{"paper":{"title":"Candidate Water Vapor Lines to Locate the $\\mathrm{H_2O}$ Snowline through High-dispersion Spectroscopic Observations. III. Submillimeter $\\mathrm{H_2}$$^{16}\\mathrm{O}$ and $\\mathrm{H_2}$$^{18}\\mathrm{O}$ Lines","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Catherine Walsh, Eiji Akiyama, Hideko Nomura, Mitsuhiko Honda, Shota Notsu, T. J. Millar, Tomoya Hirota","submitted_at":"2018-01-23T08:38:25Z","abstract_excerpt":"In this paper, we extend the results presented in our former papers (Notsu et al. 2016, 2017) on using ortho-$\\mathrm{H_2}$$^{16}\\mathrm{O}$ line profiles to constrain the location of the $\\mathrm{H_2O}$ snowline in T Tauri and Herbig Ae disks, to include sub-millimeter para-$\\mathrm{H_2}$$^{16}\\mathrm{O}$ and ortho- and para-$\\mathrm{H_2}$$^{18}\\mathrm{O}$ lines. Since the number densities of the ortho- and para-H$_{2}$$^{18}$O molecules are about 560 times smaller than their $^{16}$O analogues, they trace deeper into the disk than the ortho-H$_{2}$$^{16}$O lines (down to $z=0$, i.e., the mid"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1801.07437","kind":"arxiv","version":2},"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"}