Table 2: The parameters of the Gaussian components of the [OIII] lines. Gaussian widths (W) and $\Delta z= z_{\rm NLR2}-z_{\rm NLR1}$ are given in km s-1. The intensity ratio $R_{\rm NLR1}=I_{5007}/I_{4959}$of the "blue component'' obtained from the Gaussian fit, the measured flux ratio $R_{\rm F}=F_{5007}/F_{4959}$ and central intensity ratio of the "blue'' and "central'' Gaussian components ( $I_{\rm B}/I_{\rm C}$) are also given (Cols. 2, 3 and 6). The data for the objects denoted with stars should be taken with caution, because their [OIII] lines are too weak.
Object $W_{\rm NLR1}$ $R_{\rm NLR1}$ $R_{\rm F}$ $W_{\rm NLR2}$ $\Delta z$ $I_{\rm B}/I_{\rm C}$

3c120

 420 3.0 2.9 $\pm$ 0.1 130 -110 0.25
3c273* 950 2.7 - 497 -200 0.39
Mrk 1040 330 1.8 2.4 $\pm$ 0.1 190 -340 0.30
Mrk 110 300 2.6 3.0 $\pm$ 0.1 150 -40 0.17
Mrk 817 510 3.0 3.0 $\pm$ 0.1 145 -300 0.43
Mrk 841 215 2.6 2.8 $\pm$ 0.1 80 -20 0.45
NGC 3227 400 3.0 3.0 $\pm$ 0.1 140 -120 1.87
NGC 4253 340 2.8 3.0 $\pm$ 0.1 105 -55 0.55
PG 1116* 650 1.8 - 239 -345 0.88
PG 1211 270 2.8 3.0 $\pm$ 0.1 81 -180 1.8


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