Fe XXIII - VERSION 4.0

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

• fe_23.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: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8
  %observed energy levels (12,21,22,25,29,34,37,39-42): Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 
           1995, NIST Database, Version 2.0, NIST Standard Reference Database 61.
  %comment: the following NIST observed energy levels have been changed.
                 old value    new value
         2p3d 3F2  9646000     9638000            
              3D2  9728000     9646000
              1D2  9638000     9728000            
              3P2  9753000     9753000
  %theoretical energy levels (n=2): Chidichimo,M.C., Zeman,V., Tully,J.A., Berrington,K.A., 1999,A&AS, 137, 175
  %theoretical energy levels (n=3): Sampson,D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
  %theoretical energy levels (n=4): Bhatia, 1996, unpublished calculations
  %Observed energy level innershell: Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 1995, NIST Database, 
         Version 2.0, NIST Standard Reference Database 61.
  %theoretical energy levels innershell: from the Flexible Atomic Code (developed by Dr. Ming-Feng Gu)
  %comment: innershell levels have been added to account for important spectral features at around 1.870 A
            (Oct 2003). All the rest is unchanged.
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % E.Landi - Oct 2003
  

  
  

• fe_23.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: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8
  %observed energy levels (12,21,22,25,29,34,37,39-42): Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R.,
           1995, NIST Database, Version 2.0, NIST Standard Reference Database 61.
  %theoretical energy levels (n=2): Chidichimo,M.C., Zeman,V., Tully,J.A., Berrington,K.A., 1999, A&AS, 137, 175
  %theoretical energy levels (n=3): Sampson,D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
  %theoretical energy levels (n=4): Bhatia, 1996, unpublished calculations
  %comment: the following NIST observed energy levels have been changed.
                 old value    new value
         2p3d 3F2  9646000     9638000            
              3D2  9728000     9646000
              1D2  9638000     9728000            
              3P2  9753000     9753000
  %oscillator strengths (n=2 levels): Zhang, H.L., Sampson. D.H., 1992, ADNDT, 1992, 52, 143
  %oscillator strengths (n=3 levels): Sampson,D.H., Goett,S.J., Clark,R.E.H., 1984, ADNDT, 30, 125
  %oscillator strengths (n=4 levels): Bhatia, 1996, unpublished calculations
  %comment:  gf values for transitions 19-26 and 23-26 were simply taken to be
      equal to the O V gf values reported by Hibbert, 1980, J. Phys. B, 13, 1721.
      The A values were obtained from the gf values by using the wavelengths listed.
  %Observed energy level innershell: Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 1995, NIST Database,
         Version 2.0, NIST Standard Reference Database 61.
  %theoretical energy levels innershell: from the Flexible Atomic Code (developed by Dr. Ming-Feng Gu)
  %Radiative data innershell: from the Flexible Atomic Code (developed by Dr. Ming-Feng Gu)
  %comment: The wavelength of the 1 - 57 transition has been considered observed even though it comes from
            theoretical energies.
  %comment: innershell levels have been added to account for important spectral features at around 1.870 A
            (Oct 2003). All the rest is unchanged.
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % E. Landi - Oct 2003
  

  
  

• fe_23.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_23.splups
  %oscillator strengths (n=2 levels): Zhang, H.L., Sampson. D.H., 1992, ADNDT, 1992, 52, 143
  %oscillator strengths (n=3 levels): Sampson,D.H., Goett,S.J., Clark,R.E.H., 1984, ADNDT, 30, 125.
  %oscillator strengths (n=4 levels): Bhatia, 1996, unpublished calculations
  %effective collision strengths (n=2): Chidichimo,M.C., Zeman,V., Tully,J.A., Berrington,K.A., 1999, A&AS, 137, 175
  %collision strengths (n=3): Sampson, D.H., Goett, S.J., Clark, R.E.H., 1984, ADNDT, 30, 125
  %collision strengths all other transitions: Bhatia A.K. (private communications)
  %gf values innershell: from the Flexible Atomic Code (developed by Dr. Ming-Feng Gu)
  %Collision strengths innershell: from the Flexible Atomic Code (developed by Dr. Ming-Feng Gu)
  %comment: Effective collision strengths from Chidichimo et al are provided for 6.3 < log T < 8.1
  %comment: innershell levels have been added to account for important spectral features at around 1.870 A
            (Oct 2003). All the rest is unchanged.
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % Enrico Landi May 2001 (n=2, n=4); K.P. Dere Sept. 97 (n=3); Enrico Landi Oct 2003 (innershell)
  

  
  

• fe_23.psplups (electron collision data)

  contains the spline fits to the scaled proton collision strengths.

  References:

  
  %filename: fe_23.psplups
  %rates: Ryans R.S.I., Foster-Woods V.J, Copeland F., Keenan F.P., Matthews A., Reid R.H.G., 1998, ADNDT 70, 179-229
  %energies: CHIANTI database, ver.1, Dere et al., A&AS 125, 149, 1997
  %comment: Fits valid for temperatures 4e6 to 3e8 K.
  %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
  %
  % Peter Young  24-Oct-00