{"paper":{"title":"A UV-to-NIR Study of Molecular Gas in the Dust Cavity Around RY Lupi","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. Banzatti, A. Miotello, C.F. Manara, C. Walsh, E.F. van Dishoeck, H.M. G\\\"unther, J.M. Alcal\\'a, J.P. Williams, K. France, K. Hoadley, N. Arulanantham, N. Van der Marel, P.C. Schneider","submitted_at":"2018-02-14T19:00:01Z","abstract_excerpt":"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 "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1802.05275","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}