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We use PIONIER data from the ESO archive and GRAVITY data that were obtainedin June 2017 with the four 8m telescopes. We use a parametric disk model andthe 3D radiative transfer code MCFOST to reproduce the Spectral EnergyDistribution and match the interferometric observations. To match the SED , ourmodel requires a stellar luminosity of 2.5 Lsun, higher than any previouslydetermined values. Such a high value is needed to accommodate the circumstellarextinction caused by the highly inclined disk, which has been neglected inprevious studies. While using an effective temperature of 4800 K determinedthrough high-resolution spectroscopy, we derive a stellar radius of 2.29 Rsun.These revised fundamental parameters, when combined with the mass estimatesavailable , lead to an age of 0.5-2.0 Ma for RY Lup, in better agreement withthe age of the Lupus association than previous determinations. Our disk modelnicely reproduces the interferometric GRAVITY data and is in good agreementwith the PIONIER ones. We derive an inner rim location at 0.12~au from thecentral star. This model corresponds to an inclination of the inner disk of50deg, which is in mild tension with previous determinations of a more inclinedouter disk from SPHERE (70 deg in NIR) and ALMA(67 $\pm$5 deg) images, butconsistent with the inclination determination from the ALMA CO spectra(55$\pm$5deg). Increasing the inclination of the inner disk to 70 deg leads toa higher line-of-sight extinction and therefore requires a higher stellarluminosity of 4.65 Lsun to match the observed flux levels. This luminositywould translate to a stellar radius of 3.13~Rsun, leading to an age of 2-3~Ma,and a stellar mass of about 2 Msun, in disagreement with the observed dynamicalmass estimate of 1.3-1.5 Msun. Critically, this high-inclination inner diskmodel also fails to reproduce the visibilities observed with GRAVITY.

The GRAVITY young stellar object survey III. The dusty disk of RY Lup