{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:57RBB6KKK2G5NXII2IYRVBCEJ6","short_pith_number":"pith:57RBB6KK","schema_version":"1.0","canonical_sha256":"efe210f94a568dd6dd08d2311a84444fa584aca17cb2dfb68118f05776b1d3db","source":{"kind":"arxiv","id":"1910.12874","version":1},"attestation_state":"computed","paper":{"title":"Mind the gap: The location of the lower edge of the pair instability supernovae black hole mass gap","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"M. Renzo, P. Marchant, R. Farmer, S. E de Mink, S. Justham","submitted_at":"2019-10-28T18:00:01Z","abstract_excerpt":"Gravitational-wave detections are now starting to probe the mass distribution of stellar-mass black holes (BHs). Robust predictions from stellar models are needed to interpret these. Theory predicts the existence of a gap in the BH mass distribution because of pair-instability supernova. The maximum BH mass below the gap is the result of pulsational mass loss. We evolve massive helium stars through their late hydrodynamical phases of evolution using the open-source MESA stellar evolution code. We find that the location of the lower edge of the mass gap at 45$M_\\odot$ is remarkably robust again"},"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":"1910.12874","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2019-10-28T18:00:01Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"68cbb6fe0e20d4834be1c7a540ce1dbb249dea87706e7d300be7b76762c13617","abstract_canon_sha256":"1b68cab21527308b9fb26e4b7ed6fb48b6e628c152fd50baf08152d393a362e3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:31:27.488330Z","signature_b64":"d/w9ubmSsQV27bK+sjbEToIbkqw6MHgNKr/GUlCPYP5te/LATjn7x+AtCI5nyW5R8JfWeytGe+4oL/ewU78LBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"efe210f94a568dd6dd08d2311a84444fa584aca17cb2dfb68118f05776b1d3db","last_reissued_at":"2026-07-05T00:31:27.487898Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:31:27.487898Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Mind the gap: The location of the lower edge of the pair instability supernovae black hole mass gap","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"M. Renzo, P. Marchant, R. Farmer, S. E de Mink, S. Justham","submitted_at":"2019-10-28T18:00:01Z","abstract_excerpt":"Gravitational-wave detections are now starting to probe the mass distribution of stellar-mass black holes (BHs). Robust predictions from stellar models are needed to interpret these. Theory predicts the existence of a gap in the BH mass distribution because of pair-instability supernova. The maximum BH mass below the gap is the result of pulsational mass loss. We evolve massive helium stars through their late hydrodynamical phases of evolution using the open-source MESA stellar evolution code. We find that the location of the lower edge of the mass gap at 45$M_\\odot$ is remarkably robust again"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1910.12874","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/1910.12874/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":"1910.12874","created_at":"2026-07-05T00:31:27.487959+00:00"},{"alias_kind":"arxiv_version","alias_value":"1910.12874v1","created_at":"2026-07-05T00:31:27.487959+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1910.12874","created_at":"2026-07-05T00:31:27.487959+00:00"},{"alias_kind":"pith_short_12","alias_value":"57RBB6KKK2G5","created_at":"2026-07-05T00:31:27.487959+00:00"},{"alias_kind":"pith_short_16","alias_value":"57RBB6KKK2G5NXII","created_at":"2026-07-05T00:31:27.487959+00:00"},{"alias_kind":"pith_short_8","alias_value":"57RBB6KK","created_at":"2026-07-05T00:31:27.487959+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":9,"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":2,"is_internal_anchor":true},{"citing_arxiv_id":"2311.01300","citing_title":"Waveform Modelling for the Laser Interferometer Space Antenna","ref_index":189,"is_internal_anchor":false},{"citing_arxiv_id":"2512.09978","citing_title":"Gravitational-wave parameter estimation to the Moon and back: massive binaries and the case of GW231123","ref_index":11,"is_internal_anchor":false},{"citing_arxiv_id":"2601.09678","citing_title":"The impact of waveform systematics and Gaussian noise on the interpretation of GW231123","ref_index":6,"is_internal_anchor":false},{"citing_arxiv_id":"2108.01045","citing_title":"GWTC-2.1: Deep Extended Catalog of Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","ref_index":35,"is_internal_anchor":false},{"citing_arxiv_id":"2602.11282","citing_title":"Measurement prospects for the pair-instability mass cutoff with gravitational waves","ref_index":33,"is_internal_anchor":false},{"citing_arxiv_id":"2604.02413","citing_title":"The Black Hole Mass Gap as a New Probe of Millicharged Particles","ref_index":32,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22634","citing_title":"Constraints on the Primordial Black Hole Abundance using Pulsar Parameter Drifts","ref_index":10,"is_internal_anchor":false},{"citing_arxiv_id":"2604.07456","citing_title":"Second-Generation Mass Peak in the Gravitational-Wave Population as a Probe of Globular Clusters","ref_index":47,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6","json":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6.json","graph_json":"https://pith.science/api/pith-number/57RBB6KKK2G5NXII2IYRVBCEJ6/graph.json","events_json":"https://pith.science/api/pith-number/57RBB6KKK2G5NXII2IYRVBCEJ6/events.json","paper":"https://pith.science/paper/57RBB6KK"},"agent_actions":{"view_html":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6","download_json":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6.json","view_paper":"https://pith.science/paper/57RBB6KK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1910.12874&json=true","fetch_graph":"https://pith.science/api/pith-number/57RBB6KKK2G5NXII2IYRVBCEJ6/graph.json","fetch_events":"https://pith.science/api/pith-number/57RBB6KKK2G5NXII2IYRVBCEJ6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6/action/storage_attestation","attest_author":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6/action/author_attestation","sign_citation":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6/action/citation_signature","submit_replication":"https://pith.science/pith/57RBB6KKK2G5NXII2IYRVBCEJ6/action/replication_record"}},"created_at":"2026-07-05T00:31:27.487959+00:00","updated_at":"2026-07-05T00:31:27.487959+00:00"}