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An analysis of electron distributions in galaxy clusters by means of the flux ratio of iron lines FeXXV and XXVI
Univ Paris 06, CNRS, France ; Moscow Inst Phys & Technol, Russia.ORCID iD: 0000-0001-6511-4330
Univ Paris 06, CNRS, France.
PN Lebedev Phys Inst, Russia.
INAF Osservatorio Astron Roma, Italy.
2009 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 496, no 1, p. 25-30Article in journal (Refereed) Published
Abstract [en]

Aims The interpretation of hard X-ray emission from galaxy clusters is still ambiguous and different proposed models can be probed using various observational methods. Here we explore a new method based on Fe-line observations. Methods. Spectral-line emissivities have usually been calculated by assuming a Maxwellian electron distribution. In this paper, a generalized approach to calculating the iron-line flux for a modified Maxwellian distribution is considered. Results. We calculated the flux ratio of iron lines for various possible populations of electrons proposed to account for measurements of hard X-ray excess-emission from the clusters A2199 and Coma. We found that the influence of the suprathermal electron population on the flux ratio is more significant in low temperature clusters (as Abell 2199) than in high temperature clusters (as Coma).

Place, publisher, year, edition, pages
2009. Vol. 496, no 1, p. 25-30
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
URN: urn:nbn:se:lnu:diva-42860DOI: 10.1051/0004-6361/200811095ISI: 000264404800003OAI: oai:DiVA.org:lnu-42860DiVA, id: diva2:807506
Available from: 2015-04-23 Created: 2015-04-23 Last updated: 2017-12-04Bibliographically approved

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Prokhorov, Dmitry

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