Table 2: n1 and n3 estimators of the amplitude $\phi _0$ of the Gaussian component of the early-type, intermediate-type, and late-type luminosity functions for the ESO-Sculptor redshift survey, in the Johnson B, V and Cousins $R_{\rm c}$ bands.
Sample Early-type Intermediate-type Late-type
    $\Phi_1(0.51)$    $\Phi_3(0.51)$    $\Phi_1(0.51)$    $\Phi_3(0.51)$   $\Phi_1(z)$    $\Phi_1(0.51)$    $\Phi_3(0.51)$ 
$R_{\rm c}\le 21.5$   0.00333   0.00339   0.00326   0.00312    0.00194[1+3.51(z-0.15)]  0.00439 0.00328
$R_{\rm c} \le 20.5$   0.00324   0.00331   0.00351   0.00321    0.00177[1+4.45(z-0.15)]   0.00462   0.00319 
$V\le 21.0$   0.00322   0.00335   0.00379   0.00314    0.00141[1+7.52(z-0.15)]   0.00521   0.00309 
$B\le 22.0$   0.00286   0.00363   0.00357   0.00325    0.00135[1+8.59(z-0.15)]   0.00551   0.00333 
Notes:
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The listed values of the luminosity function amplitude $\phi _0$ are in units of  h3 Mpc-3 mag-1, and are obtained with  H0 = 100  h km s-1 Mpc-1,  $\Omega _{\rm m}=0.3$, and  $\Omega _\Lambda =0.7$.
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The corresponding amplitude $\phi ^*$ of the Schechter component for the intermediate-type and late-type galaxies can be derived using the values of the ratio  $\phi_0/0.4\ln10\;\phi^*$ listed in Table 1.
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The $\Phi_1(z)$ parameterization of the evolving amplitude $\phi _0$ for the late-type galaxies should be used with caution (especially in the V and B bands); more realistic parameterizations are obtained in the $R_{\rm c}$, V and B bands from the adjustment of the number counts (see Table 4, Sect. 6).

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