{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:6W2A7GZEGBEXWNB6LCATWQG3V2","short_pith_number":"pith:6W2A7GZE","schema_version":"1.0","canonical_sha256":"f5b40f9b2430497b343e58813b40dbaeb497bb3843160e960f1ee23c53680387","source":{"kind":"arxiv","id":"2204.03493","version":5},"attestation_state":"computed","paper":{"title":"Formation of black holes in the pair-instability mass gap: Hydrodynamical simulations of a head-on massive star collision","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Alessandro Ballone, Guglielmo Costa, Juan Manuel Pacheco-Arias, Michela Mapelli, Morgan MacLeod, Stefano Torniamenti","submitted_at":"2022-04-07T15:07:31Z","abstract_excerpt":"The detection of the binary black hole merger GW190521, with primary black hole mass $85^{+21}_{-14}$ ${\\rm M}_{\\odot}$, proved the existence of black holes in the theoretically predicted pair-instability gap ($\\sim60-120 \\, {\\rm M}_{\\odot}$) of their mass spectrum. Some recent studies suggest that such massive black holes could be produced by the collision of an evolved star with a carbon-oxygen core and a main sequence star. Such a post-coalescence star could end its life avoiding the pair-instability regime and with a direct collapse of its very massive envelope. It is still not clear, howe"},"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":"2204.03493","kind":"arxiv","version":5},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2022-04-07T15:07:31Z","cross_cats_sorted":["astro-ph.GA","astro-ph.HE"],"title_canon_sha256":"9cf5940b973dc0ab096f32c1e2e7fd584b55154f89bd4d8fd755d93f4927c6f1","abstract_canon_sha256":"9bad4d4a92b2ed22b793e2795fa82bd905b27a025f66e63b56bf2fb5648f83c6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:29:52.595795Z","signature_b64":"D7QNJ9lhfXlnz7b9SsrG93guugwajBzm+CG5AS2vl3Cc9UiepIOd5Rfm3Jx8Vq42VPO7B7onRxncz1Xfu3XXAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f5b40f9b2430497b343e58813b40dbaeb497bb3843160e960f1ee23c53680387","last_reissued_at":"2026-07-05T05:29:52.595213Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:29:52.595213Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Formation of black holes in the pair-instability mass gap: Hydrodynamical simulations of a head-on massive star collision","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Alessandro Ballone, Guglielmo Costa, Juan Manuel Pacheco-Arias, Michela Mapelli, Morgan MacLeod, Stefano Torniamenti","submitted_at":"2022-04-07T15:07:31Z","abstract_excerpt":"The detection of the binary black hole merger GW190521, with primary black hole mass $85^{+21}_{-14}$ ${\\rm M}_{\\odot}$, proved the existence of black holes in the theoretically predicted pair-instability gap ($\\sim60-120 \\, {\\rm M}_{\\odot}$) of their mass spectrum. Some recent studies suggest that such massive black holes could be produced by the collision of an evolved star with a carbon-oxygen core and a main sequence star. Such a post-coalescence star could end its life avoiding the pair-instability regime and with a direct collapse of its very massive envelope. It is still not clear, howe"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2204.03493","kind":"arxiv","version":5},"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/2204.03493/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":"2204.03493","created_at":"2026-07-05T05:29:52.595269+00:00"},{"alias_kind":"arxiv_version","alias_value":"2204.03493v5","created_at":"2026-07-05T05:29:52.595269+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2204.03493","created_at":"2026-07-05T05:29:52.595269+00:00"},{"alias_kind":"pith_short_12","alias_value":"6W2A7GZEGBEX","created_at":"2026-07-05T05:29:52.595269+00:00"},{"alias_kind":"pith_short_16","alias_value":"6W2A7GZEGBEXWNB6","created_at":"2026-07-05T05:29:52.595269+00:00"},{"alias_kind":"pith_short_8","alias_value":"6W2A7GZE","created_at":"2026-07-05T05:29:52.595269+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06067","citing_title":"A Possible Triple Formation Scenario of Binary Black Hole Merge With One In Pair-instability Supernova Mass Gap","ref_index":30,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2","json":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2.json","graph_json":"https://pith.science/api/pith-number/6W2A7GZEGBEXWNB6LCATWQG3V2/graph.json","events_json":"https://pith.science/api/pith-number/6W2A7GZEGBEXWNB6LCATWQG3V2/events.json","paper":"https://pith.science/paper/6W2A7GZE"},"agent_actions":{"view_html":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2","download_json":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2.json","view_paper":"https://pith.science/paper/6W2A7GZE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2204.03493&json=true","fetch_graph":"https://pith.science/api/pith-number/6W2A7GZEGBEXWNB6LCATWQG3V2/graph.json","fetch_events":"https://pith.science/api/pith-number/6W2A7GZEGBEXWNB6LCATWQG3V2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2/action/storage_attestation","attest_author":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2/action/author_attestation","sign_citation":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2/action/citation_signature","submit_replication":"https://pith.science/pith/6W2A7GZEGBEXWNB6LCATWQG3V2/action/replication_record"}},"created_at":"2026-07-05T05:29:52.595269+00:00","updated_at":"2026-07-05T05:29:52.595269+00:00"}