Volume 373, Number 1, July I 2001
|Page(s)||56 - 62|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 July 2001|
The oxygen abundance distribution in M 101
Main Astronomical Observatory of National Academy of Sciences of Ukraine, Goloseevo, 03680 Kiev-127, Ukraine
Corresponding author: L. S. Pilyugin, firstname.lastname@example.org
Accepted: 23 April 2001
The well-observed spiral galaxy M 101 was considered. The radial distributions of oxygen abundances determined in three different 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) abundance distribution. The parameters of the (O/H) abundance distribution differ significantly from those of the (O/H) abundance distribution: the central (O/H) 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) abundance distribution. The dispersion in (O/H)P abundance at fixed radius is rather small, ~0.08 dex, and is equal to that in (O/H) abundance. The dispersion in (O/H) abundance at fixed radius is appreciably larger, ~0.16 dex, compared to that in (O/H) abundance. It has been shown that the extra dispersion in (O/H) abundances is an artifact and reflects scatter in excitation parameter P at fixed radius.
Key words: galaxies: abundances / galaxies: ISM / galaxies: spiral / galaxies: individual: M 101
© ESO, 2001
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