  Long baseline interferometry is now able to resolve the pulsational change of
the angular diameter of a significant number of Cepheids in the solar
neighborhood. This allows the application of a new version of the
Baade-Wesselink (BW) method to measure their distance, for which we do not need
to estimate the star's temperature. Using angular diameter measurements from
the VLT Interferometer, we derived the distances to four nearby Cepheids. For
three additional stars, we obtained average values of their angular diameters.
Based on these new measurements and already existing data, we derived
calibrations of the Period-Luminosity and Period-Radius relations. We also
obtained reliable surface brightness-color relations, that can be employed for
the infrared surface brightness version of the BW method.
