A UV-to-NIR Study of Molecular Gas in the Dust Cavity around RY Lupi
Journal
Date Issued
2018
Author(s)
Arulanantham, N.
•
France, K.
•
Hoadley, K.
•
Manara, C. F.
•
Schneider, P. C.
•
•
Banzatti, A.
•
Günther, H. M.
•
Miotello, A.
•
van der Marel, N.
•
van Dishoeck, E. F.
•
Walsh, C.
•
Williams, J. P.
Abstract
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 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}}broad,{{{H}}}2}=105 +/- 15 {km} {{{s}}}-1{FWHM}}narrow,{{{H}}}2}=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,{{{H}}}2}> ∼ 0.4+/- 0.1 {au};< {r}narrow,{{{H}}}2}> ∼ 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.
Volume
855
Issue
2
Start page
98
Issn Identifier
0004-637X
Ads BibCode
2018ApJ...855...98A
Rights
open.access
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