Notes. The fractional luminosities (L_disk/L_bol) are from Appendix A.5. For detected disks, the estimates of the flux density at 1.33 mm (F_1.33mm), the disk radius (R_disk), the ring width (W_disk), the inclination (i), and the position angle (PA) parameters are the results of model fitting with the UVGULTIFIT tool. The quoted uncertainties of the flux densities are quadratic sums of the measurement errors (listed in brackets) and the absolute calibration error (which were conservatively assumed to be 10%). With the exception of HD 112532 and HD 145101, where an elliptical Gaussian and a point source model were used, respectively, we applied Gaussian ring models to fit the visibility data of the detected disks (Sect. 4.2). In the latter cases, the radius of the disk corresponds to the radius of the fitted ring, while for HD 112532 to the semimajor axis (0.5 FWHM_maj) of the best-fitting Gaussian model. For HD 152989, an alternative model consisting of two infinitesimally thin rings was also tested (Sect. 5.3). To estimate the flux density upper limits for non-detections, we followed the method described in Sect. 4.2. Column 9 lists the derived dust masses (Sect. 4.3). ^(a)In the case of HD 31305, a significant fraction or even all of the observed excess of the system probably comes from the disk around the late-type companion, HD 31305 B. Due to the low spatial resolution of the available IR data, the fractional luminosity of the disk around HD 31305 A (if it exists at all) cannot be constrained. The last column shows which label we use to mark the given object in Figs. 7–9.