The apparent lack or weakness of some Si II lines, (e.g. 
1260.42, 1304.37, 1526.71),
while other lines (e.g. 
1533.44) are present is caused by i.s.
re-absorption
since the lower level of these lines is the zero-volt ground state.
The 1260.42 emission is absorbed also by FeII(9) 1260.53 Å,
while the
1526.71 emission is also affected by a reseaux mark.
The 1309.28 line is present as a weak feature on the violet wing of the
unidentified
feature at 1309.32 Å. The 1808.01 Å zero-volt line is less affected by
re-absorption since its f-factor is small.
Similarly, the OI triplet near 1300 Å is affected by i.s. re-absorption
in the 1302.17 line and by partial absorption by SiII
1304.37 in the 04.86 line.
Also the 1670.81 emission line of Al II is affected by i.s. re-absorption
and by a reseaux mark.
The presence of a few lines of SiI, as reported in ADB, is
questionable; in our opinion it is just by chance coincidence because of the
richness of the SiI spectrum.
We prefer to ascribe the 1698.6 and 1727.27
features to SIII] 1698.79 and
1722 respectively, as in Penston et al. (1983), and
Williams (1995).
We leave as unidentified the rather strong feature observed at
1530.7 Å
that is not included in the lists of Penston (1983) or DF. We recall that
an unidentified emission in the solar limb at 1530.89 Å is reported by
Burton & Rydgeley (1970). We also leave as unidentified the feature at
1565.49 Å.
A few lines identified as Fe II by DF, e.g., 1360.20,
1776.61,
1881.22, 1884.11 are very weak or absent in the FeII-rich spectrum of the
symbiotic star CH Cyg. For this reason we consider these identifications as
doubtful,
although we are aware that different FeII excitation mechanisms in the two
stars could explain this behavior. On the other hand, we have identified as
FeII the two features at 1869.26 and 1872.41 Å.
These two lines are present
in CH Cyg also and are excited by a fluorescent mechanism involving 
.
as pointed out by Johansson & Jordan (1985) for late type stars.
The line at 1707.59 is identified as FeII
1708.24 in ADB; we prefer OV
07.95 due to the large FWHM in the observed profile,
thus indicating a high
ionization emitter, and to the better consistency in the wavelengths.
It is worth to point out that, to the best of our knowledge, the newly
found Ne V 1145.60
line (Table 2) is the feature at the shortest wavelength ever reported in
an IUE spectrum.
1189.8 is identified as NI
1190.0 in ADB and as SIII (1) in
Penston
(1983), but, because of its large width we prefer Mg VI 90.03,
as in DF.
1198.95 is generally identified as SV
1199.18 but the
sharpness of the profile
would suggests, rather, a low ionization species.
1324.24 is generally ident. as Mg V, but the absence of the resonance
line at
1293.9 Å casts some doubts on this identification.
1351.34 previously unidentified, is attributed to ClI(2) 51.66,
also in CH Cyg;
1367.64 prev. unid. is attributed to CuII(2) 67.
95 (Morton 1991), also in
CH Cyg;
1389.58 prev. unid. is attributed to ClI(1) 89.90,
also in CH Cyg;
1413.30 is present in both orders but not included in the lists of ADB
and
DF. We attribute it to FeII (68) 13.71;
1513.99 prev. unid. is probably FeII 14.11 + 14.37, also in CH Cyg;
1619.35 a rather wide feature, is attributed to NV 19.74 recombination
line (Williams 1995). A possible contribution by CV 1619.80
seems unlikely because of the very high excitation (380 eV) of this transition;
1882.28 absent in Penston (1983), not listed in ADB, unid. in
DF; we
attribute it to
SiIII] 1882.65, the low-density companion to the SiIII] 1892.03 line. This
is supported by the similarity in the two profiles;
1910.29, previously unidentified, is attributed to FeII (124) 10.67, also in
CH Cyg.