Sketches of the natural weighting of the synthesized wide-field visibilities. Each measured spatial frequency will produce wide-field spatial frequencies apodized by the transfer function () centered on the measured spatial frequency. The used transfer function depends on the telescopes used, explaining why wide-synthesis naturally handles the short spacing either from a single-dish antenna or from a heterogeneous array. The synthesized visibilities in the overlapping regions will then be averaged. Two textbook examples are illustrated: 1) the combination of data from the IRAM-30 m single-dish (red transfer function) and from the Plateau de Bure Interferometer (black transfer functions) at the top; and 2) the combination of data from ALMA 12 m-antennas used either in single-dish mode (red transfer function), in interferometric mode (black transfer functions) and of data from the ACA 7 m-antennas (blue transfer functions) at the bottom. The minimum uv distances measured by each interferometer were set from the minimum possible distance between antennas (24 m for PdBI, 15 m for ALMA and 9 m for ACA).