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: c_5.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 Yerokhin, V. A.; Surzhykov, A. Theoretical Energy Levels of 1sns and 1snp States of Helium-Like Ions Journal of Physical and Chemical Reference Data, Volume 48, Issue 3, id.033104 (2019) ADSref: https://ui.adsabs.harvard.edu/abs/2019JPCRD..48c3104Y/abstract Observed energies of bound levels: Observed energy levels: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2018). NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/asd [Tue Feb 20 2018]. National Institute of Standards and Technology, Gaithersburg, MD. Theoretical energies for n=2, 3 above IP Goryaev, F. F.; Vainshtein, L. A.; Urnov, A. M. Atomic data for doubly-excited states 2lnl of He-like ions and 1s2lnl of Li-like ions with Z = 6-36 and n = 2 , 3 2017, ADNDT, 113, 117-257 adsRef: http://adsabs.harvard.edu/abs/2017ADNDT.113..117G DOI: 10.1016/j.adt.2016.04.002 Theoretical energy levels (n=4,5 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 adjusted by SHFTIC file derived from NIST, Yerokhin, Goryaev (n=2, 3 above IP) and Safronova (n= 4,5,6 above IP energies produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2020 June 10
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: c_5.wgfa.olg.imp %Theoretical 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 Observed energy levels (1s2s, 1s2p): Artemyev, A. N.; Shabaev, V. M.; Yerokhin, V. A.; Plunien, G.; Soff, G., 2005, Phys. Rev. A, 72, 2104 ADSref: http://adsabs.harvard.edu/abs/2005PhRvA..71f2104A Observed energies of bound levels: Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2019). NIST Atomic Spectra Database (ver. 5.7.1), [Online]. Available: https://physics.nist.gov/asd [2020, March 2]. National Institute of Standards and Technology, Gaithersburg, MD. DOI: https://doi.org/10.18434/T4W30F taken from R. L. Kelly, J. Phys. Chem. Ref. Data 16, Suppl. 1, 1-1698 (1987); Erratum: 17, 953 (1998) Theoretical energies for n=2, 3 above IP Goryaev, F. F.; Vainshtein, L. A.; Urnov, A. M. Atomic data for doubly-excited states 2lnl of He-like ions and 1s2lnl of Li-like ions with Z = 6-36 and n = 2 , 3 2017, ADNDT, 113, 117-257 adsRef: http://adsabs.harvard.edu/abs/2017ADNDT.113..117G DOI: 10.1016/j.adt.2016.04.002 Theoretical energy levels (n=4,5 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 adjusted by SHFTIC file derived from Artemyev, Goryaev (n=2, 3 above IP) and Safronova (n= 4,5,6 above IP energies two-photon A-value: Derevianko, A.; Johnson, W. R., 1997, Phys Rev A, 56, 1288 Two-photon decay of 2 1S0 and 2 3S1 states of heliumlike ions ADSref: https://ui.adsabs.harvard.edu/abs/1997PhRvA..56.1288D/abstract wavelengths determined from energy levels minimum branching ratio = 1.00e-04 sorted by lvl12 elvlcName = c_5.elvlc wgfaName = c_5.wgfa-srt allWvl = 1 minDiff = 0.00010 outfile = c_5.wgfa.olg.imp produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy K. Dere (GMU) - 2020 June 10 %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) - 2020 March 16 produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy collision strengths provided in the range 5.00e+03 to 5.00e+07 K K. Dere (GMU) - 2020 March 16 produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy DOI: http://dx.doi.org/10.1088/0953-4075/34/15/320 adsRef: http://adsabs.harvard.edu/abs/2001JPhB...34.3179W A radiation-damped R-matrix approach to the electron-impact excitation of helium-like ions for diagnostic application to fusion and astrophysical plasmas Whiteford, A. D.; Badnell, N. R.; Ballance, C. P.; O'Mullane, M. G.; Summers, H. P.; Thomas, A. L. filename: c_5.scups
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