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Using the deepest and the most complete set of observations of distantgalaxies, we investigate how extended disks could have formed. Observationsinclude spatially-resolved kinematics, detailed morphologies and photometryfrom UV to mid-IR. Six billion years ago, half of the present-day spiralprogenitors had anomalous kinematics and morphologies, as well as relativelyhigh gas fractions. We argue that gas-rich major mergers, i.e., fusions betweengas-rich disk galaxies of similar mass, can be the likeliest driver for suchstrong peculiarities. This suggests a new channel of disk formation, e.g. manydisks could be reformed after gas-rich mergers. This is found to be in perfectagreement with predictions from the state-of-the-art LCDM semi-empiricalmodels: due to our sensitivity in detecting mergers at all phases, from pairsto relaxed post-mergers, we find a more accurate merger rate. The scenario canbe finally confronted to properties of nearby galaxies, including M31 andgalaxies showing ultra-faint, gigantic structures in their haloes.

The Formation of Large Galactic Disks: Revival or Survival?