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Spectroscopy of high-Z ions as a way to understanding the nature of Cas A knots and intergalactic shocks

Hyperfine structure lines of highly-charged ions may open a new window in observations of hot rarefied astrophysical plasmas. In this paper we discuss spectral lines of isotopes and ions abundant at temperatures 10 − 10 K, characteristic for warm-hot intergalactic medium, hot interstellar medium, starburst galaxies, their superwinds and young supernova remnants. Observations of these lines will allow to study bulk and turbulent motions of the observed target and will broaden the information about the gas ionization state, chemical and isotopic composition. The most prospective is the line of the major nitrogen isotope having wavelength λ = 5.65 mm (Sunyaev & Churazov, 1984). Wavelength of this line is well-suited for observation of objects at z ≈ 0.15− 0.6 when it is redshifted to 6.5− 9 mm spectral band widely-used in ground-based radio observations, and, for example, for z ≥ 1.3, when the line can be observed in 1.3 cm band and at lower frequencies. Modern and future radio telescopes and interferometers are able to observe the absorption by N VII in the warmhot intergalactic medium at redshifts above z ≈ 0.15 in spectra of brightest mm-band sources. Sub-millimeter emission lines of several most abundant isotopes having hyperfine splitting might also be detected in spectra of young supernova remnants. PACS: 32.10.Fn, 98.62.Ra, 98.38.-j, 98.58.-w, 32.30.Bv