All Tables

Table 1: The configurations used to calculate the energy levels and the radiative data.
Table 2: The details of the most important configurations in Fe XXIII (only the most significant n=4 levels are shown; the full Table is available in electronic form). The percentage of level mixing (>10%) is indicated in second column. $E_{\rm best}$ indicates the best energies (cm^-1) which we propose in this work. The uncertainties in the energies reflect the estimated errors in the wavelength measurements. Levels with uncertain identification are assigned an uncertainty of 5000 cm^-1, an estimate based on the comparisons between the observed energies and the values computed ab initio. The other columns indicate the differences between our $E_{\rm best}$ and the energies from NIST $E_{\rm NIST}$ , the collisional calculations $E_{\rm CC}$ , and the adjusted SS values $E_{\rm SS}$ . Levels are ordered according to the energies $E_{\rm CC}$ from the scattering calculations.
Table 3: Results for the brightest lines in Fe XXIII. The lines are grouped in three ranges ( ${n=2\to 2}$ , $n=3 \to 2$ , $n=4 \to 2$ ), and are displayed in decreasing order of intensity. Columns 2, 3 show the relative line intensities (ergs) $Int=N_{j} A_{ji}/N_{\rm e}$ calculated at different temperatures and at an electron density of 10¹⁰ cm^-3, normalised to the intensity of the 1-15 line at 10⁷ K. Columns 4, 5 show the gf and A values calculated in this work. Column 6 shows, for comparison, the NIST A values. The last two columns show the wavelengths corresponding to the best energies $E_{\rm best}$ of Table 2 and the NIST values. The uncertainties on the proposed wavelengths are derived from the uncertainties assigned to the energies. Note the different temperature sensitivity of the various lines.
Table 4: Measured and calculated lifetimes for some of the lower levels in Fe XXIII. SS: calculated with SUPERSTRUCTURE and adjusted energies; AS: calculated with AUTOSTRUCTURE (Chidichimo et al. 2005); S99: calculated by Safronova et al. (1999) using relativistic many-body perturbation theory (including only n=2 levels).
Table 5: The fractional level populations N_j, calculated at different electron densities (cm^-3) and the temperature T= 12.6 MK (log T=7.1) for the lowest (most populated) levels.
Table 6: Summary of the line identifications for Fe XXIII The columns indicate: 1) the indices corresponding to Tables 2; 2,3) the relative intensities (in photons, scaled to the 1-15 10.980 Å line and calculated at log $T[{\rm K}]=7.2$ ) typical of astrophysical and laser plasmas (10¹², 10¹⁹ cm^-3); 4) the wavelengths calculated from our best energies $E_{\rm best}$ ; 5) observed wavelengths $\lambda _{\rm observed}$ ; some blends are indicated (bl = blend; bl-mr = blend in medium-resolution spectra; bl-w = blend with a weak line); lines with no or a tentative identification have a question mark; 6,7) previous identifications consistent or not with ours (with observed wavelengths in Å; note that observed and calculated wavelengths in the cited literature can differ from the values reported here). Legenda: Bo78: Boiko et al. (1978) (see also original work cited in this review paper); B78: Bromage et al. (1978); B85: Burkhalter et al. (1985); B02: Brown et al. (2002); D72: Doschek et al. (1972); F79: Fawcett et al. (1979); F00: Feldman et al. (2000); H80: Hinnov & Suckewer (1980); K74: Kastner et al. (1974); LP80: Lawson & Peacock (1980); S80: Spector et al. (1980) SF86: Seely & Feldman (1986); SR95: Sugar & Rowan (1995); W75: Widing (1975); W98: Wargelin et al. (1998). The final column indicates weather the lines have only been observed in high-density plasmas (H).