**Table 4:** Observed and reddening-corrected line intensity ratios relative to H $\beta$ ^a.
Line	IC 5063		NGC 7212		ESO 362-G008		NGC 3281		NGC 5643		NGC 1386
	$F_{\rm obs}$	$F_{\rm dered}$	$F_{\rm obs}$	$F_{\rm dered}$	$F_{\rm obs}$	$F_{\rm dered}$	$F_{\rm obs}$	$F_{\rm dered}$	$F_{\rm obs}$	$F_{\rm dered}$	$F_{\rm obs}$	$F_{\rm dered}$
[O II] $\lambda3727$ Å	1.48	2.96	2.03	2.63	1.48	2.61	1.80	2.62	-^b	-^b	1.81	2.63
[Ne III] $\lambda3869$ Å	0.47	0.86	0.98	1.22	-^c	-^c	0.73	1.01	-^b	-^b	0.77	1.07
[Ne III] $\lambda3967$ Å	0.18	0.31	0.4	0.49	-^c	-^c	0.26	0.35	-^b	-^b	0.48	0.64
[O III] $\lambda$ 4363 Å	0.11	0.15	0.20	0.23	-^c	-^c	0.12	0.14	-^b	-^b	0.19	0.23
He II $\lambda$ 4686 Å	0.14	0.15	0.23	0.24	-^c	-^c	0.36	0.38	-^b	-^b	0.46	0.48
[O III] $\lambda$ 5007 Å	8.88	8.03	12.52	12.06	11.57	10.65	9.21	8.72	12.38	11.40	11.34	10.73
[Fe VII] $\lambda$ 5721 Å	-	-	-	-	-	-	0.08	0.06	-^b	-^b	0.29	0.22
[Fe VII] $\lambda$ 6087 Å	0.14	0.07	0.06	0.04	-	-	0.17	0.12	-^b	-^b	0.44	0.31
[O I] $\lambda$ 6300 Å	0.71	0.32	0.76	0.56	0.44	0.23	0.46	0.30	-^b	-^b	0.46	0.30
[Fe X] $\lambda$ 6375 Å	0.04	0.02	0.04	0.03	-	-	0.02	0.01	-^b	-^b	0.07	0.05
H $\alpha$	7.10	2.87	4.04	2.87	6.06	2.87	4.71	2.87	6.03	2.87	4.70	2.87
[N II] $\lambda$ 6583 Å	4.27	1.71	2.82	1.99	6.78	3.18	4.02	2.44	6.30	2.98	5.60	3.41
[S II] $\lambda$ 6716 Å	1.51	0.58	0.80	0.56	1.19	0.54	1.31	0.78	1.74	0.80	1.04	0.62
[S II] $\lambda$ 6731 Å	1.49	0.57	0.98	0.63	1.53	0.70	1.24	0.74	1.94	0.89	1.29	0.77

^a All narrow emission line ratios were derived from the nuclear spectra. After reddening correction, other Balmer line-ratios such as H $\gamma$ /H $\beta$ and H $\delta$ /H $\beta$ are consistent with the recombination values within the errors. The uncertainties are in the range of $\sim$ 1-15%.

^b Not covered by wavelength range.

^c Underlying absorption lines.

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