'Counterpart' method for abundance determinations in H ii regions
Abstract We suggest a new way of determining abundances and electron temperatures in H ii regions from strong emission lines. Our approach is based on the standard assumption that H ii regions with similar intensities of strong emission lines have similar physical properties and abundances. A '...
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Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2012-08, Vol.424 (3), p.2316-2329 |
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Format: | Artikel |
Sprache: | eng |
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Zusammenfassung: | Abstract
We suggest a new way of determining abundances and electron temperatures in H ii regions from strong emission lines. Our approach is based on the standard assumption that H ii regions with similar intensities of strong emission lines have similar physical properties and abundances. A 'counterpart' for a studied H ii region may be chosen among H ii regions with well-measured abundances (reference H ii regions) by comparison of carefully chosen combinations of strong-line intensities. Then the abundances in the investigated H ii region can be assumed to be the same as those in its counterpart. In other words, we suggest to determine the abundances in H ii regions 'by precedent'. To get more reliable abundances for the considered H ii region, a number of reference H ii regions are selected and then the abundances in the target H ii region are estimated through extrapolation/interpolation. We will refer to this method of abundance determination as the counterpart method or, for brevity, the C method. We define a sample of reference H ii regions and verify the validity of the C method. We find that this method produces reliable abundances. Finally, the C method is used to obtain the radial abundance distributions in the extended discs of the spiral galaxies M83, NGC 4625 and NGC 628. |
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ISSN: | 0035-8711 1365-2966 |
DOI: | 10.1111/j.1365-2966.2012.21398.x |