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Supermassive black holes (SMBHs) of 10^9-10^10 Msun were already in place ~13Gyr ago, at z>6. Super-Eddington growth of low-mass BH seeds (~100 Msun) orless extreme accretion onto ~10^5 Msun seeds have been recently considered asthe main viable routes to these SMBHs. Here we study the statistics of theseSMBH progenitors at z~6. The growth of low- and high-mass seeds and their hostgalaxies are consistently followed using the cosmological data constrainedmodel GAMETE/QSOdust, which reproduces the observed properties of high-zquasars, like SDSS J1148+5251. We show that both seed formation channels can bein action over a similar redshift range, 15 < z < 18 and are found in darkmatter halos with comparable mass, ~5x10^7 Msun. However, as long as thesystems evolve in isolation (i.e. no mergers occur), noticeable differences intheir properties emerge: at z>= 10 galaxies hosting high-mass seeds havesmaller stellar mass and metallicity, the BHs accrete gas at higher rates andstar formation proceeds less efficiently than in low-mass seeds hosts. At z<10these differences are progressively erased, as the systems experience minor ormajor mergers and every trace of the BH origin gets lost.

Chasing the observational signatures of seed black holes at z > 7: candidate statistics