Fe XXV - VERSION 10.1


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

  1. fe_25.elvlc (energy levels)
  2. contains the energy levels (in cm-1). It includes both experimental and theoretical values of the levels energies.

     
    
    %filename:  fe_25.elvlc
    Theoretical energy levels:  Autostructure calculation
    A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE
    Badnell, N.R., 2011, Computer Physics Communications, 182, 1528
    ADSref:  http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B
    
    observed energy levels 1s2p 1P1, 1s2p 3P1
    
    Rudolph, J. K.; Bernitt, S.; Epp, S. W.; Steinbrugge, R.; Beilmann, C.; Brown, G. V.; Eberle, S.; Graf, A.; Harman, Z.; Hell, N.; Leutenegger, M.; Mueller, A.; Schlage, K.; Wille, H.-C.; Yavas, H.; Ullrich, J.; Crespo Loopez-Urrutia, J. R.
    X-Ray Resonant Photoexcitation: Linewidths and Energies of K alpha Transitions in Highly Charged Fe Ions
    Physical Review Letters, vol. 111, Issue 10, id. 103002
    DOI:  10.1103/PhysRevLett.111.103002
    adsRef:  http://adsabs.harvard.edu/abs/2013PhRvL.111j3002R
    
    observed energy levels:  1s3p 1P1, 1s4p 1P1, 1s5p 1P1
    
    Beiersdorfer, P.; Bitter, M.; von Goeler, S.; Hill, K. W.
    Physical Review A (General Physics), Volume 40, Issue 1, July 1, 1989, pp.150-157
    doi:10.1103/PhysRevA.40.150
    ADS:  https://ui.adsabs.harvard.edu/abs/1989PhRvA..40..150B/abstract
    
    observed energy levels 1s2p 3P2  1s2 1S0 - 1s2p 3P2  6682.7 eV     53899600.  (53899615.2)
     (listed as transition for 1s2 1S0 - 1s2p 3P1)
    
    Briand, J. P.; Tavernier, M.; Marrus, R.; Desclaux, J. P. 
    Physical Review A (General Physics), Volume 29, Issue 6, June 1984, pp.3143-3149
    doi:10.1103/PhysRevA.29.3143
    ADSref:  https://ui.adsabs.harvard.edu/abs/1984PhRvA..29.3143B/abstract
    
    (Observed) energy levels (1s2s, 1s2p):  Artemyev, A. N.; Shabaev, V. M.; Yerokhin, V. A.; Plunien, G.; Soff, G., 2005, Phys. Rev. A, 72, 2104
    ADSref:  http://adsabs.harvard.edu/abs/2005PhRvA..71f2104A
    
    %observed energy levels:  Martin, W. C., Sugar, J., Musgrove, A., and Dalton, G. R., 1995,
    NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
    %theoretical energy levels:  Sampson, D. H., Goett, S.J., Clark, R.E.H., 1983, ADNDT, 29, 467
    
    Theoretical energies for n=2, 3 above IP
    Goryaev, F. F.; Vainshtein, L. A.; Urnov, A. M.
    Atomic data for doubly-excited states 2lnl of He-like ions and 1s2lnl of Li-like ions with Z = 6-36 and n = 2 , 3
    2017, ADNDT, 113, 117-257
    adsRef:  http://adsabs.harvard.edu/abs/2017ADNDT.113..117G
    DOI:  10.1016/j.adt.2016.04.002
    
    Theoretical energy levels (n=4,5 above IP):
    calculations of U. Safronova reported in Kato et al., 1997, ADNDT, 67, 225.
    ADS http://adsabs.harvard.edu/abs/1997ADNDT..67..225K
    updated by U. Safronova, 2001, private communication
    
    theoretical energy levels adjusted by SHFTIC file derived from 
    Rudolph, Beiersdorfer, NIST, Artemyev, Goryaev (n=2, 3 above IP) and Safronova (n= 4,5,6 above IP energies
    
    K. Dere (GMU) - 2020 July 6
    fe_25 IP ev =  8.82805e+03 Ip invcm =    71203000.000 Ip Ryd =     648.84946
     
    

  3. fe_25.wgfa (radiative data)
  4. 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_25.wgfa
    
