The origin of protostellar jets, and their role in extracting angular momentum from the accreting system, remain major open questions in star formation research. We explore the possibility that molecular jets may trace dusty magneto-hydrodynamic (MHD) centrifugal disk winds, the possibility they explain the broad component observed with Herschel in H2O lines and the high angular resolution observations of molecular jets. Our model includes~: 1) A self-similar MHD-solution that fits the atomic observations of DG Tau. 2) A non-equilibrium thermo-chemical and ionization gas evolution along streamlines with a network of 134 species. 3) Heating by ambipolar diffusion, irradiation by coronal X-rays and far UV photons from the accretion shock. 4) Non-local self-shielding of H2 and CO. 5) Non equilibrium integration of 40 rovibrational levels of H2, 40 rotational levels of CO, and 80 rotational levels of H2O under the escape probability formalism. 6) water and CO IR-pumping by the dust radiation field and dust thermal profile both calculated using DUSTY. 7) Projection of the anisotropic escape probability along observer's direction. In this unprecedented work, for the first time a dynamical disk wind model is able to make synthetic predictions in molecular lines of Class 0 to class II jet for comparison with observations. We build a powerful tool that could be used with ALMA and VLT observations.
