Collisional excitation of the [c ii] fine structure transition in interstellar clouds
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In this paper, the collisional excitation of the [C II] line of ionized carbon in terms of line intensities produced by simple cloud models has been analyzed and derived for several limiting cases and carried out numerical solutions using a large velocity gradient model for more inclusive analysis.Abstract:
We analyze the collisional excitation of the 158 {mu}m (1900.5 GHz) fine structure transition of ionized carbon in terms of line intensities produced by simple cloud models. The single C{sup +} fine structure transition is a very important coolant of the atomic interstellar medium (ISM) and of photon-dominated regions in which carbon is partially or completely in ionized form. The [C II] line is widely used as a tracer of star formation in the Milky Way and other galaxies. Excitation of the [C II] fine structure transition can be via collisions with hydrogen molecules, atoms, and electrons. Analysis of [C II] observations is complicated by the fact that it is difficult to determine the optical depth of the line. We discuss the excitation of the [C II] line, deriving analytic results for several limiting cases and carry out numerical solutions using a large velocity gradient model for a more inclusive analysis. For antenna temperatures up to 1/3 of the brightness temperature of the gas kinetic temperature, the antenna temperature is linearly proportional to the column density of C{sup +} irrespective of the optical depth of the transition. This is appropriately referred to as the effectively optically thin approximation. We reviewmore » the critical densities for excitation of the [C II] line by various collision partners, briefly analyze C{sup +} absorption, and conclude with a discussion of C{sup +} cooling and how the considerations for line intensities affect the behavior of this important coolant of the ISM.« lessread more
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TL;DR: The Heterodyne Instrument for the Far-Infrared (HIFI) was launched onboard ESA's Herschel Space Observatory in May 2009 as mentioned in this paper, which is a set of 7 heterodyne receivers that are electronically tuneable, covering 480-1250 GHz with SIS mixers and the 1410-1910 GHz range with hot electron bolometer mixers.
Journal ArticleDOI
Far-Infrared Spectroscopy of Normal Galaxies: Physical Conditions in the Interstellar Medium
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