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

fe_20.elvlc (energy levels)

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

 
%Observed energy levels (2-5): Kucera et al., 2000, ApJ, 538, 424
%Observed energy levels (6-15): Edlen, B., 1984, Pysica Scripta, 30, 135
%Observed energy levels (n=3): Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8
%Observed energy levels (16-20,23,24,67,79): Kelly,R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
%Observed energy levels (25-27,29-32,34,39,42,43,45,46,48-50,52,54,59,60,66,72,73,76,83): identifications
    from the X-ray spectral line list by Brown et al., 2002, ApJS, 140, 589
%Observed energy levels (56,58,60): From the X-ray spectral line list by Phillips et al, 1982, ApJ, 256, 774
%Theoretical energy levels: Butler and Zeippen, 2001, A&A, 372, 1078
%comment: correction (Sep 2003): changed the energies of levels 56,58,60 to better match the observations.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% G. Del Zanna and E. Landi, Sep 2003
 

fe_20.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 (2 - 5): Kucera et al., 2000, ApJ, 538, 424
%Observed energy levels (6 - 15): Edlen, B., 1984, Pysica Scripta, 30, 135
%Observed energy levels (n=3): Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8
%Observed energy levels (16-20,23,24,67,79): Kelly,R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
%Observed energy levels (25-27,29-32,34,39,42,43,45,46,48-50,52,54,59,60,66,72,73,76,83): identifications
    from the X-ray spectral line list by Brown et al., 2002, ApJS, 140, 589
%Observed energy levels (56,58,60): From the X-ray spectral line list by Phillips et al, 1982, ApJ, 256, 774
%Theoretical energy levels: Butler and Zeippen, 2001, A&A, 372, 1078
% A values for transitions within the ground configuration: Merkelis et al., 1999, Physica Scripta 59, 122
% gf and A values for allowed n=2 transitions: Butler and Zeippen, 2001, A&A, 372, 1078
% A values for other n=2 transitions: Merkelis et al., 1999, Physica Scripta 59, 122
% gf and A values for n=3 transitions: Butler and Zeippen, 2001, A&A, 372, 1078
%comment: correction (Sep 2003): changed the wavelengths of transitions from levels 56,58,60 to better
          match the observations.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%  G. Del Zanna and E. Landi, Sep 2003

fe_20.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_20.splups
%oscillator strengths: Butler and Zeippen, 2001, A&A, 372, 1078
%effective collision strengths: Butler and Zeippen, 2001, A&A, 372, 1078
%comment: effective collision strengths were provided in the temperature range 5.0 < Log T < 7.6
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% G. Del Zanna, Dec 2001

fe_20.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: fe_20.psplups
%rates: Bhatia, A.K., Mason, H.E., 1980, A&A 83, 380
%energies: Bhatia, A.K., Mason, H.E., 1980, A&A 83, 380
%comments: The fits are good to < 3%. An acceptable fit could not be found to 
    the 1 - 4 transition and so it was omitted. The rates for this 
    transition are around 1e-12 and so it is not important.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   11-Sep-2002

---

The html tables below contain the radiative data of the brightest lines sorted in wavelength

fe_20_table1.html (html table -- 12.5260 -- 15.3113 A)

fe_20_table2.html (html table -- 15.3147 -- 2666.0317 A)


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