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We present a study of molecular gas in the inner disk $\left(r < 20 \,\text{AU} \right)$ around RY Lupi, with spectra from HST-COS, HST-STIS, andVLT-CRIRES. We model the radial distribution of flux from hot gas in a surfacelayer between $r = 0.1-10$ AU, as traced by Ly$\alpha$-pumped H$_2$. The resultshows H$_2$ emission originating in a ring centered at $\sim$3 AU that declineswithin $r < 0.1$ AU, which is consistent with the behavior of disks with dustcavities. An analysis of the H$_2$ line shapes shows that a two-componentGaussian profile $\left(\text{FWHM}_{broad, H_2} = 105 \pm 15 \, \text{kms}^{-1}; \, \text{FWHM}_{narrow, H_2} = 43 \pm 13 \, \text{km s}^{-1} \right)$is statistically preferred to a single-component Gaussian. We interpret this astentative evidence for gas emitting from radially separated disk regions$\left( \left \langle r_{broad, H_2} \right \rangle \sim 0.4 \pm 0.1 \,\text{AU}; \, \left \langle r_{narrow, H_2} \right \rangle \sim 3 \pm 2 \,\text{AU} \right)$. The 4.7 $\mu$m $^{12}$CO emission lines are also well fitby two-component profiles $\left( \left \langle r_{broad, CO} \right \rangle =0.4 \pm 0.1 \, \text{AU}; \, \left \langle r_{narrow, CO} \right \rangle = 15\pm 2 \, \text{AU} \right)$. We combine these results with 10 $\mu$mobservations to form a picture of gapped structure within the mm-imaged dustcavity, providing the first such overview of the inner regions of a young disk.The HST SED of RY Lupi is available online for use in modeling efforts.

A UV-to-NIR Study of Molecular Gas in the Dust Cavity Around RY Lupi