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

We present a study of molecular gas in the inner disk (r < 20 au) around RY Lupi, with spectra from HST-COS, HST-STIS, and VLT-CRIRES. We model the radial distribution of flux from hot gas in a surface layer between r = 0.1-10 au, as traced by Ly alpha-pumped H-2. The result shows H-2 emission originating in a ring centered at similar to 3 au that declines within r < 0.1 au, which is consistent with the behavior of disks with dust cavities. An analysis of the H-2 line shapes shows that a two-component Gaussian profile (FWHMbroad, (H2) = 105 +/- 15 km s(-1); FWHMnarrow, (H2) = 43 +/- 13 km s(-1)) is statistically preferred to a single-component Gaussian. We interpret this as tentative evidence for gas emitting from radially separated disk regions (< r(broad), (H2)> similar to 0.4 +/- 0.1 au; < r(narrow), (H2)> similar to 3 +/- 2 au). The 4.7 mu m (CO)-C-12 emission lines are also well fit by two-component profiles (< r(broad), (CO)> = 0.4 +/- 0.1 au; < r(narrow), (CO)> = 15 +/- 2 au). We combine these results with 10 mu m observations to form a picture of gapped structure within the mm-imaged dust cavity, 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.