**Table 8:** Fitting parameters of surface-brightness distributions^a. For ESO 362-G008, too few data points were available for a fit.
Galaxy	Data Points	$\delta_{\rm [OIII]}$	$\log L_{\rm [OIII], 0}$	$\delta_{\rm H\alpha}$	$\log L_{\rm H\alpha, 0}$	$\delta_{\rm cont}$	$\log L_{\rm cont, 0}$
			(erg s^-1 pc^-2)		(erg s^-2 pc^-2)		(erg s^-2 pc^-2)
IC 5063	9	-2.73 $\pm$ 0.33	38.41	-2.75 $\pm$ 0.31	38.01	-1.37 $\pm$ 0.18	35.2
NGC 7212	4	-2.13 $\pm$ 0.57	38.46	-2.09 $\pm$ 0.56	37.85	-0.77 $\pm$ 0.26	34.57
NGC 3281	4	-2.35 $\pm$ 0.60	38.22	-2.34 $\pm$ 0.64	37.73	-1.02 $\pm$ 0.18	35.34
NGC 5643	10	-1.42 $\pm$ 0.19	35.97	-1.34 $\pm$ 0.16	35.35	-1.54 $\pm$ 0.11	33.94
NGC 1386	6	-2.56 $\pm$ 0.82	37.16	-2.27 $\pm$ 0.60	36.55	-1.26 $\pm$ 0.48	35.46

^a A linear least-squares fit was applied with $\log L = \delta \cdot \log R/R_0 + \log L_{0}$ and R₀ = 100 pc from the nucleus. The number of data points included in the fit is given in Col. 2 (=half the number of averaged values from both sides of the nucleus). For NGC 5643 which shows a transition between line ratios typical for AGNs and H II-regions, only data points within the NLR were included.

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