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

Arulanantham, N.N.ArulananthamFrance, K.K.FranceHoadley, K.K.HoadleyManara, C. F.C. F.ManaraSchneider, P. C.P. C.SchneiderALCALA', JUAN MANUELJUAN MANUELALCALA'Banzatti, A.A.BanzattiGünther, H. M.H. M.GüntherMiotello, A.A.Miotellovan der Marel, N.N.van der Marelvan Dishoeck, E. F.E. F.van DishoeckWalsh, C.C.WalshWilliams, J. P.J. P.Williams2020-10-142020-10-1420180004-637Xhttp://hdl.handle.net/20.500.12386/27787We 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.STAMPAenA UV-to-NIR Study of Molecular Gas in the Dust Cavity around RY LupiArticle10.3847/1538-4357/aaaf652-s2.0-85044046180000427362600014https://iopscience.iop.org/article/10.3847/1538-4357/aaaf652018ApJ...855...98AFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering