Hydrogen-like nitrogen radio line from hot interstellar and warm-hot intergalactic gas |
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Authors: | R A Sunyaev D O Docenko |
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Institution: | (1) Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Postfach 1317, 85741 Garching, Germany;(2) Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117810, Russia |
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Abstract: | The hyperfine-structure lines of highly charged ions may allow one to look at hot rarefied astrophysical plasmas from a new
perspective. In this paper, we discuss the spectral lines of ions and isotopes abundant at temperatures 105–107 K characteristic of a warm-hot intergalactic gas, a hot interstellar medium, starburst galaxies, their superwinds, and young
supernova remnants. Observations of these lines will make it possible to study the bulk and turbulent motions in the observed
objects and will supplement the information about the ionization state and chemical and isotopic compositions of the gas.
The line of the main nitrogen isotope with wavelength λ = 5.65 mm is of particular interest. The wavelength of this line is
well suited for observations of objects at z ≈ 0.15−0.6, when it is redshifted to the spectral range 6.5–9 mm widely used in ground-based radio observations, and, for
example, for z ≥ 1.3, when the line is redshifted to 1.3 cm or farther. Modern and future radio telescopes and interferometers are capable
of observing the 14N VII absorption by the warm-hot intergalactic gas at redshifts higher than z ≈ 0.15 in the spectra of the brightest millimeter-band sources. The submillimeter emission lines of the most abundant isotopes
with hyperfine splitting may also be detected in the spectra of young supernova remnants.
The article was translated by the authors. |
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Keywords: | hyperfine structure intergalactic gas supernova remnants radio lines |
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