < 16 kpc, including the data from Patterson et al. (2012) with R_G < 16.

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