The CHIANTI database consists of the following primary ASCII files for this ion:

fe_23d.elvlc (energy levels)

contains the energy levels in cm^(-1) It includes both experimental and theoretical values of the levels energies.

 
%observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995, 
   NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
%theoretical energy levels: Bhatia, A.K., private communications
%energy levels (above IP): calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225.
%comment: energies have been corrected (Sep 2003). This affects the position of all wavelengths, now
          in much better agreement with observations.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Ken Dere and Enrico Landi - Sep 2003
 

fe_23d.wgfa (radiative data)

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.

 
%observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G.R., 1995, 
   NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61
%theoretical energy levels: Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
%comment:  several NIST observed energy levels have been changed.
              old value    new value      
      2p3d 3F2  9646000     9638000
           3D2  9728000     9646000
           1D2  9638000     9728000
           3P2  9753000     9753000
%oscillator strengths (n=2): Bhatia, 1996, unpublished calculations
%oscillator strengths (from n=3 to n=2): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
%comment:  gf values for transitions 19-26 and 23-26 were simply taken to be
   equal to the O V gf values reported by Hibbert, 1980, J. Phys. B, 13, 1721.
   The A values were obtained from the gf values by using the wavelengths listed.
%A values (above IP):  calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225.
%comment:  theoretical wavelengths of Kato/Safronova are used as observed wavelengths (positive values)
%comment:      1    2        0.           0.000e+00      1.000e+07 2S2           1 S0.0 2S2P          3 P0.0  a fix      
%comment: theoretical energies have been used as experimental values for the dielectronic transitions
%comment: level energies and wavelengths have been corrected (Sep 2003). This affects the position of all 
          wavelengths, now in much better agreement with observations.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  Ken Dere and Enrico Landi - Sep 2003

fe_23d.splups (electron collision data)

contains the spline fits to the electron collision strengths scaled according the rules formulated by Burgess and Tully (1992). Accurate replication of the temperature averaged collision strength over a wide range of temperatures can be accomplished with the data in this file.

 

%filename: fe_23d.splups
%collision strength values from calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Ken Dere - Aug 1999

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The html table below contains the radiative data of the brightest lines sorted in wavelength

fe_23d_table.html (html table)


Last revised by G. Del Zanna on 4-Sep-2009