Electron density in the quiet solar coronal transition region from SoHO/SUMER measurements of S VI line radiance and opacity

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Table 1:

Spectral lines present in the data sets, with parameters computed by CHIANTI and given by previous observations.
		CHIANTI^a			Curdt et al. (2001)
ion	transition $j \rightarrow i$	$\log T_{\rm max}$ (K)	wavelength (Å)	radiance^b	wavelength (Å)	peak radiance^b
S VI	$2{\rm p}^6\;3{\rm p}\;{}^2{\rm P}_{3/2} \rightarrow 2{\rm p}^6\;3{\rm s}\;{}^2{\rm S}_{1/2}$	5.3	933.3800	$3.81\times10^{-3}$	933.40	0.57
Ly $\varepsilon$	$6{\rm p}\;{}^2{\rm P}_{3/2} \rightarrow 1{\rm s}\;{}^2{\rm S}_{1/2}$	--	--	--	937.80	1.07
Si VIII	$2{\rm s}^2\;2{\rm p}^3\;{}^2{\rm P}_{3/2} \rightarrow 2{\rm s}^2\;2{\rm p}^3\;{}^4{\rm S}_{3/2}$	5.9	944.4670	$5.24\times10^{-3}$	944.34	0.14
S VI	$2{\rm p}^6\;3{\rm p}\;{}^2{\rm P}_{1/2} \rightarrow 2{\rm p}^6\;3{\rm s}\;{}^2{\rm S}_{1/2}$	5.3	944.5240	$1.91\times10^{-3}$	944.55	0.29

^a Using the ``Arnaud & Raymond'' ionization fractions file, the ``Sun coronal'' abundance file and the ``quiet Sun'' DEM file. CHIANTI does not include data for the Hydrogen lines (Ly $\varepsilon$ in particular).
^b Radiances are given in ${\rm W~m^{-2}~sr^{-1}}$ , and peak spectral radiances are given in ${\rm W~m^{-2}~sr^{-1}~nm^{-1}}$ .

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