The oxygen abundance gradient in M101: the reliability of the P method

Abstract

We present the oxygen abundance determination for 90 HII regions in the inner parts of the grand design galaxy M101. The abundances were derived employing the P method (Pilyugin 2001a). A comparison is made with previous determinations using another calibration and direct measurements of electron temperature to derive the oxygen abundance. The results show agreement with the abundances derived from the electron temperature method and also show that the older calibration is not as accurate as the P method.

arXiv comment4 pages, 3 figures. Accepted for publication in A&A

References in corpus (7)

• Using Strong Lines to Estimate Abundances in Extragalactic HII Regions and Starburst Galaxies
• The Composition Gradient in M101 Revisited. II. Electron Temperatures and Implications for the Nebular Abundance Scale
• On the oxygen abundance determination in HII regions: High - metallicity regions
• Chemical composition of B-type supergiants in the OB8, OB10, OB48, OB78 associations of M31
• Chemical abundances and winds of massive stars in M31: a B-type supergiant and a WC star in OB10
• The oxygen abundance distribution in M101
• Differential O and Si Abundances in M33 Early B Supergiants

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