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We investigate the morphological properties of 494 galaxies selected from theGMASS survey at z>1, primarily in their optical rest frame, using HST images,from the CANDELS survey. We propose that the Hubble sequence of galaxymorphologies takes shape at redshift 2.5<z<3. The fractions of both ellipticalsand disks decrease with increasing lookback time at z>1, such that at redshiftsz=2.5-2.7 and above, the Hubble types cannot be identified, and most galaxiesare classified as irregular. The quantitative morphological analysis showsthat, at 1<z<3, morphological parameters are not as effective in distinguishingthe different morphological Hubble types as they are at low redshift. Nosignificant morphological k-correction was found to be required for the Hubbletype classification, with some exceptions. In general, different morphologicaltypes occupy the two peaks of the rest-frame (U-B) colour bimodality ofgalaxies: most irregulars occupy the blue peak, while ellipticals are mainlyfound in the red peak, though with some level of contamination. Disks are moreevenly distributed than either irregulars and ellipticals. We find that theposition of a galaxy in a UVJ diagram is related to its morphological type: the"quiescent" region of the plot is mainly occupied by ellipticals and, to alesser extent, by disks. We find that only ~33% of all morphologicalellipticals in our sample are red and passively evolving galaxies. Bluegalaxies morphologically classified as ellipticals show a remarkable structuralsimilarity to red ones. Almost all irregulars have a star-forming galaxyspectrum. In addition, the majority of disks show some sign of star-formationactivity in their spectra, though in some cases their red continuum isindicative of old stellar populations. Finally, an elliptical morphology may beassociated with either passively evolving or strongly star-forming galaxies.

Listening to galaxies tuning at z ~ 2.5 - 3.0: The first strikes of the Hubble fork