Abstract
The well-observed spiral galaxy M 101 was considered. The radial distributions of oxygen abundances determined in three dierent ways (with the classic Te{method, with the R23{method, and with the P {method) were compared. It was found that the parameters (the central oxygen abundance and the gradient) of the radial (O/H)P abundance distribution are close to those of the (O/H)Te abundance distribution. The parameters of the (O/H)R23 abundance distribution dier signicantly from those of the (O/H)Te abundance distribution: the central (O/H)R23 oxygen abundance is higher by around 0.4 dex and the gradient is steeper by a factor of around 1.5 as compared to those values in the (O/H)Te abundance distribution. The dispersion in (O/H)P abundance at xed radius is rather small,0.08 dex, and is equal to that in (O/H)Te abundance. The dispersion in (O/H)R23 abundance at xed radius is appreciably larger,0.16 dex, compared to that in (O/H)Te abundance. It has been shown that the extra dispersion in (O/H)R23 abundances is an artifact and reflects scatter in excitation parameter P at xed radius.
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