Best-fit parameters for the debris disks listed in Table G.1. Panel a: comparison of the measured ($R_{\text{belt}}^{\text{mex}}$) and modeled ($R_{\text{belt}}^{\text{mod}}$) radial distances of the planetesimal belts. The empirical fit is shown by the black solid line, which coincides with the 1:1 relation. The blue-shaded area represents the uncertainty on the slope of the fit. Panel b: HG asymmetry parameter g versus disk inclination. Panel c: exponent of the inner radial power law α_in as a function of stellar luminosity. Open circles show the exponents obtained by modeling the total intensity images of the HD 114082, HD 117214 and HD 131488 disks. Panel d: disk aspect ratio versus radius of the planetesimal belt. Debris disks with unresolved FWHM are marked with open symbols. Gas-rich systems are indicated by triangles. The blue solid line represents the theoretical scale height value of 0.04 for a collisionally excited debris disk, while the blue-shaded area indicates its associated uncertainty (Thebault 2009). The red ellipse encloses targets HD 106906, HD 115600 and HD 129590. Panel e: disk aspect ratio versus stellar luminosity. Marker symbols are the same as in panel d. Panel f: exponent of the outer radial power law α_out as a function of stellar luminosity. The solid horizontal line indicates the value α_out = −2.5, as theoretically predicted for the outer regions of debris disks (Strubbe & Chiang 2006; Thebault et al. 2023).