Hostname: page-component-78c5997874-s2hrs Total loading time: 0 Render date: 2024-11-17T21:25:52.758Z Has data issue: false hasContentIssue false
  • English
  • Français

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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

References

Bregman, J. N. & Irwin, J. A. 2007, ApJ 666, 139CrossRefGoogle Scholar
Cen, R. & Fang, T. 2006 ApJ 650, 573CrossRefGoogle Scholar
Cen, R. & Ostriker, J. P. 1999 ApJ 514, 1CrossRefGoogle Scholar
Cen, R. & Ostriker, J. P. 2006 ApJ 650, 560CrossRefGoogle Scholar
Chen, X., Weinberg, D. H., Katz, N. & Davé, R. 2003 ApJ 594, 42CrossRefGoogle Scholar
Docenko, D. & Sunyaev, R. A. 2007a, in: Böhringer, H., Pratt, G. W., Finoguenov, A., & Schuecker, P. (eds.), Heating versus Cooling in Galaxies and Clusters of Galaxies, ESO Astrophysics Symposia (Berlin, Heidelberg: Springer), p. 333CrossRefGoogle Scholar
Docenko, D. & Sunyaev, R. A. 2007b, in: From Planets to Dark Energy: the Modern Radio Universe, Published online at SISSA, Proceedings of Science, p.90Google Scholar
Hellsten, U., Gnedin, N. Y., & Miralda-Escudé, J. 1998 ApJ 509, 56CrossRefGoogle Scholar
Shabaev, V. M., Shabaeva, M. B., & Tupitsyn, I. I. 1995, Phys. Rev. A 52, 3686CrossRefGoogle Scholar
Sunyaev, R. A. & Churazov, E. M. 1984, Soviet Astron. Lett. 10, 201Google Scholar
Sunyaev, R. A. & Docenko, D. O. 2007, Astron. Lett. 33, 67CrossRefGoogle Scholar
Vanden Bout, P. A., Solomon, P. M., & Maddalena, R. J. 2004 ApJ 614, L97CrossRefGoogle Scholar
Volotka, A. V., Glazov, D. A., Tupitsyn, I. I., Oreshkina, N. S., Plunien, G., & Shabaev, V. M. 2008 Phys. Rev. A 78, 062507CrossRefGoogle Scholar