Optical Recombination Lines of Heavy-elements in Giant Extragalactic HII Regions

Details Optical Recombination Lines of Heavy-elements in Giant Extragalactic HII Regions Optical Recombination Lines of Heavy-elements in Giant Extragalactic HII Regions

2002-08-16

arxiv.org/abs/astro-ph/0208313v1

Astrophys.J. 581 (2002) 241-257

Astronomy and Astrophysics

Astrophysics

42 pages, 5 figures. To be published in ApJ

Scientific paper

10.1086/344104

We present high resolution observations of the giant extragalactic H II regions NGC 604, NGC 2363, NGC 5461 and NGC 5471, based on observations taken with the ISIS spectrograph on the William Herschel Telescope. We have detected -by the first time- C II and O II recombination lines in these objects. We find that recombination lines give larger C^{++} and O^{++} abundances than collisionallly excited lines, suggesting that temperature variations can be present in the objects. We detect [Fe IV] lines in NGC 2363 and NGC 5471, the most confident detection of optical lines of this kind in H II regions. Considering the temperature structure we derive their H, He, C, N, O, Ne, S, Ar, and Fe abundances. From the recombination lines of NGC 5461 and NGC 5471 we determine the presence of C/H and O/H gradients in M101. We calculate the Delta Y/Delta O and Delta Y/Delta Z values considering the presence of temperature variations and under the assumption of constant temperature. We obtain a better agreement with models of galactic chemical evolution by considering the presence of temperature variations than by assuming that the temperature is constant in these nebulae.

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