{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:ISSY3KUPO32V6OBLE25QZ4USXM","short_pith_number":"pith:ISSY3KUP","schema_version":"1.0","canonical_sha256":"44a58daa8f76f55f382b26bb0cf292bb29d4f792cbf12e8be73417164e167859","source":{"kind":"arxiv","id":"2504.17903","version":1},"attestation_state":"computed","paper":{"title":"Delayed and Displaced: The Impact of Binary Interactions on Core-collapse SN Feedback","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Adrian M. Price-Whelan, Akaxia Cruz, Alyson Brooks, Eric C. Bellm, Julianne J. Dalcanton, Katelyn Breivik, Mathieu Renzo, Matthew E. Orr, Tom Wagg, Ulrich P. Steinwandel","submitted_at":"2025-04-24T19:31:10Z","abstract_excerpt":"Core-collapse supernova feedback models in hydrodynamical simulations typically assume that all stars evolve as single stars. However, the majority of massive stars are formed in binaries and multiple systems, where interactions with a companion can affect stars' subsequent evolution and kinematics. We assess the impact of binary interactions on the timing and spatial distribution of core-collapse supernovae, using `cogsworth` simulations to evolve binary star populations, and their subsequent galactic orbits, within state-of-the-art hydrodynamical zoom-in galaxy simulations. We show that bina"},"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":"2504.17903","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2025-04-24T19:31:10Z","cross_cats_sorted":[],"title_canon_sha256":"219cb24c26170440c882aa55bde02330d138779ef98f1e2533308fda9bb562dc","abstract_canon_sha256":"548133662835733176a1d68408c647caea01ed0cc9efc07e88e94661bfe6abd1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:53:58.463045Z","signature_b64":"ukvk2g6RLaYO/9NB9K1az1dXP0zK/wzHcbKF5CAszob/fO7+KaNr05J+luztL7Qz3KC9EXsHkUQub9Knb3OhCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"44a58daa8f76f55f382b26bb0cf292bb29d4f792cbf12e8be73417164e167859","last_reissued_at":"2026-07-05T10:53:58.462541Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:53:58.462541Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Delayed and Displaced: The Impact of Binary Interactions on Core-collapse SN Feedback","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Adrian M. Price-Whelan, Akaxia Cruz, Alyson Brooks, Eric C. Bellm, Julianne J. Dalcanton, Katelyn Breivik, Mathieu Renzo, Matthew E. Orr, Tom Wagg, Ulrich P. Steinwandel","submitted_at":"2025-04-24T19:31:10Z","abstract_excerpt":"Core-collapse supernova feedback models in hydrodynamical simulations typically assume that all stars evolve as single stars. However, the majority of massive stars are formed in binaries and multiple systems, where interactions with a companion can affect stars' subsequent evolution and kinematics. We assess the impact of binary interactions on the timing and spatial distribution of core-collapse supernovae, using `cogsworth` simulations to evolve binary star populations, and their subsequent galactic orbits, within state-of-the-art hydrodynamical zoom-in galaxy simulations. We show that bina"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2504.17903","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2504.17903/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"2504.17903","created_at":"2026-07-05T10:53:58.462599+00:00"},{"alias_kind":"arxiv_version","alias_value":"2504.17903v1","created_at":"2026-07-05T10:53:58.462599+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2504.17903","created_at":"2026-07-05T10:53:58.462599+00:00"},{"alias_kind":"pith_short_12","alias_value":"ISSY3KUPO32V","created_at":"2026-07-05T10:53:58.462599+00:00"},{"alias_kind":"pith_short_16","alias_value":"ISSY3KUPO32V6OBL","created_at":"2026-07-05T10:53:58.462599+00:00"},{"alias_kind":"pith_short_8","alias_value":"ISSY3KUP","created_at":"2026-07-05T10:53:58.462599+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2504.16161","citing_title":"Stellar ejection velocities from the binary supernova scenario: A comparison across population synthesis codes","ref_index":77,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM","json":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM.json","graph_json":"https://pith.science/api/pith-number/ISSY3KUPO32V6OBLE25QZ4USXM/graph.json","events_json":"https://pith.science/api/pith-number/ISSY3KUPO32V6OBLE25QZ4USXM/events.json","paper":"https://pith.science/paper/ISSY3KUP"},"agent_actions":{"view_html":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM","download_json":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM.json","view_paper":"https://pith.science/paper/ISSY3KUP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2504.17903&json=true","fetch_graph":"https://pith.science/api/pith-number/ISSY3KUPO32V6OBLE25QZ4USXM/graph.json","fetch_events":"https://pith.science/api/pith-number/ISSY3KUPO32V6OBLE25QZ4USXM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM/action/storage_attestation","attest_author":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM/action/author_attestation","sign_citation":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM/action/citation_signature","submit_replication":"https://pith.science/pith/ISSY3KUPO32V6OBLE25QZ4USXM/action/replication_record"}},"created_at":"2026-07-05T10:53:58.462599+00:00","updated_at":"2026-07-05T10:53:58.462599+00:00"}