Table 1: Correlations between mass structural parameters.
  $\Sigma _{\rm eff}$ vs. Log $r_{\rm eff}$   $\Sigma^{\rm o}_{\rm d}$ vs. Log $r_{\rm d}$   Log n vs. $\Sigma ^{\rm o}_{\rm b}$  
  a r   a r   a r a
Sim(z=0) 0.13 $\pm$ 0.01 0.94   0.13 $\pm$ 0.02 0.92   $-0.09 \pm 0.02$ -0.77  
Sim(z >0) 0.15 $\pm$ 0.01 0.90   0.14 $\pm$ 0.01 0.91   $-0.10 \pm 0.01$ -0.71  
K00b 0.15 $\pm$ 0.05 0.52   0.24 $\pm$ 0.06 0.65   $-0.08 \pm 0.01$ -0.88  
a Slopes of linear regressions ( y = ax + b) and Pearson linear correlation coefficients for the simulated galaxy-like objects at z=0 (Sim(z=0)), for their progenitors during merger events (Sim(z > 0)), and the observed bulges and discs of Khosrhoshahi et al. (2000b).

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