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We use a deep K(AB)<25 galaxy sample in the Hubble Deep Field South to tracethe evolution of the cosmological stellar mass density from z~ 0.5 to z~3. Wefind clear evidence for a decrease of the average stellar mass density at highredshift, 2<z<3.2, that is 15^{+25}_{-5}% of the local value, two times higherthan what observed in the Hubble Deep Field North. To take into account for theselection effects, we define a homogeneous subsample of galaxies with10^{10}M_\odot \leq M_* \leq 10^{11}M_\odot: in this sample, the mass densityat z>2 is 20^{+20}_{-5} % of the local value. In the mass--limited subsample atz>2, the fraction of passively fading galaxies is at most 25%, although theycan contribute up to about 40% of the stellar mass density. On the other hand,star--forming galaxies at z>2 form stars with an average specific rate at least<\dot M/M_*> ~4 x10^{-10} yr$^{-1}$, 3 times higher than the z<~1 value. Thisimplies that UV bright star--forming galaxies are substancial contributors tothe rise of the stellar mass density with cosmic time. Although these resultsare globally consistent with $\Lambda$--CDM scenarios, the present rendition ofsemi analytic models fails to match the stellar mass density produced by moremassive galaxies present at z>2.Comment: Accepted for publication on ApJLetter

The Assembly of Massive Galaxies from Near-Infrared Observations of the Hubble Deep Field-South