1. Introduction  
2. Observations  
2.1. Photometry  
2.2. Interferometry  
3. Model fitting  
3.1. Model definition and spectral dependence  
3.2. Single star and background flux: s 0-1  
3.4. Binary: b 1-2  
3.5. Binary and a ring: br 1-5  
3.6. Strategy  
4. Results  
4.1. Results of the model selection  
4.2. Inner rim radius ruled by dust sublimation physics  
4.3. Dust temperature  
4.4. Disk inclinations  
4.5. Disk width  
4.6. Rim brightness distribution  
4.7. Extended flux statistics  
5. Discussion  
5.1. Outliers  
5.2. Origin of the shift between pAGBs and YSOs in the size luminosity relation  
5.3. Relation between the RVb phenomenon and disk inclination  
5.4. Comparison between near-infrared and mid-infrared sizes  
5.5. Continuing the comparison between pAGB and YSOs  
6. Conclusions