EDP Sciences
Free Access
Volume 432, Number 3, March IV 2005
Page(s) 1137 - 1150
Section Atomic, molecular and nuclear data
DOI https://doi.org/10.1051/0004-6361:20041849
Published online 07 March 2005

A&A 432, 1137-1150 (2005)
DOI: 10.1051/0004-6361:20041849

Benchmarking atomic data for astrophysics: $\ion{Fe}{xxiii}$

G. Del Zanna, M. C. Chidichimo and H. E. Mason

Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge CB3 0WA, UK
    e-mail: G.Del-Zanna@damtp.cam.ac.uk

(Received 16 August 2004 / Accepted 29 November 2004)

Recent scattering calculations for $\ion{Fe}{xxiii}$ are benchmarked against laboratory and astrophysical observations. The collisional data are supplemented by radiative data obtained with empirical adjustments that take into account observed wavelengths. All previous line identifications and energy levels are reviewed and assessed in light of these new calculations. Most of the previous identifications, in particular of the astrophysically-important spectral lines are confirmed. However, some identification are rejected or questioned, and new ones proposed. The agreement between theoretical and experimental data in terms of wavelengths, line intensities and level lifetimes is very good. Observations of $\ion{Fe}{xxiii}$ L-shell emission lines provide a great opportunity to directly measure electron temperatures for a wide range of astrophysical sources. Examples from solar (SMM, SOLEX) and stellar (Chandra, EUVE) observations are provided.

Key words: atomic data -- line: identification -- Sun: corona -- techniques: spectroscopic

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© ESO 2005

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