Table 5.

Observed IUE emission lines from two co-added short wavelength primary camera and single long wavelength redundant camera spectra

λobserved	Ion	kλ	I(IUE)	Flux*	Notes
1238.45	N v	1.638	582	2.55	Doublet
1379.52	O v?	1.339	49.7	0.77
1402.50	O iv]1397-1407, Si iv	1.306	9.03	0.16:	Very weak
1484.79	N iv]1483/87	1.231	163	3.95	Doublet
1548.79	C iv 1548/50	1.184	313	9.23	Doublet
1577.86	[Ne v]?	1.166	37.5	1.19
1597.84	[Ne iv]?	1.155	36.8	1.22
1641.14	He ii	1.136	140	5.04	P Cyg?
1663.63	O iii]	1.128	105	3.91	Doublet
1734.07	N iii?	1.118	40.7	1.57
1749.48	N iii]	1.119	105	4.02	Quintet
1835.14	?	1.152	44.7	1.50
1889.67	Si iii]1882/92	1.203	54.9	1.49
1908.20	C iii]1907/09	1.227	131	3.22	Doublet
2423.27	[Ne iv]2423/5	1.118	186	7.20	Doublet
3130.53	O iii	0.455	38.8	23.44	Bowen line
3200.17	He ii 3203	0.426	13.8	9.42

Colon means estimated errors are large, ±40%, others ±15%. The UV line intensities in column 4 are given based on the scale of I(Hβ) = 100 (with the interstellar extinction corrections, C = 1.80). 

*The fluxes are in units of 10⁻¹⁴ ergs⋅cm⁻²⋅s⁻¹.