The CHIANTI database has the following primary ASCII files for this ion:
contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.
%filename: cr_22.elvlc Theoretical energy levels: Autostructure calculation A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE Badnell, N.R., 2011, Computer Physics Communications, 182, 1528 ADSref: http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B Observed energy levels: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD. energy levels (above IP): calculations of U. Safronova reported in Kato et al., 1997, ADNDT, 67, 225. ADS http://adsabs.harvard.edu/abs/1997ADNDT..67..225K updated by U. Safronova, 2001, private communication theoretical energy levels corrected by Safronova data on an inner term basis energies of Safronova have been treated as "observed energies" produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2014 November 19 -1
contains wavelengths, gf and A values of the transitions. The wavelengths are based on the experimental energy levels and should be the best available. Wavelengths calculated from the theoretical energies are of an indeterminate accuracy and their values are presented as negative values of the calculated wavelength.
%filename: cr_22.wgfa Observed wavelengths: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [2012, September 14]. National Institute of Standards and Technology, Gaithersburg, MD. Theoretical energies, gf and A-values: Autostructure calculation A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE Badnell, N.R., 2011, Computer Physics Communications, 182, 1528 ADSref: http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B wavelengths determined from energy levels wavelengths: calculations of U. Safronova reported in Kato et al., 1997, ADNDT, 67, 225. ADS http://adsabs.harvard.edu/abs/1997ADNDT..67..225K updated by U. Safronova, 2001, private communication theoretical energy levels corrected by Safronova data on an inner term basis wavelengths of Safronova have been treated as "observed wavelengths" minimum branching ratio = 1.00e-05 produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2014 November 19 %File processed with wgfa_tidy by pryoung on 6-Mar-2019 %File processed with wgfa_tidy by pryoung on 31-May-2023
contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).
K. Dere (GMU) - 2013 January 16 produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy ADS ref: https://ui.adsabs.harvard.edu/abs/2011A%26A...528A..69L/abstract DOI: https://ui.adsabs.harvard.edu/link_gateway/2011A&A...528A..69L/doi:10.1051/0004-6361/201016417 Astronomy & Astrophysics, Volume 528, id.A69, 15 pp including Auger and radiation damping R-matrix electron-impact excitation data for the Li-like iso-electronic sequence Liang, G. Y.; Badnell, N. R. Theoretical collision strengths: %filename: cr_22.scups
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