{"paper":{"title":"A Detailed Study of the Molecular and Atomic Gas Toward the {\\gamma}-ray SNR RX J1713.7-3946: Spatial TeV {\\gamma}-ray and ISM Gas Correspondence","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Kawamura, A. Mizuno, G. Rowell, H. Horachi, H. Ogawa, H. Sano, H. Yamamoto, J. Sato, K. Torii, N. Mizuno, N. M. McClure-Griffiths, S. Inutsuka, T. Hayakawa, T. Inoue, T. Okuda, T. Onishi, Y. Fukui","submitted_at":"2011-07-04T00:45:07Z","abstract_excerpt":"RX J1713.7$-$3946 is the most remarkable TeV $\\gamma$-ray SNR which emits $\\gamma$-rays in the highest energy range. We made a new combined analysis of CO and \\ion{H}{1} in the SNR and derived the total protons in the interstellar medium (ISM). We have found that the inclusion of the \\ion{H}{1} gas provides a significantly better spatial match between the TeV $\\gamma$-rays and ISM protons than the H$_2$ gas alone. In particular, the southeastern rim of the $\\gamma$-ray shell has a counterpart only in the \\ion{H}{1}. The finding shows that the ISM proton distribution is consistent with the hadr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1107.0508","kind":"arxiv","version":4},"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"}