Satellite galaxies around present-day massive ellipticals

Using the spectroscopic New York University Value-Added Galaxy Catalogue and the photometric photo-z catalogues of the Sloan Digital Sky Survey Data Release 7, we have explored the satellite distribution around similar to 1000 massive (M-* greater than or similar to 2 x 10(11) M-circle dot) visually classified elliptical galaxies down to a satellite mass ratio of 1:400 (i.e. 5 x 10(8) less than or similar to M-sat less than or similar to 2 x 10(11) M-circle dot). Our host galaxies were selected to be representative of a mass complete sample. The satellites of these galaxies were searched within a projected radial distance of 100 kpc to their hosts. We have found that only 20-23 per cent of the massive ellipticals have at least a satellite down to a mass ratio 1:10. This number increases to 45-52 per cent if we explore satellites down to 1: 100 and is >60-70 per cent if we go further down to 1:400. The average projected radial distance of the satellites to their hosts for our whole sample down to 1: 400 is similar to 59 kpc (which can be decreased at least down to 50 kpc if we account for incompleteness effects). The number of satellites per galaxy host only increases very mildly at decreasing the satellite mass. The fraction of mass which is contained in the satellites down to a mass ratio of 1: 400 is 8 per cent of the total mass contained by the hosts. Satellites with a mass ratio from 1: 2 to 1: 5 (with similar to 28 per cent of the total mass of the satellites) are the main contributor to the total satellite mass. If the satellites eventually infall into the host galaxies, the merger channel will be largely dominated by satellites with a mass ratio down to 1:10 (as these objects have 68 per cent of the total mass in satellites).