    Theoretical gf and A-values:  Autostructure calculation
    A Breit-Pauli distorted wave implementation for AUTOSTRUCTURE
    Badnell, N.R., 2011, Computer Physics Communications, 182, 1528
    ADSref:  http://adsabs.harvard.edu/abs/2011CoPhC.182.1528B
    
    two-photon rate:  Derevianko, A.; Johnson, W. R., 1997, Phys Rev A, 56, 1288
    Two-photon decay of 2 1S0 and 2 3S1 states of heliumlike ions
    ADSref:  https://ui.adsabs.harvard.edu/abs/1997PhRvA..56.1288D/abstract
    
    observed energy levels 1s2p 1P1, 1s2p 3P1
    
    Rudolph, J. K.; Bernitt, S.; Epp, S. W.; Steinbrugge, R.; Beilmann, C.; Brown, G. V.; Eberle, S.; Graf, A.; Harman, Z.; Hell, N.; Leutenegger, M.; Mueller, A.; Schlage, K.; Wille, H.-C.; Yavas, H.; Ullrich, J.; Crespo Loopez-Urrutia, J. R.
    X-Ray Resonant Photoexcitation: Linewidths and Energies of K alpha Transitions in Highly Charged Fe Ions
    Physical Review Letters, vol. 111, Issue 10, id. 103002
    DOI:  10.1103/PhysRevLett.111.103002
    adsRef:  http://adsabs.harvard.edu/abs/2013PhRvL.111j3002R
    
    observed energy levels:  1s3p 1P1, 1s4p 1P1, 1s5p 1P1
    
    Beiersdorfer, P.; Bitter, M.; von Goeler, S.; Hill, K. W.
    Physical Review A (General Physics), Volume 40, Issue 1, July 1, 1989, pp.150-157
    doi:10.1103/PhysRevA.40.150
    ADS:  https://ui.adsabs.harvard.edu/abs/1989PhRvA..40..150B/abstract
    
    (Observed) energy levels (1s2s, 1s2p):  Artemyev, A. N.; Shabaev, V. M.; Yerokhin, V. A.; Plunien, G.; Soff, G., 2005, Phys. Rev. A, 72, 2104
    ADSref:  http://adsabs.harvard.edu/abs/2005PhRvA..71f2104A
    
    %observed energy levels:  Martin, W. C., Sugar, J., Musgrove, A., and Dalton, G. R., 1995,
    NIST Database for Atomic Spectroscopy, Version 1.0, NIST Standard Reference Database 61.
    
    Theoretical energies for n=2, 3 above IP
    Goryaev, F. F.; Vainshtein, L. A.; Urnov, A. M.
    Atomic data for doubly-excited states 2lnl of He-like ions and 1s2lnl of Li-like ions with Z = 6-36 and n = 2 , 3
    2017, ADNDT, 113, 117-257
    adsRef:  http://adsabs.harvard.edu/abs/2017ADNDT.113..117G
    DOI:  10.1016/j.adt.2016.04.002
    
    Theoretical energy levels (n=4,5 above IP):
    calculations of U. Safronova reported in Kato et al., 1997, ADNDT, 67, 225.
    ADS http://adsabs.harvard.edu/abs/1997ADNDT..67..225K
    updated by U. Safronova, 2001, private communication
    
    theoretical energy levels adjusted by SHFTIC file derived from 
    Rudolph, NIST, Artemyev, Goryaev (n=2, 3 above IP) and Safronova (n= 4,5,6 above IP energies
    
    wavelengths determined from energy levels
    minimum branching ratio =   1.00e-04
    
    sorted by lvl12
    elvlcName = fe_25.elvlc
     wgfaName = fe_25.wgfa-srt
     allWvl =   1
     minDiff =      0.00010
     outfile = fe_25.wgfa.olg.imp
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
     K. Dere (GMU) - 2020 October 11
    %File processed with wgfa_tidy by pryoung on 31-May-2023
    

  5. fe_25.scups (electron collision data)
  6. contains the effective electron collision strengths scaled according to the rules formulated by Burgess and Tully (1992).

     
    K. Dere (GMU) - 2020 July 06
    produced as a part of the 'CHIANTI' atomic database for astrophysical spectroscopy
    
    collision strengths provided in the range   1.25e+05 to   1.25e+09 K
    
    DOI:  http://dx.doi.org/10.1088/0953-4075/34/15/320
    adsRef:  http://adsabs.harvard.edu/abs/2001JPhB...34.3179W
    A radiation-damped R-matrix approach to the electron-impact excitation of helium-like ions for diagnostic application to fusion and astrophysical plasmas
    Whiteford, A. D.; Badnell, N. R.; Ballance, C. P.; O'Mullane, M. G.; Summers, H. P.; Thomas, A. L.
    Theoretical collision strengths:
    
    filename: fe_25.scups
    

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

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

    fe_25_table.html (html table)

    Page created by Giulio Del Zanna on Mon Jun 26 11:16:28 2023