J. Bernard-Salas^1,2 - S. R. Pottasch² - D. A. Beintema¹ - P. R. Wesselius¹

1 - SRON Laboratory for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands
2 - Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands

Key words: ISM: abundances - planetary nebulae: individual: NGC7027 - infrared: ISM: lines and bands - errata, addenda

**Table 3:** Ultraviolet (IUE) and optical line fluxes (Keyes & Aller 1990). Keyes fluxes were dereddened fluxes using an interstellar extinction of E_B-V=0.85.
Wavelength	Ident.	Measured	Dereddened
(nm)		Fluxes¹	Intensities¹
123.83	N V	0.12	240
140.06	O IV	0.61	271
148.50	N IV]	0.70	415
154.83	C IV	20.80	12100
157.57	[Ne V]	0.21	17.4
164.20	He II	5.00	2700
174.95	N III]	0.62	275
189.20	Si III]	0.17	87.5
190.67	C III]	4.23	2300
190.88	C III]	6.85	3700
232.55	C II	0.61	526
232.75	C II	0.48	411
242.14	[Ne IV]	1.32	609
242.45	[Ne IV]	0.43	198
278.23	[Mg V]	0.83	98.4
334.68	[Ne V]		700
342.68	[Ne V]		2100
372.62	[O II]	5.98	220
372.88	[O II]	2.19	80.2
386.98	[Ne III]	43.34	1500
396.86	[Ne III]	15.56	500
436.44	[O III]	13.36	340
447.10	He I	1.90	45.4
468.60	He II	32.3	660
471.14	[Ar IV]	1.91	38.1
474.00	[Ar IV]	6.74	131.7
486.10	H $_{\beta}$	75.9	1360
493.26	[O III]	0.17	2.9
496.03	[O III]	388.61	6400
500.82	[O III]	1178.73	19000
551.70	[Cl III]	0.20	2.23
553.80	[Cl III]	0.77	8.6
658.40	[N II]	202.65	1500
671.63	[S II]	3.57	24.1
673.10	[S II]	8.20	56
857.70	[Cl II]	1.01	3.6

¹ Units: $10^{-12}\,{\rm erg~cm^{-2}~s^{-1}}$ .

In this paper we complemented the infrared spectrum with published ultraviolet and optical data to derive abundances. We found some mistakes in Table3 which affect the ultraviolet fluxes. We present here the correct Table3. These corrected ultraviolet fluxes imply the following changes: (1) The temperature of the O IV is now 14500 and better matches the trend (solid line) in Fig.3 of the article. That of Mg V is 13000K, slightly lower than the erroneous value. This last deviation does not alter any ionic abundance because at high ionization potentials only infrared lines (which are not temperature dependent) are used to derive the abundances. (2) The abundances of silicon, nitrogen and carbon should be 6.0(-6), 1.5(-4) and 5.2(-4) respectively and not 6.2(-6), 1.6(-4) and 6.0(-4) as published. Since the error on the abundances is $\sim$ 30%, none of these erratum change any main conclusion of the paper. The authors regret these mistakes.

As minor details; in Fig.1 (top-panel) there is a line at 4.48 $\mu$ m that has been labeled as H I but is [Mg IV]. In Table2 the 3.625 $\mu$ m lines is identified as a blend of H I transitions, 6-20 and 6-19, but is probably due to Zn IV (see Dinerstein & Geballe 2001).

Contents

The ISO-SWS spectrum of planetary nebula NGC7027

References