All Tables

Table 1: Lines used for the integral inversion and for evaluating the elemental abundances. $\lambda ^{\rm ad}$ is our preferred laboratory wavelength and $\lambda ^{\rm cor}$ the "corrected'' observed wavelength in Brooks et al. (1999). $T_{\rm p}$ is the peak temperature of line formation. Since one line per ion at most is used in the integral inversion, we indicate with "i'' the lines used in the integral inversion and "f'' the lines compared with observations in the forward sense, i.e. by comparing the intensities predicted using the DEM with the observed intensities. The source for the adopted wavelengthis is denoted by E for Edlén (1983a,1984,1985c,b,a,1983b), F for Fawcett (1975), K for Kelly (1987), N for Martin et al. (1995), and O for Wiese (1985), respectively.
Table 2: Comparison between the Be-like Mg IX (368.057 Å) and the Li-like Mg X (624.95 Å) transitions in the selected segments.
Table 3: Electron density derived from Mg VIII lines ratios. The 315.015 Å and 335.231 Å line intensities have been corrected assuming that they are affected by blendings contributing 50% and 20% of the observed intensity, respectively. C is the correction factor applied to the line ratio to take blending into account.
Table 4: Electron density derived from the Mg VIII 338.983/313.743 Å line ratio in the selected segments. The lower limit and the upper limit are indicated with "ll'' and "ul'', respectively.
Table 6: Abundance enhancement factors (with respect to photospheric composition) for the low FIP elements in the selected segments. $\beta$ is the FIP bias deduced from the observed Mg VI (349.2 Å)/Ne VI (562.8 Å) line intensity ratio as in Young & Mason (1997). The result for Ar in segment 2(1) is not reported because the estimated error is very large.
Table 7: Comparison of the median $I_{\rm th}/I_{\rm obs}$ between NIS-1 and NIS-2 lines for the ions O III, Ne IV, and Ne V.