Fe V - VERSION 10.1

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

fe_5.elvlc (energy levels)

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

 
%filename:  fe_5.elvlc
%Observed energies: Ralchenko, Yu., Kramida, A.E., Reader, J., and NIST ASD Team (2008). 
       NIST Atomic Spectra Database (version 3.1.5), [Online]. Available: http://physics.nist.gov/asd3 
       [2009, September 1]. National Institute of Standards and Technology, Gaithersburg, MD.
%Theoretical energies: Ballance, C.P., Griffin, D.C., & McLaughlin, B.M. 2007, J.Phys.B, 40, F327
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%   Peter Young, 3-Sep-2009

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.

 
%filename: fe_5.wgfa
%Observed energies: Ralchenko, Yu., Kramida, A.E., Reader, J., and NIST ASD Team (2008).
       NIST Atomic Spectra Database (version 3.1.5), [Online]. Available: http://physics.nist.gov/asd3
       [2009, September 1]. National Institute of Standards and Technology, Gaithersburg, MD
%A-values: Nahar, S.N., Delahaye, F., Pradhan, A.K., Zeippen, C.J., 2000, A&AS, 144, 141
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%      Peter Young, 2-Sep-2009
%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

fe_5.scups (electron collision data)

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

 
%   - updated fit for transition 1-33 (removed negative spline value)
% Peter Young, 22-Sep-2011
% Peter Young, 2-Sep-2009
%
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%Comment: The spline fits are accurate to 0.59 % or better over the temeprature range 5000 to 50,000 K.
%Theoretical energies: Ballance, C.P., Griffin, D.C., & McLaughlin, B.M. 2007, J.Phys.B., 40, F327
         [2009, September 1]. National Institute of Standards and Technology, Gaithersburg, MD.
         Spectra Database (version 3.1.5), [Online]. Available: http://physics.nist.gov/asd3 
%Observed energies: Ralchenko, Yu., Kramida, A.E., Reader, J., and NIST ASD Team (2008). NIST Atomic 
%filename: fe_5.splups

(proton collisional data) Not available in this VERSION.

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

fe_5_table1.html (html table -- 1039.9630 -- 66871.7422 A)

fe_5_table2.html (html table -- 208463.6250 -- 259201.6562 A)

Page created by Giulio Del Zanna on Mon Jun 26 11:16:21 2023