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There is a correlation between bulge mass of the three main galaxies of theLocal Group (LG), i.e. M31, Milky Way (MW), and M33, and the number of theirdwarf spheroidal galaxies. A similar correlation has also been reported forspiral galaxies with comparable luminosities outside the LG. These correlationsdo not appear to be expected in standard hierarchical galaxy formation. In thiscontribution, and for the first time, we present a quantitative investigationof the expectations of the standard model of cosmology for this possiblerelation using a galaxy catalogue based on the Millennium-II simulation. Ourmain sample consists of disk galaxies at the centers of halos with a range ofvirial masses similar to M33, MW, and M31. For this sample, we find an averagetrend (though with very large scatter) similar to the one observed in the LG;disk galaxies in heavier halos on average host heavier bulges and larger numberof satellites. In addition, we study sub-samples of disk galaxies with verysimilar stellar or halo masses (but spanning a range of 2-3 orders of magnitudein bulge mass) and find no obvious trend in the number of satellites vs. bulgemass. We conclude that while for a wide galaxy mass range a relation arises(which seems to be a manifestation of the satellite number - halo masscorrelation), for a narrow one there is no relation between number ofsatellites and bulge mass in the standard model. Further studies are needed tobetter understand the expectations of the standard model for this possiblerelation.

The number of dwarf satellites of disk galaxies versus their bulge mass in the standard model of cosmology