Fe XXII d - VERSION 4.0

The CHIANTI database consists of 4 primary ASCII files for each ion in the database.

• fe_22d.elvlc (energy levels)

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

  References:

  %observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G. R., 1995, 
    NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61
  %observed energy levels (2,3,4,5): Edlen, B, 1981, Phys. Scripta, 23, 1079
  %theoretical energy levels(16 - 125):  Sampson and Zhang, 1995, unpublished calculations
  %observed energy levels: J.Sugar and C.Corliss, 1985, J.Phys.Chem.Ref.Data, 14, Supplement No.2
  %observed energy levels: Kelly, R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
  %Theoretical energy levels: Zhang, H.L., Graziani, M., Pradhan, A.K., 1994, A&A, 283, 319
  %  comment:  deleted the following energy level
  125    12 2s.2p(3P).3d    4  3 F  4.5 10          0.000       0.000000    8922488.000      81.307701     P1 
  %energy levels (above IP):  calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data collaboration
  %
  % Ken Dere   Aug 1999
  

  
  

• fe_22d.wgfa (radiative data)

  contains wavelengths, gf and A values for each transition. Wavelengths are based on experimental level energies where available; wavelengths calculated from theoretical energies are less accurate and are given as negative values.

  References:

  %observed energy levels: Martin, W.C., Sugar, J., Musgrove, A., Dalton, G. R., 1995,
    NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61
  %observed energy levels (2,3,4,5): Edlen, B, 1981, Phys. Scripta, 23, 1079
  %theoretical energy levels(16 - 125):  Sampson and Zhang, 1995, unpublished calculations
  %observed energy levels: J.Sugar and C.Corliss, 1985, J.Phys.Chem.Ref.Data, 14, Supplement No.2
  %observed energy levels: Kelly, R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
  %Theoretical energy levels: Zhang, H.L., Graziani, M., Pradhan, A.K., 1994, A&A, 283, 319
  %energy levels (above IP):  calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
  %comment: theoretical wavelengths agree with NIST observed wavelength on the order of 1- 10%
  %oscillator strengths(16- 125): Sampson, D.H., Weaver, G.M., Goett, S.J., 
       Zhang, H., Clark, R.E.H., 1990, ADNDT, 44, 31
  %A values (above IP):  calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
  %comment: theoretical energies have been used as experimental values for the dielectronic transitions
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data collaboration
  %
  % Ken Dere   Aug 27 1999
  

  
  

• fe_22d.splups (electron collision data)

  contains the spline fits to the electron collision strengths scaled according to 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.

  References:

  
  %filename: fe_22d.splups
  %collision strength values from calculations of Safronova reported in Kato et al., 1997, ADNDT, 67, 225
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % Ken Dere - Aug 1999
  

  
  

• fe_22d.psplups (electron collision data) - Not Present in CHIANTI 4

  contains the spline fits to the scaled proton collision strengths.

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