{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:TOEKBKNHGOUSLEKQPPL7I6DYN4","short_pith_number":"pith:TOEKBKNH","schema_version":"1.0","canonical_sha256":"9b88a0a9a733a92591507bd7f478786f1025c3cc3144be8f0e6f244b8fcd16b7","source":{"kind":"arxiv","id":"2104.13384","version":2},"attestation_state":"computed","paper":{"title":"On the population III binary black hole mergers beyond the pair-instability mass gap","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Ataru Tanikawa, Hideyuki Umeda, Kotaro Hijikawa, Takashi Yoshida, Tomoya Kinugawa","submitted_at":"2021-04-27T18:00:01Z","abstract_excerpt":"We perform a binary population synthesis calculation incorporating very massive population (Pop.) III stars up to 1500 $M_\\odot$, and investigate the nature of binary black hole (BBH) mergers. Above the pair-instability mass gap, we find that the typical primary black hole (BH) mass is 135-340 $M_\\odot$. The maximum primary BH mass is as massive as 686 $M_\\odot$. The BBHs with both of their components above the mass gap have low effective inspiral spin $\\sim$ 0. So far, no conclusive BBH merger beyond the mass gap has been detected, and the upper limit on the merger rate density is obtained. I"},"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":"2104.13384","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-04-27T18:00:01Z","cross_cats_sorted":["astro-ph.GA","astro-ph.SR"],"title_canon_sha256":"037781b3384e52eb310110c5906de562be5f29290585c5d4b0fdb38052ea5d43","abstract_canon_sha256":"e83d6b7043943209180b092970113f66f6857983c8c4fd89753bb4bf6a985343"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:43:22.386996Z","signature_b64":"HGzB59X5E8qQs4KJI0mQE7oDnh6lbYmHRjUEw6d8hSwKjrWnYTC9ug6zmQrplThjvoN5Fwg/4ZQ9TiEbxZKbCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9b88a0a9a733a92591507bd7f478786f1025c3cc3144be8f0e6f244b8fcd16b7","last_reissued_at":"2026-07-05T02:43:22.386475Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:43:22.386475Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the population III binary black hole mergers beyond the pair-instability mass gap","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Ataru Tanikawa, Hideyuki Umeda, Kotaro Hijikawa, Takashi Yoshida, Tomoya Kinugawa","submitted_at":"2021-04-27T18:00:01Z","abstract_excerpt":"We perform a binary population synthesis calculation incorporating very massive population (Pop.) III stars up to 1500 $M_\\odot$, and investigate the nature of binary black hole (BBH) mergers. Above the pair-instability mass gap, we find that the typical primary black hole (BH) mass is 135-340 $M_\\odot$. The maximum primary BH mass is as massive as 686 $M_\\odot$. The BBHs with both of their components above the mass gap have low effective inspiral spin $\\sim$ 0. So far, no conclusive BBH merger beyond the mass gap has been detected, and the upper limit on the merger rate density is obtained. I"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2104.13384","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2104.13384/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":"2104.13384","created_at":"2026-07-05T02:43:22.386550+00:00"},{"alias_kind":"arxiv_version","alias_value":"2104.13384v2","created_at":"2026-07-05T02:43:22.386550+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2104.13384","created_at":"2026-07-05T02:43:22.386550+00:00"},{"alias_kind":"pith_short_12","alias_value":"TOEKBKNHGOUS","created_at":"2026-07-05T02:43:22.386550+00:00"},{"alias_kind":"pith_short_16","alias_value":"TOEKBKNHGOUSLEKQ","created_at":"2026-07-05T02:43:22.386550+00:00"},{"alias_kind":"pith_short_8","alias_value":"TOEKBKNH","created_at":"2026-07-05T02:43:22.386550+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2508.09965","citing_title":"GW231123: A Possible Primordial Black Hole Origin","ref_index":127,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4","json":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4.json","graph_json":"https://pith.science/api/pith-number/TOEKBKNHGOUSLEKQPPL7I6DYN4/graph.json","events_json":"https://pith.science/api/pith-number/TOEKBKNHGOUSLEKQPPL7I6DYN4/events.json","paper":"https://pith.science/paper/TOEKBKNH"},"agent_actions":{"view_html":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4","download_json":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4.json","view_paper":"https://pith.science/paper/TOEKBKNH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2104.13384&json=true","fetch_graph":"https://pith.science/api/pith-number/TOEKBKNHGOUSLEKQPPL7I6DYN4/graph.json","fetch_events":"https://pith.science/api/pith-number/TOEKBKNHGOUSLEKQPPL7I6DYN4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4/action/storage_attestation","attest_author":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4/action/author_attestation","sign_citation":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4/action/citation_signature","submit_replication":"https://pith.science/pith/TOEKBKNHGOUSLEKQPPL7I6DYN4/action/replication_record"}},"created_at":"2026-07-05T02:43:22.386550+00:00","updated_at":"2026-07-05T02:43:22.386550+00:00"}