All Figures

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{1448fig1a.eps}\par\includegraphics[width=7.3cm,clip]{1448fig1b.eps} \end{figure}$ Figure 1: Relative distributions of passive (type 1), quiet-SF (type 2), active-SF (type 3 + 4) and all-type galaxies as a function of number of fainter neighbours (in 4 intervals), for the 10 volume limited samples. Numbers are normalized to the total number of galaxies of a given type: for each spectral type the sum over all environments is 1. The number of neighbour distribution, in the all-type galaxy sample, undergoes no significant modification with luminosity.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1448fig2.eps} \end{figure}$ Figure 2: The relative content in passive, quiet-SF and active-SF galaxies in the 10 volume-limited samples. Error bars are multinomial. The 40% fraction line is drawn to reveal "dominant'' populations. Passive galaxies dominate in bright samples, active-SF galaxies in faint samples, quiet-SF galaxies are never dominant. The contribution of the 3 populations is comparable in the M_B - 5 $\log$ h₇₅ $\in$ [ $-20 \div -19$ ] range.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1448fig3.eps} \end{figure}$ Figure 3: Relative content in passive, quiet-SF and active-SF galaxies in the 10 volume-limited samples (symbols as in Fig. 2). Each panel refers to galaxies in a specific neighbour density bin. The absence of satellites (neigh = 0) efficiently reduces the dominance of passive galaxies in luminous samples, raising the contribution of quiet-SF galaxies. Conversely, a high density environment (neigh > 8) significantly enhances the contribution of passive galaxies in faint samples.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1448fig4.eps} \end{figure}$ Figure 4: Relative content in passive ( top-left), quiet-SF ( top-right) and active-SF ( bottom-left) galaxies in samples of galaxies in different environments. Continuum lines are used to connect galaxy fractions with 0 and >8 neighbours, dotted and hatched lines to connect galaxy fractions in intermediate dense environments (1 $\leq$ neigh $\leq$ 2 and 3 $\leq$ neigh $\leq$ 8).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1448fig5.eps} \end{figure}$ Figure 5: The spectral-type/satellite-density relation for passive, quiet-SF and active-SF galaxies in the 9 brightest samples. Symbols are as in Fig. 2, small dots indicate the cumulative contribution of active and quiet-SF galaxies. Fractions have been computed using values listed in Table 2, normalized to the total number of galaxies in a given density bin so that, in each environment, the sum over all spectral types is 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1448fig4.eps} \end{figure}$	Figure 4: Relative content in passive ( top-left), quiet-SF ( top-right) and active-SF ( bottom-left) galaxies in samples of galaxies in different environments. Continuum lines are used to connect galaxy fractions with 0 and >8 neighbours, dotted and hatched lines to connect galaxy fractions in intermediate dense environments (1 $\leq$ neigh $\leq$ 2 and 3 $\leq$ neigh $\leq$ 8).
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