Table 6 : part 4
OHP preprint 132
Table:  Fitting profile analysis results. Col. 1 gives the name of the object, col. 2 the adopted redshift, cols. 4 and 9 the velocities for each set of components measured on the blue and red spectra, respectively, and de-redshifted using the redshift given in col. 2; cols. 5 and 10 the corresponding FWHM, cols. 6, 11 and 12 the intensity ratios $\lambda$5007/H$\beta$, $\lambda$6583/H$\alpha$ and $\lambda$6300/H$\alpha$ respectively, and cols. 7 and 13 the fraction of the $\rm H\beta$ emission flux (respectively $\rm H\alpha$) in each component with respect to the total flux of the line in each object. A ``T'' in col. 3 (or 8) indicates that the blue (or red) spectrum has been corrected for starlight using a suitable fraction of a template (in the blue, we have used the elliptical galaxy NGC 5982 and in the red, the elliptical galaxy NGC 4365; NGC 821 was used as a template for the objects observed in October and November 1997); in the same columns, an ``A'' indicates that a $\rm H\beta$ (or $\rm H\alpha$) absorption component was added to the model. In col. 14 we give the velocity difference between the blue and red systems, and in col. 15 the spectroscopic classification of each component in the model; Gaussian profiles were used throughout, except when indicated by ``lz'' (Lorentzian profile) . Values in parenthesis have been fixed.
Name z Stellar $V\; \; \; \; \; \;$ FWHM $\lambda$5007$\:$ $\rm H\beta$ Stellar $V\; \; \; \; \; \;$ FWHM $\lambda$6583$\:$ $\lambda$6300$\:$ $\rm H\alpha$ $\Delta V \verb*+ + $ Class.
    corr. (kms-1) (kms-1) $\rm H\beta$$\;\;$ (%) corr. (kms-1) (kms-1) $\rm H\alpha$$\;\;$ $\rm H\alpha$$\;\;$ (%) (kms-1)  
Mark 938 0.019 A 111 240 1.18 91 T 173 270 0.71 0.07 89 -62 Hii
      (-79)$\;$ 890 (10)$\;\verb*+ +$ 9   -11 648 6.78 < 0.3 11 -68 Sey2
Mark 957 0.0732   -402 710 9.00 8   -201 726 1.35 < 0.3 18 -201 Sey2
      -43 200 0.15 92   3 192 0.35 < 0.02 82 -46 Hii
IRAS 01346-0924 0.070   114 178 2.13 38   165 148 0.70 < 0.04 23 -51 Hii
      -83 < 80 0.83 39   -33 219 0.46 0.07 37 -50 Hii
      -224 1069 (10)$\;\verb*+ +$ 23   - - - - -$\;$ - Sey2
      - - - -$\;$   219 2640 - - 40 - Sey1
Mark 1066 0.0122   -116 348 12.38 11   -51 270 0.77 0.07 35 -65 Sey2
      30 220 1.54 66   54 205 0.89 0.08 39 -24 Hii
      -262 875 5.76 23   -165 (875) 1.49 0.15 26 -97 Sey2
IRAS 03355+0104 0.0398   -1 364 13.69 100   12 354 0.49 0.12 66 -13 Sey2
      - - - -$\;$   264 1930 - - 34 - Sey1
IRAS 04210+0400 0.0462   14 178 13.30 41   63 219 0.40 0.17 47 -49 Sey2
      0 541 13.03 59   41 615 0.34 0.06 53 -41 Sey2
IRAS 04507+0358 0.0296   -28 240 11.00 82   14 282 0.47 0.09 64 -42 Sey2
      -146 603 14.57 18   - - - - -$\;$ - Sey2
      - - - -$\;$   -88 1254lz - - 36 - Sey1
VII Zw 73 0.0405   0 307 (15)$\;\verb*+ +$ 28   17 272 0.80 0.10 37 -17 Sey2
      -186 794 (15)$\;\verb*+ +$ 12   -171 685 0.52 0.22 16 15 Sey2
      3 151 1.28 60   14 111 0.48 0.02 47 -11 Hii
Mark 622 0.0233 T, A 6 178 (0.1) 59 T 12 205 0.79 0.06 49 -6 Hii
      -58 1172 (10)$\;\verb*+ +$ 41   -22 748 1.44 < 0.5 51 -36 Sey2
3C 198.0 0.081   - - - -$\;$   125 294 0.28 0.05 100 - ?
KUG 0825+248 0.083   108 < 80 0.62 100   135 95 0.29 0.02 100 -27 Hii
IRAS 09111-1007E 0.055   -113 < 80 (0.1) 16   -230 95 0.55 < 0.09 12 117 Hii
      (-76)$\;$ 259 (0.1) 53   -41 257 0.86 < 0.05 40 -35 Hii
      -113 430 (10)$\;\verb*+ +$ 31   -96 626 0.95 0.12 48 -17 Sey2
Zw 238.066 0.034 T, A 95 220 0.60 54 A 149 < 80 0.69 < 0.05 14 -54 Hii
      -134 154 1.33 37   -71 307 0.79 0.05 78 -63 Hii
      -295 935 (10)$\;\verb*+ +$ 9   -529 1130 3.75 < 0.6 8 234 Sey2