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7.7. A search for [Ne II] 12.8 micron line emission from Galactic ultracompact H II regions

Published online by Cambridge University Press:  25 May 2016

H. Matsuhara ,
H. Takahashi  and
H. Watarai
H. Matsuhara
Affiliation:
Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-01, Japan
H. Takahashi
Affiliation:
Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-01, Japan
H. Watarai
Affiliation:
Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-01, Japan

Extract

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Starburst galaxies are powered by newly formed massive stars, and are heavily obscured by dust, prohibiting the UV and optical studies. A fine-structure line from Ne+ ion ([Ne II] 12.8 μm) is usually the brightest mid-infrared(MIR) line emitted from starburst galaxies. The [Ne II] line suffers from far less dust extinction than the optical line does, and hence it is often used as a probe for starburst properties of galaxies(Achtermann & Lacy, 1995; Roche et al., 1991). However, the [Ne II] line should not be used as the physical probe unless the relationship between Ne+ abundance and spectral type of the ionizing star is established for very dusty H II regions. To study this, we started the [Ne II] line survey toward dusty ultracompact(UC) H II regions in our Galaxy. The UC H II regions are powered by newly formed early-type stars whose spectral type can be inferred from their radio and far-infrared(FIR) properties.

Type
Part II. Nuclear Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 305 - 306
Copyright
Copyright © Kluwer 1998 

References

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