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Judging from the low NH$_{3}$/CCS ratios, they are possible candidates for \"Carbon-Chain--Producing Regions (CCPRs)\" recognized as chemically young dark cloud cores. The deuterium fractionation ratios DNC/HN$^{13}$C in CB130-3 and L673-SMM4 are found to be 1.28$^{+0.27}_{-0.05}$ and 1.96$^{+0.32}_{-0.01}$, respectively, which are comparable to or"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1105.0081","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2011-04-30T12:10:43Z","cross_cats_sorted":[],"title_canon_sha256":"c48eadc52f13ab88c2b9dcd12e3a511f8eacfb89b4a2794cd7ffa35a06074802","abstract_canon_sha256":"c97ca5fb4390e73aee9f5033a32d71f3c9bd095116a7501fe6f8c6f6ff0b2dd3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:02:10.752760Z","signature_b64":"3WCSFykV3rGsxlCijzd35Go6bOO3lrf3Fi3zNT3nvvMyQA3lTFH4EFgI5Pxxh1P3irBmwKvPGSeKtaHY/12UBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8a5eeba47e029060d54063b89ecac7f8be5080bfddd59cd70801c11ec6352ebc","last_reissued_at":"2026-05-18T02:02:10.752110Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:02:10.752110Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Detection of Two Carbon-Chain-Rich Cores; CB130-3 and L673-SMM4","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Nami Sakai, Satoshi Yamamoto, Takeshi Sakai, Tomoya Hirota","submitted_at":"2011-04-30T12:10:43Z","abstract_excerpt":"We have found two dense cores, CB130-3 and L673-SMM4, where the carbon-chain molecules are extremely abundant relative to NH$_{3}$, during a survey observation of radio emission lines of CCS, HC$_{3}$N, HC$_{5}$N, and NH$_{3}$ toward dark cloud cores. 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The deuterium fractionation ratios DNC/HN$^{13}$C in CB130-3 and L673-SMM4 are found to be 1.28$^{+0.27}_{-0.05}$ and 1.96$^{+0.32}_{-0.01}$, respectively, which are comparable to or"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1105.0081","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"},"aliases":[{"alias_kind":"arxiv","alias_value":"1105.0081","created_at":"2026-05-18T02:02:10.752233+00:00"},{"alias_kind":"arxiv_version","alias_value":"1105.0081v2","created_at":"2026-05-18T02:02:10.752233+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1105.0081","created_at":"2026-05-18T02:02:10.752233+00:00"},{"alias_kind":"pith_short_12","alias_value":"RJPOXJD6AKIG","created_at":"2026-05-18T12:26:41.206345+00:00"},{"alias_kind":"pith_short_16","alias_value":"RJPOXJD6AKIGBVKA","created_at":"2026-05-18T12:26:41.206345+00:00"},{"alias_kind":"pith_short_8","alias_value":"RJPOXJD6","created_at":"2026-05-18T12:26:41.206345+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.22090","citing_title":"Measuring Magnetic Field Strengths in Galactic Star-forming Regions via the Zeeman Effect with the SKA","ref_index":76,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C","json":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C.json","graph_json":"https://pith.science/api/pith-number/RJPOXJD6AKIGBVKAMO4J5SWH7C/graph.json","events_json":"https://pith.science/api/pith-number/RJPOXJD6AKIGBVKAMO4J5SWH7C/events.json","paper":"https://pith.science/paper/RJPOXJD6"},"agent_actions":{"view_html":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C","download_json":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C.json","view_paper":"https://pith.science/paper/RJPOXJD6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1105.0081&json=true","fetch_graph":"https://pith.science/api/pith-number/RJPOXJD6AKIGBVKAMO4J5SWH7C/graph.json","fetch_events":"https://pith.science/api/pith-number/RJPOXJD6AKIGBVKAMO4J5SWH7C/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C/action/storage_attestation","attest_author":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C/action/author_attestation","sign_citation":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C/action/citation_signature","submit_replication":"https://pith.science/pith/RJPOXJD6AKIGBVKAMO4J5SWH7C/action/replication_record"}},"created_at":"2026-05-18T02:02:10.752233+00:00","updated_at":"2026-05-18T02:02:10.752233+00:00"}