Far-infrared mapping of the double-lobed H II region S106

1982 ◽  
Vol 258 ◽  
pp. 568 ◽  
Author(s):  
P. M. Harvey ◽  
I. Gatley ◽  
H. A., Jr. Thronson ◽  
M. W. Werner
Keyword(s):  
Far Infrared ◽  
H Ii Region

scholarly journals An extensive study of interstellar matter in the IC 1396 region using several molecular lines and transitions of CO and far-infrared maps from IRAS

1991 ◽  
Vol 147 ◽  
pp. 513-514
Author(s):  
H. Weikard ◽  
K. Sugitani ◽  
G. Duvert ◽  
M. Miller
Keyword(s):  
Molecular Clouds ◽  
Far Infrared ◽  
Extensive Study ◽  
Interstellar Matter ◽  
Molecular Lines ◽  
H Ii Region

IC 1396 is an H II region in Cepheus excited by the massive 06.5 star HD 206267. The distance is about 750 pc. The region exhibits a number of bright-rimmed molecular clouds in which outflows have been detected (Sugitani et al. 1989, Duvert et al. 1990).

Far-infrared observations of M17 - The interaction of an H II region with a molecular cloud

1979 ◽  
Vol 233 ◽  
pp. 575 ◽  
Author(s):  
I. Gatley ◽  
E. E. Becklin ◽  
K. Sellgren ◽  
M. W. Werner
Keyword(s):  
Molecular Cloud ◽  
Far Infrared ◽  
Infrared Observations ◽  
H Ii Region

scholarly journals 3D structure of the H ii region Sh2-235 from tunable-filter optical observations

2020 ◽  
Vol 497 (1) ◽  
pp. 1050-1058 ◽  
Author(s):  
M S Kirsanova ◽  
P A Boley ◽  
A V Moiseev ◽  
D S Wiebe ◽  
R I Uklein
Keyword(s):  
Column Density ◽  
3D Structure ◽  
Far Infrared ◽  
Tunable Filter ◽  
Optical Observations ◽  
Special Astrophysical Observatory ◽  
Neutral Medium ◽  
Neutral Material ◽  
H Ii Region ◽  
Academy Of Sciences

ABSTRACT We present observations of the H α, H β, [S ii] λλ6716, 6731 and [N ii] λ6583 emission lines in the galactic H ii region Sh2-235 with the Mapper of Narrow Galaxy Lines (MaNGaL), a tunable filter at the 1-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. We show that the H ii region is obscured by neutral material with AV ≈ 2−4 mag. The area with the highest AV is situated to the south-west from the ionizing star and coincides with a maximum detected electron density of ≳300 cm−3. The combination of these results with archive AKARI far-infrared data allows us to estimate the contribution of the front and rear walls to the total column density of neutral material in S235 and explain the 3D structure of the region. The H ii region consist of a denser, more compact portion deeply embedded in the neutral medium and the less dense and obscured gas. The front and rear walls of the H ii region are inhomogeneous, with the material in the rear wall having a higher column density. We find a two-sided photodissociation region in the dense clump S235 East 1, illuminated by a UV field with G0 = 50−70 and 200 Habing units in the western and eastern parts, respectively.

High resolution far-infrared observations of the evolved H II region M16

1982 ◽  
Vol 254 ◽  
pp. 126 ◽  
Author(s):  
B. McBreen ◽  
G. G. Fazio ◽  
D. T. Jaffe
Keyword(s):  
High Resolution ◽  
Far Infrared ◽  
Infrared Observations ◽  
H Ii Region

scholarly journals The Peculiar Planetary Nebula M1-78

1989 ◽  
Vol 131 ◽  
pp. 216-216
Author(s):  
S. R. Pottasch ◽  
A. A. Zijlstra ◽  
N. Ukita ◽  
A. Manchado ◽  
M. Ratag
Keyword(s):  
High Resolution ◽  
Planetary Nebula ◽  
Far Infrared ◽  
Radio Continuum ◽  
Continuum Emission ◽  
Spectral Information ◽  
Low Oxygen ◽  
H Ii Region ◽  
Infrared Continuum ◽  
Absorption Measurements

