| Résumé | We present a study of molecular gas in the inner disk (r < 20au) 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 Lyα-pumped H2. The result shows H2 emission originating in a ring centered at ~3 au that declines within r < 0.1 au, which is consistent with the behavior of disks with dust cavities. An analysis of the H2 line shapes shows that a two-component Gaussian profile $(FWHM mathrm,H2=105 +- 15 km s ^-1; FWHM mathrm,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} ~0.4 +- 0.1 au; {r narrow,H2} ~ 3 +- 2 au). The 4.7 μm 12CO 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 μm 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. |
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