The abundance of satellites depends strongly on the morphology of the
  host galaxy
  Using the spectroscopic catalogue of the Sloan Digital Survey Data Release
10, we have explored the abundance of satellites around a sample of 254 massive
(10^11< M_star < 2 x 10^11 M_sun) local (z < 0.025) galaxies. We have divided
our sample into four morphological groups (E, S0, Sa, Sb/c). We find that the
number of satellites with M_star > 10^9 M_sun and R < 300 kpc depends
drastically on the morphology of the central galaxy. The average number of
satellites per galaxy host (N_Sat/N_Host) down to a mass ratio of 1:100 is 4.5
+/- 0.3 for E hosts, 2.6 +/- 0.2 for S0, 1.5 +/- 0.1 for Sa and 1.2 +/- 0.2 for
Sb/c. The amount of stellar mass enclosed by the satellites around massive
E-type galaxies is a factor of 2, 4 and 5 larger than the mass in the
satellites of S0, Sa and Sb/c types, respectively. If these satellites would
eventually infall into the host galaxies, for all the morphological types, the
merger channel will be largely dominated by satellites with a mass ratio
satellite-host $\mu$ > 0.1. The fact that massive elliptical galaxies have a
significant larger number of satellites than massive spirals could point out
that elliptical galaxies inhabit heavier dark matter haloes than equally
massive galaxies with later morphological types. If this hypothesis is correct,
the dark matter haloes of late-type spiral galaxies are a factor ~2-3 more
efficient on producing galaxies with the same stellar mass than those dark
matter haloes of early-type galaxies.
