CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.

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Naval Research Laboratory (USA) - Rutherford Appleton Laboratory (UK)
University of Cambridge (UK) - George Mason University (USA) - Universita' degli Studi di Firenze (Italy)

Fe XVIII - VERSION 4.2

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

  1. fe_18.elvlc (energy levels)

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

     
%energy levels: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8
%Energy levels 9,27,91: Kelly,R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
%Energy levels 30, 52, 83: from the identifications of Brown et al., 2002, ApJS, 140, 589
%theoretical energy levels: Sampson,D.H., Zhang,H.L., Fontes,C.J., 1991, ADNDT, 48, 25
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% K.P. Dere & E.Landi 2002

  2. fe_18.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. 

     
%energy levels: Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8
%Energy levels 9,27,91: Kelly,R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. 1
%Energy levels 30, 52, 83: from the identifications of Brown et al., 2002, ApJS, 140, 589
%theoretical energy levels: Sampson,D.H., Zhang,H.L., Fontes,C.J., 1991, ADNDT, 48, 25
%oscillator strengths: Sampson,D.H., Zhang,H.L., Fontes,C.J., 1991, ADNDT, 48, 25.
%transition probabilities: Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 1995, 
       NIST Standard Reference Database 61, NIST Database for Atomic Spectroscopy, Version 1.0
%transition probabilities: Blackford,H.M.S., Hibbert,A., 1994,  ADNDT, 58, 101.
%transition probabilities: Cornille,M., Dubau,J., Loulergue,M., Bely-Dubau,F., Faucher,P., 1992, A&A, 259, 669.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
%   K.P.Dere and E.Landi 2000

  3. fe_18.splups (electron collision data)

    4. contains the spline fits to the electron collision strengths scaled according the rules formulated by 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. 

     

%filename: fe_18.splups
%Effective collision strengths 1-2 transition: Berrington, K.A., Saraph, H.E., Tully, J.A., 1998, A&AS 129, 161
%collision strengths all other transitions: Sampson, D.H., Zhang, H.L., Fontes, C.J., 1991, ADNDT, 48, 25
%produced as part of the Arcetri/Cambridge/NRL atomic data base collaboration CHIANTI
%
% P.R.Young 2001 (1-2), K.P.Dere (other trans)

  4. fe_18.psplups (proton collision data)

    5. contains the spline fits to the scaled proton collision strengths. 

     

%filename: fe_18.psplups
%rates: Foster V.J, Keenan F.P., Reid R.H.G., 1994, Phys. Rev. A 49, 3092-3095
%energies: Reader J., Sugar J., 1975, J.Phys.Chem.Ref.Data 4, 353
%comment: Fit valid for temperatures 2e6 to 2.5e8 K.
%produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Peter Young   16-May-2001

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

    fe_18_table.html (html table)


    Last revised by G. Del Zanna on 4-Sep-2009