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We use an adaptation of the BzKs technique to select ~40,000 z~2 galaxies (toK(AB) = 24), including ~5,000 passively evolving (PE) objects (to K(AB) = 23),from 2.5 deg^2 of deep CFTH imaging. The passive galaxy luminosity functionexhibits a clear peak at R = 22 and a declining faint-end slope ({\alpha} = -0.12 [+0.16 -0.14]),while that of star-forming galaxies is characterized by asteep faint-end slope ({\alpha} = -1.43 +- [0.02] (systematic) [+0.05 -0.04](random)). The details of the LFs are somewhat sensitive (at <25% level) tocosmic variance even in these large(~0.5 deg^2) fields, with the D2 field(located in the COSMOS field) most discrepant from the mean. The shape of the z~ 2 stellar mass function of passive galaxies is remarkably similar to that atz ~ 0.9, save for a factor of ~4 lower number density. This similarity suggeststhat the same mechanism may be responsible for the formation of passivegalaxies seen at both these epochs. This same formation mechanism may alsooperate down to z ~ 0 if the local PE galaxy mass function, known to betwo-component, contains two distinct galaxy populations. This scenario isqualitatively in agreement with recent phenomenological mass-quenching modelsand extends them to span more than three quarters of the history of theUniverse.

The numbers of z~2 star-forming and passive galaxies in 2.5 square degrees of deep CFHT imaging