Notes. Collected observed properties of known HAeBe discs, including the discs from our sample = B15, the discs from van der Plas et al. (2015) = vdP, and discs from Salyk et al. (2011) = S11, where the FWHM have been taken from Blake & Boogert (2004) = B4 if indicated. The R_CO10% is the radius derived from the Keplerian velocity at the half width at 10% of the maximum in the averaged line profiles. The column labelled dust/gas consistent?, indicates whether there are inconsistencies between the dust inner radii based on the SED classification and gas radii based on the CO ro-vibrational emission lines. For HD 101412 and HD 104237, CO ro-vibrational lines were detected, but owing to blending and telluric residuals the FWHM could not be measured reliably. [30/13.5] values are taken from Table 1 of Maaskant et al. (2014). An asterisk after the inclination and mass indicates that in the absence of a measurement, a typical inclination consistent with the line profile shape and a stellar mass estimated from the spectral type was assumed. ^‡Blondel & Djie (2006) note the distance ambiguity and that this star is likely a spectroscopic double star.