[C II] 158 μm self-absorption and optical depth effects

@article{Guevara2020CI1,
title={[C II] 158 $\mu$m self-absorption and optical depth effects},
author={Cristian Guevara and J{\"u}rgen Stutzki and Volker Ossenkopf-Okada and Robert Simon and J. P. P'erez-Beaupuits and Henrik Beuther and Simon Bihr and R. Higgins and Urs U. Graf and Rolf Gusten},
journal={Astronomy \& Astrophysics},
year={2020}
}
• Published 28 February 2020
• Physics
• Astronomy & Astrophysics
Context. The [C II] 158 μm far-infrared fine-structure line is one of the most important cooling lines of the star-forming interstellar medium (ISM). It is used as a tracer of star formation efficiency in external galaxies and to study feedback effects in parental clouds. High spectral resolution observations have shown complex structures in the line profiles of the [C II] emission. Aims. Our aim is to determine whether the complex profiles observed in [12C II] are due to individual velocity…
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References

SHOWING 1-10 OF 88 REFERENCES

self-absorption and optical depth effects

• Physics
• 2020
Context. The [C ii] 158 μm far-infrared (FIR) fine-structure line is one of the most important cooling lines of the star-forming interstellar medium (ISM). It is used as a tracer of star formation

VELOCITY-RESOLVED [C ii] EMISSION AND [C ii]/FIR MAPPING ALONG ORION WITH HERSCHEL

• Physics
The Astrophysical journal
• 2015
It is concluded that the [C ii] emitting column relative to the total dust column along each line of sight is responsible for the observed L[C ii?]/LFIR variations through the cloud.

COLLISIONAL EXCITATION OF THE [C ii] FINE STRUCTURE TRANSITION IN INTERSTELLAR CLOUDS

• Physics
• 2012
We analyze the collisional excitation of the 158 μm (1900.5 GHz) fine structure transition of ionized carbon in terms of line intensities produced by simple cloud models. The single C+ fine structure

The optical depth of the 158 micron forbidden C-12 II line - Detection of the F = 1 - 0 forbidden C-13 II hyperfine-structure component. [in Orion nebula]

• Physics
• 1991
The detection of the F = 1 - 0 hyperfine component of the 158-micron forbidden C-13 II fine-structure line in the interstellar medium is reported. A 12-point intensity map was obtained of the

The ionized and hot gas in M17 SW: SOFIA/GREAT THz observations of [C II] and 12CO J=13-12

• Physics
• 2012
With new THz maps that cover an area of ~3.3x2.1 pc^2 we probe the spatial distribution and association of the ionized, neutral and molecular gas components in the M17 SW nebula. We used the dual

Herschel/HIFI observations of [C II] and [13C II] in photon-dominated regions

• Physics
• 2013
Context. Chemical fractionation reactions in the interstellar medium can result in molecular isotopologue abundance ratios that differ by many orders of magnitude from the isotopic abundance ratios.

[12Cii] and [13C ii] 158 μ m emission from NGC 2024: Large column densities of ionized carbon

• Physics
• 2012
Context. We analyse the NGC 2024 Hii region and molecular cloud interface using [ 12 Cii] and [ 13 Cii] observations. Aims. We attempt to gain insight into the physical structure of the interface

[C II] and [N II] from dense ionized regions in the Galaxy

• Physics
• 2016
The interstellar medium (ISM) consists of highly ionized and neutral atomic, as well as molecular, components. Knowledge of their distribution is important for tracing the structure and lifecycle of

Ionized gas at the edge of the Central Molecular Zone

• Physics
• 2015
To determine the properties of the ionized gas at the edge of the CMZ near Sgr E we observed a small portion of the edge of the CMZ near Sgr E with spectrally resolved [C II] 158 micron and [N II]

HERSCHEL GALACTIC PLANE SURVEY OF [N ii] FINE STRUCTURE EMISSION

• Physics
• 2015
We present the first large-scale high angular resolution survey of ionized nitrogen in the Galactic Plane through emission of its two fine structure transitions ([N ii]) at 122 and 205 μm. The