A UV-to-NIR Study of Molecular Gas in the Dust Cavity Around RY Lupi
arXiv:1802.05275 · doi:10.3847/1538-4357/aaaf65
Abstract
We present a study of molecular gas in the inner disk 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 AU, as traced by Ly-pumped H. The result shows H emission originating in a ring centered at 3 AU that declines within AU, which is consistent with the behavior of disks with dust cavities. An analysis of the H line shapes shows that a two-component Gaussian profile is statistically preferred to a single-component Gaussian. We interpret this as tentative evidence for gas emitting from radially separated disk regions . The 4.7 m CO emission lines are also well fit by two-component profiles . We combine these results with 10 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.
arXiv commentAccepted for publication in ApJ
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