Dirty images of the raw (left), model (center), and residual (right) data of VACA LoCA observations. All the images are generated by applying a multi-frequency naturally weighted, imaging scheme, and extend out to where the ACA primary beam reaches 20% of its peak amplitude. To better highlight the SZ features in each field a 10 kλ taper is applied, but without correction for the primary beam attenuation. Furthermore, as in Fig. 3, the most significant point-like sources from the raw interferometric data are removed.