166$^{+7.8}_{-3.9}$ (151$^{+77.7}_{-107}$) & 1.6$^{+0.6}_{-0.2}$ (1.5$^{+0.2}_{-0.2}$) & 9.3$^{+0.0}_{-0.1}$ (9.2$^{+0.1}_{-0.4}$)\
A2-24511 & 25.32 & 22.97 & 21.89$\pm$0.09 & 3.76$^{+0.17}_{-0.12}$ & 11.68$^{+0.11}_{-0.10}$ (11.38$^{+0.28}_{-0.36}$) & 170$^{+298}_{-125}$ (97.7$^{+594}_{-97.7}$) & 1.4$^{+0.2}_{-0.2}$ (1.3$^{+0.4}_{-0.6}$) & 8.9$^{+0.3}_{-0.2}$ (8.4$^{+0.4}_{-0.7}$)\

The redshift-dependent completeness limit in stellar mass has been estimated following the approach described in detail in @marchesini09, which exploits the availability of samples with different depths. The completeness of a sample is estimated empirically from the available deeper samples, namely, the FIRES (@labbe03; @forster06) and the FIREWORKS [@wuyts08] catalogs. Briefly, to estimate the redshift-dependent stellar mass completeness limit of the NMBS sample, we first selected galaxies belonging to the available deeper samples. Then, we scaled their fluxes and stellar masses to match the $K$-band completeness limit of the NMBS sample. The upper envelope of points in the ($M_{\rm star,scaled}-z$) space, encompassing 95% of the points, represents the most massive galaxies at the considered flux limit ($K=23.15$ for the NMBS catalog adopted in this work), and so provides a redshift-dependent stellar mass completeness limit for the NMBS sample. We refer to @marchesini09 for a detailed description of this method. The resulting completeness in mass of the NMBS catalog used in this work is $M_{\rm star} = 10^{11.40}$ M$_{\sun}$ $\approx 2.5\times10^{11}$ M$_{\sun}$ 