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)

O II - VERSION 6.0

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

  1. o_2.elvlc (energy levels)

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

     
%experimental 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.
%Theoretical energy levels (levels 1-5): Montenegro, M., Eissner, W., Nahar, S., Pradhan, A.K., 2006, J.Phys.B, 39, 1863
%Theoretical energy levels (levels 6-15): Bhatia A.K. (private communications)
%comment: swapped levels 4 and 5 to be consistent with new collision data, and updated theoretical energy levels
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Enrico Landi and Peter Young - Jun 6, 2006

  2. o_2.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. 

     
%filename: o_2.wgfa
%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
%Theoretical energy levels: Bhatia A.K. (private communications)
%oscillator strengths ground configuration: Zeippen, C.J., 1987, A&A, 173, 410
%other oscillator strengths: Bhatia A.K. (private communications)
%comment: swapped levels 4 and 5 to be consistent with new collision data.
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Enrico Landi and Peter Young - Jun 6, 2006

  3. o_2.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: o_2.splups
%oscillator strengths: Bhatia A.K. (private communication)
%effective collision strengths (ground configuration): Pradhan, A.K., Montenegro, M., Nahar, S., Eissner, W., 2006, MNRAS, 366, L6
%effective collision strengths (other transitions): McLaughlin, B.M., Bell, K.L., 1994, ApJSS, 94, 825
%Collision strengths: Bhatia A.K. (private communication)
%comment: The Bhatia data were used for transitions involving the 2p5 configuration and for fine structure transitions.
%comment: The Pradhan upsilons are tabulated over the range 3.0 < Log T < 4.4. The fits reproduce the upsilons to within 0.61 %
%comment: The McLaughlin & Bell upsilons are accurate in the temperature range 3.7 < Log T < 6.0.
%comment: levels 4 and 5 are swapped in this file compared to earlier versions of CHIANTI.
% produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration
%
% Enrico Landi and Peter Young  -  Jun 7, 2006

  4. o_2.splups (proton collisional data) Not available in this VERSION.

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

    o_2_table.html (html table)


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