{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:ZQD4MZG22THMTHRY3JK65QGPKM","short_pith_number":"pith:ZQD4MZG2","schema_version":"1.0","canonical_sha256":"cc07c664dad4cec99e38da55eec0cf5304abf2b128cfb1b599d30b63bb1cad89","source":{"kind":"arxiv","id":"2203.12586","version":2},"attestation_state":"computed","paper":{"title":"Detectability and parameter estimation of stellar origin black hole binaries with next generation gravitational wave detectors","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Angelo Ricciardone, Enrico Barausse, Mauro Pieroni","submitted_at":"2022-03-23T17:52:11Z","abstract_excerpt":"We consider stellar-origin black hole binaries, which are among the main astrophysical sources for next generation gravitational wave (GW) detectors such as the Einstein Telescope (ET) and Cosmic Explorer (CE). Using population models calibrated with the most recent LIGO/Virgo results from O3b run, we show that ET and CE will be capable of detecting tens of thousands of such sources (and virtually all of those present in our past light cone up to $z\\lesssim 0.7$ for ET and $z\\lesssim 1$ for CE) with a signal-to-noise ratio up to several hundreds, irrespective of the detector design. When it co"},"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":"2203.12586","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2022-03-23T17:52:11Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"94baf0d7e10b99a6f19290869a51db66a92c92c2894fcac0a201ac471479ca5d","abstract_canon_sha256":"8164a9fea57692fb8d76704619f5662dba87131ca10475ce7f0026b6821953d4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:18:02.342532Z","signature_b64":"AEFHeBLC2znXWoL0Stf7Ps4G65EVwuHIkak6X9XprEbmw175mXmZ0EXV0zk+NyrYnCY9uRrifztyK85IJd9QDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cc07c664dad4cec99e38da55eec0cf5304abf2b128cfb1b599d30b63bb1cad89","last_reissued_at":"2026-07-05T05:18:02.342080Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:18:02.342080Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Detectability and parameter estimation of stellar origin black hole binaries with next generation gravitational wave detectors","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Angelo Ricciardone, Enrico Barausse, Mauro Pieroni","submitted_at":"2022-03-23T17:52:11Z","abstract_excerpt":"We consider stellar-origin black hole binaries, which are among the main astrophysical sources for next generation gravitational wave (GW) detectors such as the Einstein Telescope (ET) and Cosmic Explorer (CE). Using population models calibrated with the most recent LIGO/Virgo results from O3b run, we show that ET and CE will be capable of detecting tens of thousands of such sources (and virtually all of those present in our past light cone up to $z\\lesssim 0.7$ for ET and $z\\lesssim 1$ for CE) with a signal-to-noise ratio up to several hundreds, irrespective of the detector design. When it co"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2203.12586","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/2203.12586/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":"2203.12586","created_at":"2026-07-05T05:18:02.342140+00:00"},{"alias_kind":"arxiv_version","alias_value":"2203.12586v2","created_at":"2026-07-05T05:18:02.342140+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2203.12586","created_at":"2026-07-05T05:18:02.342140+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZQD4MZG22THM","created_at":"2026-07-05T05:18:02.342140+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZQD4MZG22THMTHRY","created_at":"2026-07-05T05:18:02.342140+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZQD4MZG2","created_at":"2026-07-05T05:18:02.342140+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07120","citing_title":"Prospect for Detection of Strongly Lensed Multi-messenger Signals of Binary Neutron Star Mergers","ref_index":262,"is_internal_anchor":true},{"citing_arxiv_id":"2509.04028","citing_title":"Primordial black holes versus their impersonators at gravitational wave observatories","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2303.15923","citing_title":"Science with the Einstein Telescope: a comparison of different designs","ref_index":35,"is_internal_anchor":false},{"citing_arxiv_id":"2604.11871","citing_title":"Not too close! Evaluating the impact of the baseline on the localization of binary black holes by next-generation gravitational-wave detectors","ref_index":21,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM","json":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM.json","graph_json":"https://pith.science/api/pith-number/ZQD4MZG22THMTHRY3JK65QGPKM/graph.json","events_json":"https://pith.science/api/pith-number/ZQD4MZG22THMTHRY3JK65QGPKM/events.json","paper":"https://pith.science/paper/ZQD4MZG2"},"agent_actions":{"view_html":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM","download_json":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM.json","view_paper":"https://pith.science/paper/ZQD4MZG2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2203.12586&json=true","fetch_graph":"https://pith.science/api/pith-number/ZQD4MZG22THMTHRY3JK65QGPKM/graph.json","fetch_events":"https://pith.science/api/pith-number/ZQD4MZG22THMTHRY3JK65QGPKM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM/action/storage_attestation","attest_author":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM/action/author_attestation","sign_citation":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM/action/citation_signature","submit_replication":"https://pith.science/pith/ZQD4MZG22THMTHRY3JK65QGPKM/action/replication_record"}},"created_at":"2026-07-05T05:18:02.342140+00:00","updated_at":"2026-07-05T05:18:02.342140+00:00"}