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

fe_19.elvlc (energy levels)

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

 
% filename: fe_19.elvlc
% observed energy levels: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L.,2000, J.Phys.Chem.Ref.Data, Monograph 8
% observed energy levels 57,61,71,74,77,86,87: Kelly, R.L., 1987, J.Phys.Chem.Ref.Data, 16, Suppl. 1
% observed energy levels 75: Phillips, K.J.H., et al., 1999, A&A, 138, 381
% observed energy levels 37,43,44,45,47,50,53,59,81,82,91: Brown et al, 2002, ApJS, 140, 589
% theoretical energy levels: Butler, K., Zeippen, C.J., 2001, A&A, 372, 1083
% produced as part of the Arcetri/Cambridge/NRL "CHIANTI" atomic data base collaboration
%
% Enrico Landi - Aug 2002
 

fe_19.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: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L.,2000, J.Phys.Chem.Ref.Data, Monograph 8
%observed energy levels 57,61,71,74,77,86,87: Kelly, R.L., 1987, J.Phys.Chem.Ref.Data, 16, Suppl. 1
%theoretical energy levels: Butler, K., Zeippen, C.J., 2001, A&A, 372, 1083
%Radiative data: Butler, K., Zeippen, C.J., 2001, A&A, 372, 1083
%Radiative data for transitions within the ground configuration: Loulergue et al, 1985, A&A, 150, 246
%Comment: correction (Nov 2003): put correct gf values in place of f values in V.4.02. The changes
          in level population and line emissivities should be minimal.
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Enrico Landi - Nov 2003

fe_19.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_19.splups
%Oscillator strengths: Butler, K., Zeippen, C.J., 2001, A&A, 372, 1083
%Effective collision strengths: Butler, K., Zeippen, C.J., 2001, A&A, 372, 1083
%Comment: correction (Nov 2003): put correct gf values in place of f values in V.4.02, and re-fitted
          all allowed transitions. The changes in level population and line emissivities should be minimal.
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Enrico Landi - Nov 2003

fe_19.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: fe_19.psplups
%rates: Ryans R.S.I., Keenan F.P., Reid R.H.G., unpublished.
%energies: Observed values, from .elvlc file
%comment: Fits valid for temperatures 2e6 to 4e7 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   15-May-2001

---

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

fe_19_table1.html (html table -- 13.2188 -- 106.1055 A)

fe_19_table2.html (html table -- 106.3177 -- 1328.9061 A)


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