1 Blend with first-order line (Fe XI 349.035 A); listed values are based on
   second-order response.
 2 Blend with first-order line (Mn XV 384.745 A); listed values are based on
   second-order response.
 3 Intensity relative to other Fe XII lines is significantly lower than
   predicted by Monsignori-Fossi 1992.
 4 Intensity may be affected by possible vignetting at extreme edge of
   wavelength range.
 5 Identified as Ar XIII by Dere 1978, but our wavelength and intensity match
   better with Ni XVIII.
 6 Identified as blend with Ar XIV by Dere 1978, but our wavelength and
   intensity match better with Fe XV alone.
 7 Identified as Si X by Behring et al. 1976.  Their Table 1 lists 256.38 A,
   but the accompanying note makes clear that this is a calculated value for Si
   X whereas the wavelength they actually measured was 256.42 A.
 8 Identified as blend with Ar XIV by Dere 1978, but our wavelength and
   intensity match better with Fe XIV alone.
 9 Identified as blend with Fe XXI by Dere 1978 in his study of flare spectra.
10 Identified as S XIII by Dere 1978, probably a typographical error.
11 Gaussian fit only to unsaturated portion of line profile; thus, measurements
   are very uncertain.  Listed values for e_Lambda, e_I, and e_W have been
   increased by a factor of 2 over those resulting from the fit itself.
12 Lower level is given as ^1S_1 by Kelly 1987; it should be ^1S_0.
13 Identified as N IV by Feldman et al. 1987.
14 Measurements very uncertain due to plate flaw.  Listed values for e_Lambda,
   e_I, and e_W have been increased by a factor of 2 over those resulting from
   the fit itself.
15 Blend with second-order line (Fe X 2x174.517 A); listed values are based on
   first-order response.
16 Identified as blend with second-order Fe X by Feldman et al. 1987, but much
   stronger Fe X at 2x175.47 A is not seen in our spectrum.
17 Identified as blend with Ar XVI by Dere 1978; we resolve these two lines.
18 Blend with second-order line (Fe XII 2x192.373 A); listed values are based
   on first-order response.
19 Identified as Ca X by Behring et al. 1976 and by Dere 1978, and as blend
   with Ca X by Feldman et al. 1987.  See Keenan et al. 1993b for our analysis
   of this line.
20 Intensity relative to other Mg IX lines is significantly lower than that
   predicted by Keenan et al. 1993a; may be due to instrumental vignetting at
   extreme edge of wavelength range.
 i Fit from data smoothed with a 5 pixel ``boxcar'' routine; listed values for
   e_Lambda, e_I, and e_W have been increased by a factor of sqrt(2) over those
   resulting from the fit itself.
ii Partially saturated at a few spatial locations along the slit, with slight
   effect on the averaged profile.  Listed values for e_Lambda, e_I, and e_W
   have been increased by a factor of sqrt(2) over those resulting from the fit
   itself.