H2 infrared line emission from S140: A warm PDR

R. Timmermann; F. Bertoldi; C. M. Wright; S. Drapatz; B. T. Draine; L. Haser; A. Sternberg

H₂ infrared line emission from S140: A warm PDR

R. Timmermann, F. Bertoldi, C. M. Wright, S. Drapatz, B. T. Draine, L. Haser, A. Sternberg

Astrophysical Sciences

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59 Scopus citations

Abstract

ISO SWS spectra of H₂ pure rotational and rovibrational transitions, as well as [FeII], and [SiII] fine structure lines were obtained for one position on the photodissociation region (PDR) adjacent to the bright rim of the S140 HII region. The gas density is ≈ 10⁴ cm^-3 and the incident UV flux χ ≈ 400 at the location of the ionization front. Our PDR model analysis shows that the relative H₂ line intensities are characteristic of low-density fluorescent emission and that the gas temperature is T > 500K in the partially dissociated gas. A comparison of predicted and observed fine structure line intensities permits an estimate of the abundances of Fe and Si.

Original language	English (US)
Pages (from-to)	L281-L284
Journal	Astronomy and Astrophysics
Volume	315
Issue number	2
State	Published - Nov 10 1996

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Abundances
HII regions
ISM: individual: S140
Infrared: ISM: lines and bands
Molecules
Reflection nebulae

Cite this

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title = "H2 infrared line emission from S140: A warm PDR",

abstract = "ISO SWS spectra of H2 pure rotational and rovibrational transitions, as well as [FeII], and [SiII] fine structure lines were obtained for one position on the photodissociation region (PDR) adjacent to the bright rim of the S140 HII region. The gas density is ≈ 104 cm-3 and the incident UV flux χ ≈ 400 at the location of the ionization front. Our PDR model analysis shows that the relative H2 line intensities are characteristic of low-density fluorescent emission and that the gas temperature is T > 500K in the partially dissociated gas. A comparison of predicted and observed fine structure line intensities permits an estimate of the abundances of Fe and Si.",

keywords = "Abundances, HII regions, ISM: individual: S140, Infrared: ISM: lines and bands, Molecules, Reflection nebulae",

author = "R. Timmermann and F. Bertoldi and Wright, {C. M.} and S. Drapatz and Draine, {B. T.} and L. Haser and A. Sternberg",

year = "1996",

month = nov,

day = "10",

language = "English (US)",

volume = "315",

pages = "L281--L284",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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TY - JOUR

T1 - H2 infrared line emission from S140

T2 - A warm PDR

AU - Timmermann, R.

AU - Bertoldi, F.

AU - Wright, C. M.

AU - Drapatz, S.

AU - Draine, B. T.

AU - Haser, L.

AU - Sternberg, A.

PY - 1996/11/10

Y1 - 1996/11/10

N2 - ISO SWS spectra of H2 pure rotational and rovibrational transitions, as well as [FeII], and [SiII] fine structure lines were obtained for one position on the photodissociation region (PDR) adjacent to the bright rim of the S140 HII region. The gas density is ≈ 104 cm-3 and the incident UV flux χ ≈ 400 at the location of the ionization front. Our PDR model analysis shows that the relative H2 line intensities are characteristic of low-density fluorescent emission and that the gas temperature is T > 500K in the partially dissociated gas. A comparison of predicted and observed fine structure line intensities permits an estimate of the abundances of Fe and Si.

AB - ISO SWS spectra of H2 pure rotational and rovibrational transitions, as well as [FeII], and [SiII] fine structure lines were obtained for one position on the photodissociation region (PDR) adjacent to the bright rim of the S140 HII region. The gas density is ≈ 104 cm-3 and the incident UV flux χ ≈ 400 at the location of the ionization front. Our PDR model analysis shows that the relative H2 line intensities are characteristic of low-density fluorescent emission and that the gas temperature is T > 500K in the partially dissociated gas. A comparison of predicted and observed fine structure line intensities permits an estimate of the abundances of Fe and Si.

KW - Abundances

KW - HII regions

KW - ISM: individual: S140

KW - Infrared: ISM: lines and bands

KW - Molecules

KW - Reflection nebulae

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M3 - Article

AN - SCOPUS:0000380063

SN - 0004-6361

VL - 315

SP - L281-L284

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 2

ER -

H₂ infrared line emission from S140: A warm PDR

Abstract

All Science Journal Classification (ASJC) codes

Keywords

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