SIMBAD references

2001A&A...369..594P - Astronomy and Astrophysics, volume 369, 594-604 (2001/4-2)

On the oxygen abundance determination in HII regions. High-metallicity regions.

PILYUGIN L.S.

Abstract (from CDS):

This is our second paper devoted to the problem of line intensity - oxygen abundance calibration starting from the idea of McGaugh (1991ApJ...380..140M) that the strong oxygen lines ([OII] λλ3727, 3729 and [OIII] λλ4959, 5007) contain the necessary information to determine accurate abundances in HII regions. In the previous study (Pilyugin, 2000) the corresponding relations were obtained for the low-metallicity HII regions (12+logO/H≤7.95, the lower branch of the O/H-R23 diagram). The high-metallicity HII regions (12+logO/H≥8.2, the upper branch of the O/H-R23 diagram) are considered in the present study. A relation of the type O/H=f(P, R23) between oxygen abundance and the value of abundance index R23, introduced by Pagel et al. (1979MNRAS.189...95P), and the excitation parameter P (which is defined here as the contribution of the radiation in [OIII] λλ4959, 5007 lines to the ``total" oxygen radiation) has been derived empirically using the available oxygen abundances determined via measurement of a temperature-sensitive line ratio [OIII]4959,5007/[OIII]4363 (Te-method). By comparing oxygen abundances in high-metallicity HII regions derived with the Te-method and those derived with the suggested relations (P-method), it was found that the precision of oxygen abundance determination with the P-method is around 0.1dex (the mean difference for the 38 HII regions considered is ∼0.08 dex) and is comparable to that of the Te-method. A relation of the type Te=f(P, R23) between electron temperature and the values of abundance index R23 and the excitation parameter P was derived empirically using the available electron temperatures determined via measurement of temperature-sensitive line ratios. The maximum value of differences between electron temperatures determined via measurement of temperature-sensitive line ratios and those derived with the suggested relation is around 1000K for HII regions considered here, the mean value of differences for 38 HII regions is ∼500K, which is the same order of magnitude as the uncertainties of electron temperature determinations in high-metallicity HII regions via measured temperature-sensitive line ratios.

Abstract Copyright:

Journal keyword(s): ISM: HII regions - galaxies: abundances - galaxies: ISM - galaxies: spiral

CDS comments: Table 1: C6w aperture not HII region

Simbad objects: 47

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2019.09.16-03:05:48

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