{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:RMJ6IKEILTNB3IRBMQPRESWM7N","short_pith_number":"pith:RMJ6IKEI","schema_version":"1.0","canonical_sha256":"8b13e428885cda1da221641f124accfb69914faf36dad7241e56d8da521e55d1","source":{"kind":"arxiv","id":"1801.03099","version":3},"attestation_state":"computed","paper":{"title":"Predicting the binary black hole population of the Milky Way with cosmological simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Andrew Wetzel, Astrid Lamberts, Claude-Andr\\'e Faucher-Gigu\\`ere, Dusan Keres, Eliot Quataert, James Bullock, Kaliden Drango, Philip Hopkins, Robyn Sanderson, Shea Garrison-Kimmel","submitted_at":"2018-01-09T19:00:07Z","abstract_excerpt":"Binary black holes are the primary endpoint of massive stellar evolution. Their properties provide a unique opportunity to constrain binary evolution, which is still poorly understood. In this paper, we predict the inventory of binary black holes and their merger products in/around the Milky Way, and detail their main properties. We present the first combination of a high-resolution cosmological simulation of a Milky Way-mass galaxy with a binary population synthesis model. The hydrodynamic simulation, taken from the FIRE project, provides a cosmologically realistic star formation history for "},"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":"1801.03099","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-01-09T19:00:07Z","cross_cats_sorted":[],"title_canon_sha256":"cdb2ab605559063603f0942a04f7fb4af711e381ddac56d5dd1b515f57aa7c88","abstract_canon_sha256":"c5373f55ad4fee14a04459b83be06a48775c3d950d5349f7e71b9c4a5aedcbc1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:08:43.623526Z","signature_b64":"ho3ed+KIRXxnW5Dg1djUd04WNk5el/NejaGcPWiU7CDAJa/+aZyqbgUQqgGy6somcHiVdlEbAGztIzPoVPmDBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8b13e428885cda1da221641f124accfb69914faf36dad7241e56d8da521e55d1","last_reissued_at":"2026-05-18T00:08:43.622865Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:08:43.622865Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Predicting the binary black hole population of the Milky Way with cosmological simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Andrew Wetzel, Astrid Lamberts, Claude-Andr\\'e Faucher-Gigu\\`ere, Dusan Keres, Eliot Quataert, James Bullock, Kaliden Drango, Philip Hopkins, Robyn Sanderson, Shea Garrison-Kimmel","submitted_at":"2018-01-09T19:00:07Z","abstract_excerpt":"Binary black holes are the primary endpoint of massive stellar evolution. Their properties provide a unique opportunity to constrain binary evolution, which is still poorly understood. In this paper, we predict the inventory of binary black holes and their merger products in/around the Milky Way, and detail their main properties. We present the first combination of a high-resolution cosmological simulation of a Milky Way-mass galaxy with a binary population synthesis model. The hydrodynamic simulation, taken from the FIRE project, provides a cosmologically realistic star formation history for "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1801.03099","kind":"arxiv","version":3},"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":"1801.03099","created_at":"2026-05-18T00:08:43.622964+00:00"},{"alias_kind":"arxiv_version","alias_value":"1801.03099v3","created_at":"2026-05-18T00:08:43.622964+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1801.03099","created_at":"2026-05-18T00:08:43.622964+00:00"},{"alias_kind":"pith_short_12","alias_value":"RMJ6IKEILTNB","created_at":"2026-05-18T12:32:50.500415+00:00"},{"alias_kind":"pith_short_16","alias_value":"RMJ6IKEILTNB3IRB","created_at":"2026-05-18T12:32:50.500415+00:00"},{"alias_kind":"pith_short_8","alias_value":"RMJ6IKEI","created_at":"2026-05-18T12:32:50.500415+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.15265","citing_title":"Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO Era","ref_index":99,"is_internal_anchor":true},{"citing_arxiv_id":"2602.18560","citing_title":"Inferring the population properties of galactic binaries from LISA's stochastic foreground","ref_index":37,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N","json":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N.json","graph_json":"https://pith.science/api/pith-number/RMJ6IKEILTNB3IRBMQPRESWM7N/graph.json","events_json":"https://pith.science/api/pith-number/RMJ6IKEILTNB3IRBMQPRESWM7N/events.json","paper":"https://pith.science/paper/RMJ6IKEI"},"agent_actions":{"view_html":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N","download_json":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N.json","view_paper":"https://pith.science/paper/RMJ6IKEI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1801.03099&json=true","fetch_graph":"https://pith.science/api/pith-number/RMJ6IKEILTNB3IRBMQPRESWM7N/graph.json","fetch_events":"https://pith.science/api/pith-number/RMJ6IKEILTNB3IRBMQPRESWM7N/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N/action/storage_attestation","attest_author":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N/action/author_attestation","sign_citation":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N/action/citation_signature","submit_replication":"https://pith.science/pith/RMJ6IKEILTNB3IRBMQPRESWM7N/action/replication_record"}},"created_at":"2026-05-18T00:08:43.622964+00:00","updated_at":"2026-05-18T00:08:43.622964+00:00"}