Analysis of chemical abundances in planetary nebulae with [WC] central stars - I. Line intensities and physical conditions

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Table 3

Observed and reddening corrected line ratios (F(Hβ) = 100) and line identifications.

			Cn 1-5
λ_o (Å)	Ion	Mult.	λ_obs (Å)	V_rad (km s^-1)	F(λ)/F(Hβ)	I(λ)/I(Hβ)	err (%)	notes

3447.59	He i	7	3447.24	–30.45	0.286	0.441	16
3478.97	He i	43	3478.76	–18.09	0.169	0.257	23
3487.73	He i	42	3487.44	–24.93	0.106	0.161	33
3512.51	He i	38	3512.17	–29.03	0.225	0.338	18
3530.50	He i	36	3530.15	–29.73	0.202	0.302	20
3554.42	He i	34	3554.05	–31.20	0.232	0.343	18
3587.28	He i	32	3586.89	–32.61	0.350	0.512	13
3613.64	He i	6	3613.26	–31.52	0.363	0.525	13
3634.25	He i	28	3633.85	–32.99	0.484	0.696	11
3669.47	H i	H25	3669.07	–32.68	0.352	0.500	13
3671.48	H i	H24	3671.07	–33.47	0.399	0.567	12
3673.76	H i	H23	3673.34	–34.27	0.452	0.641	11
3676.37	H i	H22	3675.97	–32.63	0.518	0.733	10
3679.36	H i	H21	3678.94	–34.24	0.492	0.696	11
3682.81	H i	H20	3682.48	–26.87	0.636	0.898	9
3686.83	H i	H19	3686.46	–30.10	0.586	0.827	10
3691.56	H i	H18	3691.17	–31.69	0.606	0.854	10
3694.22	Ne ii	1	3693.80	–34.08	0.124	0.175	29
3697.15	H i	H17	3696.75	–32.43	0.745	1.047	9
3703.86	H i	H16	3703.47	–31.58	0.914	1.279	8
3705.04	He i	25	3704.63	–33.19	0.740	1.036	9
3711.97	H i	H15	3711.60	–29.88	1.063	1.485	7
3721.83	[S iii]	2F	3721.42	–33.04	2.386	3.321	6
3721.93	H i	H14	*	*	*	*	*
3726.03	[O ii]	1F	3725.62	–32.98	51.615	71.752	6
3728.82	[O ii]	1F	3728.37	–36.18	25.956	36.053	6
3734.37	H i	H13	3733.97	–32.13	1.610	2.233	7
3750.15	H i	H12	3749.72	–34.37	2.195	3.029	6
3770.63	H i	H11	3770.22	–32.59	2.675	3.669	6
3797.63	[S iii]	2F	3797.48	–11.83	3.834	5.217	6
3797.90	H i	H10	*	*	*	*	*
3819.61	He i	22	3819.24	–29.05	1.317	1.781	7
3835.39	H i	H9	3834.97	–32.83	5.738	7.725	6
3862.59	Si ii	1	3861.97	–48.14	0.061	0.082	:
3868.75	[Ne iii]	1F	3868.33	–32.54	71.411	95.248	6
3871.82	He i	60	3871.35	–36.39	0.086	0.115	39
3888.65	He i	2	3888.42	–17.73	17.195	22.809	6
3889.05	H i	H8	*	*	*	*	*

Notes. The full version of this table is online.

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