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P. Palmeri, T.R. Kallman (LHEA, NASA/Goddard, Greenbelt MD 20771), C. Mendoza, M.A. Bautista (Centro de Fisica, IVIC, Caracas, Venezuela)
Iron K lines have proven crucial diagnostics in the X-ray spectra of compact objects such as low mass X-ray binaries and active galaxies. However, much of the available atomic data is not sufficiently accurate to fully exploit the diagnostic potential of these lines. To remedy this situation, we have carried out calculations of atomic energy levels, wavelengths, radiative and non-radiative rates for K shell transitions in all ions of iron. These make use of experimental energy levels where available. We have used a variety of available computational codes, i.e. AUTOSTRUCTURE, HFR, and BPRM. In this paper we present results of these calculations, including comparison of results from various codes and experiments, compare their relative accuracy, and present what we consider to be the most accurate selection of these data. We also present synthetic spectra calculated by incorporating these data into the xstar simulation code, and discuss some of the likely astrophysical applications for these results.
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Bulletin of the American Astronomical Society,
© 2003. The American Astronomical Soceity.