  Up to now, the completion of an ALMA interferometric observation is
determined based on the achievement of a given shape and size of the
synthesized beam and the noise RMS in the representative spectral range. This
approach with respect to the angular resolution investigates mainly the longest
baselines of the interferometer and says little about the sensitivity at larger
angular scales. We are exploring the ideas of angular-scale-based scheduling
and quality assessment, and of angular-scale-based visibility weighting as a
step towards optimising both observation efficiency and image fidelity. This
approach carries the imaging quality assurance into the visibility space where
interferometers record the data, and therefore simplifies many aspects of the
procedure. Similarly, during scheduling such detailed assessment of the
expected imaging properties helps optimising the scheduling process. The
methodology is applicable to all radio interferometers with more than ca. 10
antennas.
