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 $\left(r < 20 \,
\text{AU} \right)$ 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 $\sim$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 $\left(\text{FWHM}_{broad, H_2} = 105 \pm 15 \, \text{km
s}^{-1}; \, \text{FWHM}_{narrow, H_2} = 43 \pm 13 \, \text{km s}^{-1} \right)$
is statistically preferred to a single-component Gaussian. We interpret this as
tentative 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 fit
by 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 $\mu$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.
