Falomo (1996) & R & 11 & 0.143$\pm$0.082 & -26.3$\pm$2.1 & -26.0$\pm$0.6\
BL Wurtz (1996) & r & 35 & 0.266$\pm$0.162 & -24.5$\pm$2.3 & -26.3$\pm$0.7\
BL Falomo (1997b), Jannuzi (1997) & I & 6 & 0.351$\pm$0.172 & -26.0$\pm$0.8 & -26.0$\pm$0.8\
& & & & &\
RG Fasano (1996) & R & 25 & 0.061$\pm$0.027 & & -26.6$\pm$0.6\
RG low–z Zirbel (1996) & V & 55 & 0.107$\pm$0.047 & &-25.8$\pm$0.6\
RG F–R II high–z Zirbel (1996) & V & 25 & 0.389$\pm$0.053 & & -25.9$\pm$0.4\
RG F–R II Taylor (1996) & K & 12 & 0.214$\pm$0.049 & -25.1$\pm$0.7 & -26.1$\pm$0.8\
& & & & &\
FSRQ/R+M KFS98 & H & 9 & 0.671$\pm$0.157 & -29.7$\pm$0.8 & -26.7$\pm$1.2\
FSRQ/R KFS98 & H & 4 & 0.673$\pm$0.141 & -30.2$\pm$0.7 & -27.8$\pm$0.3\
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In Fig. 5 (upper panel) we show the H–z (Hubble) diagram for the BL Lac hosts (this work), together with data for FSRQs (KFS98) and F–R II RGs (Taylor 1996), compared to the established relation for RGs (solid line; Lilly & Longair 1984; Lilly, Longair & Miller 1985; Eales 1997), and the evolutionary model for elliptical galaxies derived from passive stellar evolution models (Bressan, Chiosi & 