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Debate over the planet occurrence rates around intermediate-mass stars hashinged on the accurate determination of masses of evolved stars, and has beenexacerbated by a paucity of reliable, directly-measured fundamental propertiesfor these stars. We present long-baseline optical interferometry of fiveevolved intermediate-mass ($\sim\,1.5\,\mathrm{M}_\odot$) planet-hosting starsusing the PAVO beam combiner at the CHARA Array, which we combine withbolometric flux measurements and parallaxes to determine their radii andeffective temperatures. We measured the radii and effective temperatures of 6Lyncis ($5.12\pm0.16\,\mathrm{R}_\odot$, $4949\pm58\,\mathrm{K}$), 24 Sextantis($5.49\pm0.18\,\mathrm{R}_\odot$, $4908\pm65\,\mathrm{K}$), $\kappa$ CoronaeBorealis ($4.77\pm0.07\,\mathrm{R}_\odot$, $4870\pm47\,\mathrm{K}$), HR 6817($4.45\pm0.08\,\mathrm{R}_\odot$, $5013\pm59\,\mathrm{K}$), and HR 8641($4.91\pm0.12\,\mathrm{R}_\odot$, $4950\pm68\,\mathrm{K}$). We finddisagreements of typically 15 per cent in angular diameter and $\sim$200 K intemperature compared to interferometric measurements in the literature, yetgood agreement with spectroscopic and photometric temperatures, concluding thatthe previous interferometric measurements may have been affected by systematicerrors exceeding their formal uncertainties. Modelling based on BaSTIisochrones using various sets of asteroseismic, spectroscopic, andinterferometric constraints tends to favour slightly ($\sim$15 per cent) lowermasses than generally reported in the literature.

Interferometric diameters of five evolved intermediate-mass planet-hosting stars measured with PAVO at the CHARA Array