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

fe_12.elvlc (energy levels)

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

 
%observed energy levels: (2-4,9,11-13) Jupen, Isler & Trabert, 1994, MNRAS, 264, 627
%observed energy levels: Corliss & Sugar, 1982, J.Phys.Chem.Ref.Data, 11, 135
%theoretical energy levels: Binello, A.M., Landi, E., Mason, H.E., Storey, P.J., Brosius, J.W., 2001, A&A, 370, 1071
%comment: The third column of energies denotes energies "rescaled" from the output
   of "superstructure". The 24 configuration model used to derive the transition
   probabilities in the ".wgfa" file, gave energy levels which were slightly
   different from the observed levels. A way of estimating this difference
   for the 3s2 3p2 3d levels is to take all the levels with the same parent
   configuration (i.e., the term in brackets, e.g., (3P), (1D)), and average
   the difference between the observed and theoretical level. For the levels
   for which we don't have observed energies, we subtract the averaged
   difference for the particular parent configuration.
   The energies so derived by this method are expected to be accurate to
 

fe_12.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: (2-4,9,11- 13) Jupen, Isler & Trabert, 1994, MNRAS, 264, 627
%observed energy levels: Corliss & Sugar, 1982, J.Phys.Chem.Ref.Data, 11, 135
%theoretical energy levels: Binello, A.M., Landi, E., Mason, H.E., Storey, P.J., Brosius, J.W., 2001, A&A, 370, 1071
%Radiative data: Binello, A.M., Landi, E., Mason, H.E., Storey, P.J., Brosius, J.W., 2001, A&A, 370, 1071
%comment: the gf and A values in fourth and fifth column, respectively, have been computed by
   SuperStructure using a 24 configuration model with 4s,4p,4d,4f correlation
   (Hydrogenic) orbitals. The theoretical values so obtained have been rescaled using
   experimental and "corrected" energy levels (see ".elvlc" file).
%comment: the addition of the M2 component to the E1 A values did not introduce any change in
   the actual figures contained in this file, due to their limited precision of three
   decimal figures, except for two transitions, 3 - 18 (A(E1)=4.991E+03, A(M2)=7.3197E-01)
   and 3 - 23 (A(E1)=7.271E+03, A(M2)=4.3539E+01). For them A=A(E1)+A(M2) has been given.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% A.M.Binello and E.Landi 1998

fe_12.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_12.splups
%collision strengths (1-5): Tayal, Henry & Pradhan 1987, ApJ, 319, 951
%collision strengths (6-41): Flower, 1977, A&A, 54, 163
%comment: The collision strengths for levels 37 and 40 were mis-assigned
   in Flower's paper (compare the 2D5/2 - 2P3/2 and 2F5/2 - 2P3/2
   transitions). This has been corrected here.
%comment: The gf values were not given in Flower's paper, so a 4 configuration
   "superstructure" model was used to derive them.
%comment: effective collision strengths were provided in the temperature range 5.6 < Log T < 6.5
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% A.M.Binello and E. Landi 1998

fe_12.psplups (proton collision data)

contains the spline fits to the scaled proton collision strengths.

 

%filename: fe_12.psplups
%rates: Landman, D.A., 1978, ApJ 220, 366
%energies: Landman, D.A., 1978, ApJ 220, 366
%comment: Errors (comparing original rates with those derived from the above 
    splines) are at most 2\% for individual points. For transition 3-4, 
    a good fit could not be found, likely implying errors in the original 
    data values. Errors of up to 4.5\% are found for this transition.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   7-Jun-2001

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

fe_12_table.html (html table)


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