Appendix I. Tables of line intensities and identifications

Appendix I contains 11 tables with all line identifications, and a detailed comparison of the wavelengths (all expressed in Å) of the lines present in the current MEKAL code (Mewe et al. 1995) with observed wavelengths, with the final adopted values.

For Tables A1 to A8, Col. 2 gives the SMM FCS wavelengths from the 1980 August 25 flare (Ph82: [26, Phillips et al. (1982)], sometimes slightly corrected: see Sect. 2). Wavelengths from laboratory experiments - the Lawrence Livermore National Laboratory Electron Beam Ion Trap (EBIT) facility [, (Beiersdorfer et al. 1998)] and the Princeton Large Torus (PLT) tokamak [7, (Brown et al. 1998)] - are given in Col. 1. Column 3 gives the scan number according to the labelling of Table 1 of the main text. Column 4 gives the present MEKAL line wavelengths, and Col. 5 those now adopted. Columns 6 and 7 give approximate total line intensities (i.e. integrated over the line profile) from respectively [26, Phillips et al. (1982)] (units: photon counts in a 0.427 s interval) and those from our fits of the SMM FCS observed lines to the corrected MEKAL model (Intf. Fit: arbitrary units). Note that these intensities are only a rough indication of line strength, and that the intensity scale of the spectra shown in Figs. 3 and 4 for this flare is in arbitrary units. The emitting ion is given in the next column. The last column contains details of the transition, with H, He, Li, etc. indicating the iso-electronic sequence and the letters or numbers the energy levels in the notation used in Appendix II. An asterix denotes dielectronic satellite line with principal quantum number n (2, 3, 4) close to a resonance line. As mentioned in §3.2, there are several lines mismatched which we arbitrarily fitted by Gaussian profiles (so-called ``missing" lines); these are labelled by letters a, b, c, ... Note that the Fe XVII $\lambda 15.014$ Å line is subject to resonance scattering (Phillips et al. 1996a), and the line at 17.626 Å is identified with an Fe XVIII line (Beiersdorfer et al. 1998) and a second-order Fe XXIII line ($\lambda 8.815$ Å) (Fawcett et al. 1985) and not with Fe II L$\alpha$ (Phillips et al. 1982). Other second-order lines are appropriately indicated. The high instrumental background at $\lambda \gt 19$ Å makes line features in this region barely recognizable so these entries should be considered uncertain.

For Tables A9 to A11, the information for earlier tables applies except that the wavelengths of Col. 1 are from the PLT measurements of [30, Wargelin et al. (1998)] (notation L2, E1 etc. are from [22, Mewe et al. (1985)] or from the HULLAC code [17, (Klapisch et al. 1977)]; U = unidentified line; density-sensitive lines (A-G, $N_{\rm e}$) Fe XXI or Fe XXII; (H-K, $N_{\rm e}$) Fe XIX and Ne IX, see [28, Phillips et al. 1996b)]. The SMM FCS wavelengths are from Fa87 = [12, Fawcett et al. (1987)], with intensities (Col. 6) from Fa87 in absolute units (photons cm^-2 s^-1) (* means estimated on the same scale from this work). Again, the column headed Intf. Fit shows total line intensities from fits of the observed lines to the corrected MEKAL model, and are in arbitrary units.

 

Table A1: Analysis of the 1980 August 25 flare spectrum measured by the SMM-FCS

 

Table A2: continued

 

Table A3: continued

 

Table A4: continued

 

Table A5: continued

 

Table A6: continued

 

Table A7: continued

 

Table A8: continued

 

Table A9: Analysis of the 1985 July 2 flare spectrum measured by the SMM-FCS

 

Table A10: continued

 

Table A11: continued