The question of whether M1-78 is a PN or a compact H II region is discussed. We have obtained new high resolution radio continuum maps, optical spectra and CO maps. Arguments for it being a PN include spectral information, far infrared continuum emission, and radio morphology. It is the strongest CO emitting PN known. Its abundances are peculiar: high helium and very low oxygen and nitrogen abundances. If it is a PN it must be within 4 kpc, but 21-cm absorption measurements indicate that it may be further away.

scholarly journals Molecular envelope around the HII region RCW 120

2019 ◽  
Vol 488 (4) ◽  
pp. 5641-5650 ◽  
Author(s):  
M S Kirsanova ◽  
Ya N Pavlyuchenkov ◽  
D S Wiebe ◽  
P A Boley ◽  
S V Salii ◽  
...  
Keyword(s):  
Dust Emission ◽  
Far Infrared ◽  
Theoretical Models ◽  
Interstellar Extinction ◽  
Hii Region ◽  
Band Form ◽  
H Ii Region ◽  
Dust Dynamics ◽  
Molecular Envelope ◽  
2D Model

ABSTRACT The H ii region RCW 120 is a well-known object, which is often considered as a target to verify theoretical models of gas and dust dynamics in the interstellar medium. However, the exact geometry of RCW 120 is still a matter of debate. In this work, we analyse observational data on molecular emission in RCW 120 and show that 13CO(2–1) and C18O(2–1) lines are fitted by a 2D model representing a ring-like face-on structure. The changing of the C18O(3–2) line profile from double-peaked to single-peaked from the dense molecular Condensation 1 might be a signature of stalled expansion in this direction. In order to explain a self-absorption dip of the 13CO(2–1) and 13CO(3–2) lines, we suggest that RCW 120 is surrounded by a diffuse molecular cloud, and find confirmation of this cloud on a map of interstellar extinction. Optically thick 13CO(2–1) emission and the infrared 8 $\mu$m PAH band form a neutral envelope of the H ii region resembling a ring, while the envelope breaks into separate clumps on images made with optically thin C18O(2–1) line and far-infrared dust emission.

scholarly journals An extensive study of interstellar matter in the IC 1396 region using several molecular lines and transitions of CO and far-infrared maps from IRAS

1991 ◽  
Vol 147 ◽  
pp. 513-514
Author(s):  
H. Weikard ◽  
K. Sugitani ◽  
G. Duvert ◽  
M. Miller
Keyword(s):  
Molecular Clouds ◽  
Far Infrared ◽  
Extensive Study ◽  
Interstellar Matter ◽  
Molecular Lines ◽  
H Ii Region

IC 1396 is an H II region in Cepheus excited by the massive 06.5 star HD 206267. The distance is about 750 pc. The region exhibits a number of bright-rimmed molecular clouds in which outflows have been detected (Sugitani et al. 1989, Duvert et al. 1990).

scholarly journals Electron Density and Nitrogen Abundance from FIR Lines

1993 ◽  
Vol 155 ◽  
pp. 183-183
Author(s):  
R.H. Rubin ◽  
S.W.J. Colgan ◽  
E.F. Erickson ◽  
M.R. Haas ◽  
S.D. Lord ◽  
...  
Keyword(s):  
Electron Density ◽  
Spectral Region ◽  
Far Infrared ◽  
Ionic Species ◽  
Empirical Method ◽  
Total N ◽  
Elemental Abundances ◽  
Nitrogen Abundance ◽  
H Ii Region ◽  
Semi Empirical

In order to study the physical properties of nebulae and determine their elemental abundances, it is important to observe lines from many different ionic species. Such studies have been enhanced in recent years with the measurement of lines in the far-infrared (FIR). The [N III]57μm line provides a way to assess the N++ abundance – which is not readily done from any other spectral region. Recent detection of the [N II]122 and 205μm lines provides a new way to assess both the electron density in the N+ region and the total N abundance in an object. When there are few observations to warrant a detailed modeling approach, it may be necessary to use another approach which has been referred to as a semi-empirical method (hereafter SEM) (e.g. Aller 1984). We delineate a SEM scheme for doing this and apply it to observations for the H II region G333.6–0.2.

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