Chemical Abundances and Ionizing Clusters of HII Regions in the LINER Galaxy NGC 4258

Details Chemical Abundances and Ionizing Clusters of HII Regions in the LINER Galaxy NGC 4258 Chemical Abundances and Ionizing Clusters of HII Regions in the LINER Galaxy NGC 4258

2000-06-14

arxiv.org/abs/astro-ph/0006193v1

Mon.Not.Roy.Astron.Soc. 318 (2000) 462

Astronomy and Astrophysics

Astrophysics

16 pages, 16 figures. To appear in MNRAS

Scientific paper

We present long-slit observations in the optical and near infrared of eight HII regions in the spiral galaxy NGC 4258. Six of the observed regions are located in the SE inner spiral arms and the other two are isolated in the northern outer arms. A detailed analysis of the physical conditions of the gas has been performed. For two of the regions, an electron temperature has been derived from the [SIII] 6312 A line. For the rest, an empirical calibration based on the red and near infrared sulphur lines has been used. The oxygen abundances derived by both methods are found to be significantly lower (by a factor of two) than previously derived by using empirical calibrations based on the optical oxygen lines. In the brightest region, 74C, the observation of a prominent feature due to Wolf-Rayet stars provides an excellent constraint over some properties of the ionizing clusters. In the light of the current evolutionary synthesis models, no consistent solution is found to explain at the same time both the WR feature characteristics and the emission line spectrum of this region. In principle, the presence of WR stars could lead to large temperature fluctuations and also to a hardening of the ionizing radiation. None of these effects are found in region 74C for which the electron temperatures found from the [SIII] 6312A and the Paschen discontinuity at 8200A are equal within the errors and the effective temperature of the ionizing radiation is estimated at around 35,300K. Both more observations of confirmed high metallicity regions and a finer metallicity grid for the evolutionary synthesis models are needed in order to understand the ionizing populations of HII regions.

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