  We present new models for low-mass stars down to the hydrogen-burning limit
that consistently couple atmosphere and interior structures, thereby
superseding the widely used BCAH98 models. The new models include updated
molecular linelists and solar abundances, as well as atmospheric convection
parameters calibrated on 2D/3D radiative hydrodynamics simulations. Comparison
of these models with observations in various colour-magnitude diagrams for
various ages shows significant improvement over previous generations of models.
The new models can solve flaws that are present in the previous ones, such as
the prediction of optical colours that are too blue compared to M dwarf
observations. They can also reproduce the four components of the young
quadruple system LkCa 3 in a colour-magnitude diagram with one single
isochrone, in contrast to any presently existing model. In this paper we also
highlight the need for consistency when comparing models and observations, with
the necessity of using evolutionary models and colours based on the same
atmospheric structures.
