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Using the spectroscopic catalogue of the Sloan Digital Survey Data Release10, 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 dividedour sample into four morphological groups (E, S0, Sa, Sb/c). We find that thenumber of satellites with M_star > 10^9 M_sun and R < 300 kpc dependsdrastically on the morphology of the central galaxy. The average number ofsatellites 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 forSb/c. The amount of stellar mass enclosed by the satellites around massiveE-type galaxies is a factor of 2, 4 and 5 larger than the mass in thesatellites of S0, Sa and Sb/c types, respectively. If these satellites wouldeventually infall into the host galaxies, for all the morphological types, themerger channel will be largely dominated by satellites with a mass ratiosatellite-host $\mu$ > 0.1. The fact that massive elliptical galaxies have asignificant larger number of satellites than massive spirals could point outthat elliptical galaxies inhabit heavier dark matter haloes than equallymassive galaxies with later morphological types. If this hypothesis is correct,the dark matter haloes of late-type spiral galaxies are a factor ~2-3 moreefficient on producing galaxies with the same stellar mass than those darkmatter haloes of early-type galaxies.

The abundance of satellites depends strongly on the morphology of the host galaxy