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Atomic Physics Calculations for Iron L-line Spectra

Published online by Cambridge University Press:  30 March 2016

Jacques Dubau ,
Delphine Porquet  and
Oleg Zabaydullin
Jacques Dubau
Affiliation:
LIXAM, UMR8624, Université Paris-Sud, Bat. 350, 91405 Orsay Cedex, FranceLUTH, Observatoire de Paris, 5 Place J. Janssen, 92190 Meudon, France
Delphine Porquet
Affiliation:
Max-Plank-Institut für extraterrestrische Physik, Postfach 1312, D-85741, Garching, Germany
Oleg Zabaydullin
Affiliation:
Institute of Nuclear Fusion, Russian Research Center Kurchatov Institute, 123182 Moscow, Russia

Abstract

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Absorption L-lines of iron ions are observed, in spectra of Seyfert 1 galaxies by the new generation of X-ray satellites: Chandra and XMM-Newton. Lines associated to Fe 23+ to Fe16+ have been already observed in emission, in the solar corona and in laboratory. Whereas, those corresponding to Fe 15+ to Fe6+ have not been observed as emission lines, the upper level of the transition decaying preferentially by autoionization. Many atomic data are available for the first ion set. For the second set, some data have been recently published for n=2 to n’=3 transitions. We have recalculated them using another theoretical approach and have extended them to n’=4.

Type
I. Joint Discussions
Information
Highlights of Astronomy , Volume 13 , 2005 , pp. 627 - 629
Copyright
Copyright © Astronomical Society of Pacific 2005

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