Table 5: Dereddened line intensity ratios with respect to I(H$\beta $) = 100 for the faint knots observed in Mkn 1087. Correction for underlying stellar absorption in H I Balmer lines was also applied. All spectra were taken using INT.
Line f($\lambda $) #1 #3 #8 #13 #14 #15
3727 [O II] 0.27 265: 240: 290 $\pm$ 35 252 $\pm$ 75 271 $\pm$ 26 286.39:
3889 He I+H 8 0.22 ... ... 19.5 $\pm$ 6.4 ... ... ...
4340 H$\gamma$ 0.135 ... ... 46.9 $\pm$ 7.9 ... 47 $\pm$ 14 ...
4861 H$\beta $ 0.00 100: 100: 100 $\pm$ 9 100 $\pm$ 23 100 $\pm$ 12 100:
4959 [O III] -0.02 ... ... 56.7 $\pm$ 8.5 55 $\pm$ 14 50.7 $\pm$ 6.6 34.7:
5007 [O III] -0.03 136: 99: 165 $\pm$ 14 144 $\pm$ 22 173 $\pm$ 14 86.5:
5876 HeI -0.23 ... ... ... ... 11.4 $\pm$ 4.1 ...
6548 [N II] -0.34 ... ... 16.8 $\pm$ 5.9 26 $\pm$ 10 13.0 $\pm$ 4.5 ...
6563 H$\alpha $ -0.34 286 $\pm$ 46 286 $\pm$ 54 286 $\pm$ 23 286 $\pm$ 31 286 $\pm$ 10 286 $\pm$ 34
6584 [N II] -0.34 54 $\pm$ 18 51.5: 60.0 $\pm$ 9.1 51.0 $\pm$ 7.1 59.7 $\pm$ 7.2 71 $\pm$ 25
6716 [S II] -0.36 ... ... 45.7 $\pm$ 7.4 46.7 $\pm$ 7.6 43.2 $\pm$ 6.5 22:
6731 [S II] -0.36 ... ... 36.0 $\pm$ 7.9 36.0 $\pm$ 5.8 27.4 $\pm$ 5.4 57:


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