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          Institute: MPI für extraterrestrische Physik     Collection: Infrared and Submillimeter Astronomy     Display Documents



ID: 12206.0, MPI für extraterrestrische Physik / Infrared and Submillimeter Astronomy
The excitation and metallicity of galactic HII regions from Infrared Space Observatory SWS observations of mid-infrared fine-structure lines
Authors:Giveon, Uriel; Sternberg, Amiel; Lutz, Dieter; Feuchtgruber, Helmut; Pauldrach, A. W. A.
Language:English
Date of Publication (YYYY-MM-DD):2002-02-20
Title of Journal:The Astrophysical Journal
Journal Abbrev.:Astrophys. J
Volume:566
Issue / Number:2
Start Page:880
End Page:897
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:We present mid-infrared Infrared Space Observatory Short- Wavelength Spectrometer (ISO-SWS) observations of the fine- structure emissions lines [Ne II] 12.8 mum, [Ne III] 15.6 mum, [Ne III] 36.0 mum, [Ar II] 6.99 mum, [Ar III] 8.99 mum, [S III] 18.7 mum, [S III] 33.5 mum, and [S IV] 10.5 mum and the recombination lines Bralpha and Brbeta in a sample of 112 Galactic H II regions and 37 nearby extra-Galactic H II regions in the LMC, SMC, and M33. We selected our sources from archival ISO-SWS data as those showing prominent [Ne II] 12.8 mum or [Ne III] 15.6 mum emissions. The Galactic sources have a wide range in galactocentric distance (0 kpc less than or similar to R-gal less than or similar to 18 kpc), which enables us to study excitation and metallicity variations over large Galactic scales. We detect a steep rise in the [Ne III] 15.6 mum/[Ne II] 12.8 mum, [Ar III] 8.99 mum/[Ar II] 6.99 mum, and [S IV] 10.5 mum/[S III] 33.5 mum excitation ratios from the inner Galaxy outward, and a moderate decrease in metallicity, from similar to2 Z. in the inner Galaxy to similar to1 Z. in the outer disk. The extra-Galactic sources in our sample show low gas density, low metallicity, and high excitation. We find a good correlation between [Ne III] 15.6 mum/[Ne II] 12.8 mum and [Ar III] 8.99 mum/[Ar II] 6.99 mum excitation ratios in our sample. The observed correlation is well reproduced by theoretical nebular models that incorporate new-generation wind-driven non- LTE model stellar atmospheres for the photoionizing stars. In particular, the non-LTE atmospheres can account for the production of [Ne III] emission in the H II regions. We have computed self-consistent nebular and stellar atmosphere models for a range of metallicities (0.5-2 Z.). We conclude that the increase in nebular excitation with galactocentric radius is due to an increase in stellar effective temperature (as opposed to a hardening of the stellar spectral energy distributions due to the metallicity gradient). We estimate an integrated [Ne III] 15.6 mum/[Ne II] 12.8 mum ratio for the Galaxy of 0.8, which puts it well inside the range of values for starburst galaxies. The good fit between observations and our models support the conclusion of Thornley and coworkers that the low [Ne III] 15.6 mum/[Ne II] 12.8 mum ratios observed in extra- Galactic sources are due to global aging effects.
Free Keywords:galaxies : individual (M33); Galaxy : abundances; Galaxy : stellar content; HII regions; Magellanic Clouds; stars : atmospheres
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für extraterrestrische Physik
External Affiliations:Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch; Phys & Astron, IL-69978 Tel Aviv, Israel; Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel; Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Wise Observ, IL-69978 Tel Aviv, Israel; Max Planck Inst Extraterr Phys, D-85748 Garching, Germany; Univ Munich, Inst Astron & Astrophys, D-81679 Munich, Germany
Identifiers:ISI:000173804900025
ISSN:0004-637X
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