{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:PYDFUCUO53ZMN7SXQSQD5CBIC3","short_pith_number":"pith:PYDFUCUO","schema_version":"1.0","canonical_sha256":"7e065a0a8eeef2c6fe5784a03e882816cc0393819818f2efd316edfa6a96800a","source":{"kind":"arxiv","id":"1506.06354","version":1},"attestation_state":"computed","paper":{"title":"Observational Properties of Type Ib/c Supernova Progenitors in Binary Systems","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Bon-Chul Koo, Hyun-Jeong Kim, Sung-Chul Yoon","submitted_at":"2015-06-21T11:55:17Z","abstract_excerpt":"In several recent observational studies on Type Ib/c supernovae (SNe Ib/c), the inferred ejecta masses have a peak value of 2.0 -- 4.0 $M_\\odot$, in favor of the binary scenario for their progenitors rather than the Wolf-Rayet star scenario. To investigate the observational properties of relatively low-mass helium stars in binary systems as SN Ib/c progenitors, we constructed atmospheric models with the non-LTE radiative transfer code CMFGEN, using binary star evolution models. We find that these helium stars can be characterized by relatively narrow helium emission lines if the mass-loss rate"},"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":"1506.06354","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2015-06-21T11:55:17Z","cross_cats_sorted":[],"title_canon_sha256":"f44c445466716d7a1c410e308c4bed804c4e7341f8a6613aea3bf659b7d61d6a","abstract_canon_sha256":"080a43429ed06992c019b5230da0d7d37ecec5eff19625fba51c61174962502e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:34:47.947676Z","signature_b64":"80ged2eRyqPDC0dMmAyl24Z5FnjRh1CtBS+BYdBNRWoGhxbTXkRGWNRSgzpikpczbECbKXuP4U3FSEiUQOCPCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7e065a0a8eeef2c6fe5784a03e882816cc0393819818f2efd316edfa6a96800a","last_reissued_at":"2026-05-18T01:34:47.947130Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:34:47.947130Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Observational Properties of Type Ib/c Supernova Progenitors in Binary Systems","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Bon-Chul Koo, Hyun-Jeong Kim, Sung-Chul Yoon","submitted_at":"2015-06-21T11:55:17Z","abstract_excerpt":"In several recent observational studies on Type Ib/c supernovae (SNe Ib/c), the inferred ejecta masses have a peak value of 2.0 -- 4.0 $M_\\odot$, in favor of the binary scenario for their progenitors rather than the Wolf-Rayet star scenario. To investigate the observational properties of relatively low-mass helium stars in binary systems as SN Ib/c progenitors, we constructed atmospheric models with the non-LTE radiative transfer code CMFGEN, using binary star evolution models. We find that these helium stars can be characterized by relatively narrow helium emission lines if the mass-loss rate"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1506.06354","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"},"aliases":[{"alias_kind":"arxiv","alias_value":"1506.06354","created_at":"2026-05-18T01:34:47.947220+00:00"},{"alias_kind":"arxiv_version","alias_value":"1506.06354v1","created_at":"2026-05-18T01:34:47.947220+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1506.06354","created_at":"2026-05-18T01:34:47.947220+00:00"},{"alias_kind":"pith_short_12","alias_value":"PYDFUCUO53ZM","created_at":"2026-05-18T12:29:37.295048+00:00"},{"alias_kind":"pith_short_16","alias_value":"PYDFUCUO53ZMN7SX","created_at":"2026-05-18T12:29:37.295048+00:00"},{"alias_kind":"pith_short_8","alias_value":"PYDFUCUO","created_at":"2026-05-18T12:29:37.295048+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.12764","citing_title":"The long-short GRB connection","ref_index":30,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3","json":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3.json","graph_json":"https://pith.science/api/pith-number/PYDFUCUO53ZMN7SXQSQD5CBIC3/graph.json","events_json":"https://pith.science/api/pith-number/PYDFUCUO53ZMN7SXQSQD5CBIC3/events.json","paper":"https://pith.science/paper/PYDFUCUO"},"agent_actions":{"view_html":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3","download_json":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3.json","view_paper":"https://pith.science/paper/PYDFUCUO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1506.06354&json=true","fetch_graph":"https://pith.science/api/pith-number/PYDFUCUO53ZMN7SXQSQD5CBIC3/graph.json","fetch_events":"https://pith.science/api/pith-number/PYDFUCUO53ZMN7SXQSQD5CBIC3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3/action/storage_attestation","attest_author":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3/action/author_attestation","sign_citation":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3/action/citation_signature","submit_replication":"https://pith.science/pith/PYDFUCUO53ZMN7SXQSQD5CBIC3/action/replication_record"}},"created_at":"2026-05-18T01:34:47.947220+00:00","updated_at":"2026-05-18T01:34:47.947220+00:00"}