- Table 1:
Lines used for the integral inversion and for evaluating
the elemental abundances.
preferred laboratory wavelength and
"corrected'' observed wavelength in
Brooks et al. (1999).
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),
- 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
- 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
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
and NIS-2 lines for the ions O III, Ne IV,
and Ne V.