Table 1: Spectral-type content of the volume limited samples. Each sample spans a one magnitude range, and overlaps by 0.5 mag with the next one. M_B corresponds to the central value of the magnitude in each bin.

$M_{\rm B}$ $N_{\rm T1}$ $N_{\rm T2}$ $N_{\rm T3+T4}$ $N_{\rm tot}$

-22.0 782 249 41 1072

-21.5
1865 699 144 2708

-21.0
2703 1395 421 4519

-20.5
2732 1908 828 5468

-20.0
2134 1860 1100 5094

-19.5
1194 1183 918 3295

-19.0
543 692 773 2008

-18.5
277 467 663 1407

-18.0
158 327 451 936

-17.5
77 189 276 542

**Table 1:** Spectral-type content of the volume limited samples. Each sample spans a one magnitude range, and overlaps by 0.5 mag with the next one. M_B corresponds to the central value of the magnitude in each bin.
$M_{\rm B}$	$N_{\rm T1}$	$N_{\rm T2}$	$N_{\rm T3+T4}$	$N_{\rm tot}$
-22.0	782	249	41	1072
-21.5	1865	699	144	2708
-21.0	2703	1395	421	4519
-20.5	2732	1908	828	5468
-20.0	2134	1860	1100	5094
-19.5	1194	1183	918	3295
-19.0	543	692	773	2008
-18.5	277	467	663	1407
-18.0	158	327	451	936
-17.5	77	189	276	542

Source LaTeX | All tables | In the text

	1 Introduction
	2 The sample
	3 The dependence on luminosity of the satellite-density distribution
	4 The dependence on satellite-density of the spectral-type/luminosity relation
	5 The role of satelite density for passive and SF galaxies
	6 The dependence on luminosity of the spectral-type/neighbour density relation
	7 Summary and conclusions
	References