Fe III - VERSION 11.0.1

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

  1. fe_3.elvlc (energy levels)

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

     
 
 Observed energies have been assessed using:

1) Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). 
NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/
2) Ekberg,J.O., 1993, A&AS, 101, 1
adsurl = {http://adsabs.harvard.edu/abs/1993A%26AS..101....1E}

The  assignement to the higher levels was in several cases uncertain.
Some discrepancies between the NIST and Ekberg designations 
were also found. 

Theoretical energies:
Badnell, N.R. and Ballance, C.P., 2014, ApJ, 785, 99
      doi = {10.1088/0004-637X/785/2/99}
   adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...785...99B}

   The level ordering follows Badnell and Ballance (2014).
   
Produced for the CHIANTI database v.8 by Giulio Del Zanna 12  Nov 2014 
quick fix to observed ecm 0.0 -> -1.0 (kpd 7/oct/2015)

 -1

  2. fe_3.wgfa (radiative data)

    3. 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 energies have been assessed using:

1) Kramida, A., Ralchenko, Yu., Reader, J., and NIST ASD Team (2012). 
NIST Atomic Spectra Database (ver. 5.0), [Online]. Available: http://physics.nist.gov/
2) Ekberg,J.O., 1993, A&AS, 101, 1
adsurl = {http://adsabs.harvard.edu/abs/1993A%26AS..101....1E}

The  assignement to the higher levels was in several cases uncertain.
Some discrepancies between the NIST and Ekberg designations 
were also found. 

Theoretical energies and gf values:
Badnell, N.R. and Ballance, C.P., 2014, ApJ, 785, 99
doi = {10.1088/0004-637X/785/2/99}
adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...785...99B}
   
A-values have been recalculated with AUTOSTRUCTURE using the 
same target as  Badnell and Ballance (2014), but with 
the experimental energies.
   
Note: only transitions with a branching ratio above 10^-5 
have been retained.


Produced for the CHIANTI database v.8 by Giulio Del Zanna 12  Nov 2014 

% corrected wavelengths at lines 7978 and 8018
% K Dere 7 oct 2015 

Removed a few transitions from levels 11,13,68 that were unphysical
(observed energy of the upper level lower than the energy of the lower level)
G. Del Zanna 5 May 2016


%File processed with wgfa_tidy by pryoung on  6-Mar-2019
%File processed with wgfa_tidy by pryoung on  6-Mar-2019
%File processed with wgfa_tidy by pryoung on 31-May-2023
%File processed with wgfa_tidy by pryoung on 31-May-2023

  3. fe_3.scups (electron collision data)

    4. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992). 

     


Produced for the CHIANTI database v.8 by Giulio Del Zanna 12  Nov 2014 


Badnell, N.R. and Ballance, C.P., 2014, ApJ, 785, 99                   

Data from

  4. (proton collisional data) Not available in this VERSION.

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

    Page created by Giulio Del Zanna on Wed Apr 16 17:43:04 2025