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Home All issues Volume 520 (September-October 2010) A&A, 520 (2010) A109 Full HTML
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Table 11:

Linear Pearson correlation coefficients.
  $\sigma_{\rm PA}-k_{3,5}/k_{1}$ $\Delta \phi-\sigma_{\rm PA}$ $k_{3,5}/k_{1}-\Delta \phi$
c+f 0.5 (Fig. A.1a) 0.0 0.0
  $\sigma_{\rm PA}-R/R_{\rm vir}$ $\Delta \phi-R/R_{\rm vir}$ $k_{3,5}/k_{1}-R/R_{\rm vir}$
c 0.1 0.2 0.4
  $R_{\rm d}-k_{3,5}/k_{1}$ $R_{\rm d}-\sigma_{\rm PA}$ $R_{\rm d}-\Delta \phi$
c+f 0.2 0.3 -0.4
c 0.1 0.5 (Fig. 11b) -0.1
  MB-k3,5/k1 $M_{B}-\sigma_{\rm PA}$ $M_{B}-\Delta \phi$
c+f 0.0 -0.1 0.4
c -0.3 -0.5 (Fig. 11c) 0.1
  A-k3,5/k1 $A-\sigma_{\rm PA}$ $A-\Delta \phi$
c+f -0.2 0.1 -0.1
c -0.1 0.2 0.0
  C-k3,5/k1 $C-\sigma_{\rm PA}$ $C-\Delta \phi$
c+f 0.0 -0.1 0.2
c 0.1 0.0 -0.2
  $\log(L_{\rm H_\alpha})-k_{3,5}/k_{1}$ $\log(L_{\rm H_\alpha})-\sigma_{\rm PA}$ $\log(L_{\rm H_\alpha})-\Delta \phi$
c+f 0.1 0.1 -0.1
c 0.8 (Fig. 10b) 0.8 (Fig. 10a) 0.0
  z-k3,5/k1 $z-\sigma_{\rm PA}$ $z-\Delta \phi$
f 0.1 0.0 0.1
  (B-V)-k3,5/k1 $(B-V)-\sigma_{\rm PA}$ $(B-V)-\Delta \phi$
c+f -0.1 -0.2 -0.2
c -0.2 -0.1 -0.2
  (V-I)-k3,5/k1 $(V-I)-\sigma_{\rm PA}$ $(V-I)-\Delta \phi$
c+f 0.0 0.2 0.0
c 0.4 0.2 0.1
  (R-I)-k3,5/k1 $(R-I)-\sigma_{\rm PA}$ $(R-I)-\Delta \phi$
c+f -0.1 -0.2 0.0
c -0.3 -0.3 -0.2
  ${\rm Gini}-k_{3,5}/k_{1}$ ${\rm Gini}-\sigma_{\rm PA}$ ${\rm Gini}-\Delta \phi$
c+f -0.1 0.0 0.3
c 0.2 0.1 0.1
  M20-k3,5/k1 $M_{20}-\sigma_{\rm PA}$ $M_{20}-\Delta \phi$
c+f 0.1 0.2 0.0
c 0.1 0.3 0.5 (Fig. 11a)
  $\log(M_{*}[M_{\odot}])-k_{3,5}/k_{1}$ $\log(M_{*}[M_{\odot}])-\sigma_{\rm PA}$ $\log(M_{*}[M_{\odot}])-\Delta \phi$
c+f -0.3 -0.2 -0.4
c -0.2 0.0 -0.3

Notes. The figures where $\Delta \phi $ of the galaxies that have $\epsilon \leq 0.1$(galaxies 1F2, 2F4, 2F12 and 4C3 in ``this sample'', NGC 628, NGC 3184, NGC 3938 and NGC 5713 in the local sample), k3,5/k1 of galaxy 1F5 (this sample) and all parameters for galaxies 1F10, 2F5, 2F11 and 2F15&16 (this sample) are doubtful as explained in Paper III for the MS 0451 sample and here, in Sect. 3.8 for the rest. Therefore, they are excluded while calculating the correlation coefficients. For the calculation of the correlations with the redshift, only field galaxies were used, so the results do not have the bias of the environment.


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