O'Brian, T. R. and Wickliffe, M. E. and Lawler, J. E. and Whaling, W. and Brault, J. W. (1991) Lifetimes, transition probabilities, and level energies in Fe I. Journal of the Optical Society of America B, 8 (6). pp. 1185-1201. ISSN 0740-3224. http://resolver.caltech.edu/CaltechAUTHORS:OBRjosab91
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We use time-resolved laser-induced fluorescence to measure the lifetime of 186 Fe levels with energies between 25 900 and 60 758 cm . Measured emission branching fractions for these levels yield transition probabilities for 1174 transitions in the range 225-2666 nm. We find another 640 Fe transition probabilities by interpolating level populations in the inductively coupled plasma spectral source. We demonstrate the reliability of the interpolation method by comparing our transition probabilities with absorption oscillator strengths measured by the Oxford group [Blackwell et al., Mon. Not. R. Astron. Soc. 201, 595-602 (1982)]. We derive precise Fe level energies to support the automated method that is used to identify transitions in our spectra.
|Additional Information:||© 1991 Optical Society of America Received October 1, 1990; accepted December 13, 1990 This research was supported in part by National Science Foundation grants AST 87-13904 and AST 88-21051. W. Whaling was a guest observer at the National Solar Observatory (Kitt Peak) during this research. The ICP used in this work was first brought to the National Solar Observatory by Lynda M. Faires of Los Alamos National Laboratory to investigate the potential of an ICP FTS for analytical chemistry, and we are grateful for her assistance in the operation of the source for the acquisition of the present data. We are also grateful to Rolf Engleman, formerly of that laboratory, who has been responsible for a number of improvements in our use of both the hollow-cathode source and the ICP source (especially with respect to the use of carbonyl and halide vapors of several metals). M.J. Seaton of University College, London, kindly provided unpublished He gf values that were used to calibrate the IR response of the FTS. We are indebted to R.L. Kurucz of the Center for Astrophysics for generously supplying millions of semiempirical gf values. Finally, we thank S.E. Johansson for valued criticism of our Fe i level energies. The National Solar Observatory, National Optical Astronomy Observatory, is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation.|
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