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Possibility of measuring the amount of intergalactic metals with 14N VII HFS line

Published online by Cambridge University Press:  09 March 2010

Dmitrijs Docenko  and
Rashid A. Sunyaev
Dmitrijs Docenko
Affiliation:
Institute of Astronomy, University of Latvia, Rainis blvd. 19, Riga, LV-1586, Latvia email: dima@latnet.lv
Rashid A. Sunyaev
Affiliation:
Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, Postfach 1317, 85741 Garching, Germany email: sunyaev@mpa-garching.mpg.de Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, 117997 Moscow, Russia
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Abstract

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We discuss possibility of observations of the warm-hot intergalactic medium using the hyperfine structure line of highly charged nitrogen ion 14N VII (rest wavelength λ = 5.652 mm). Observations of this line will allow to separate bulk and turbulent motions in the observed target and will broaden the information about the gas ionization state, chemical and isotopic composition.

Wavelength of this line is well-suited for ground-based observation of objects at z ≈ 0.15 − 0.6 when it is redshifted to the widely-used 6.5 − 9 mm spectral band, and, for example, for z ≥ 1.3, when the line can be observed in 1.3 cm band and at lower frequencies.

Keywords

galaxies: intergalactic medium - radio lines: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 167 - 170
Copyright
Copyright © International Astronomical Union 2010

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