{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:QTLBOHKLHPUNSZ5ME73M4T5WBN","short_pith_number":"pith:QTLBOHKL","schema_version":"1.0","canonical_sha256":"84d6171d4b3be8d967ac27f6ce4fb60b40447d8cf7eba7e5586039ac739a47fa","source":{"kind":"arxiv","id":"2312.07376","version":2},"attestation_state":"computed","paper":{"title":"Impact of higher harmonics of gravitational radiation on the population inference of binary black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Aditya Vijaykumar, Mukesh Kumar Singh, Parameswaran Ajith, Shasvath J Kapadia","submitted_at":"2023-12-12T15:44:28Z","abstract_excerpt":"Templates modeling just the dominant mode of gravitational radiation are generally sufficient for the unbiased parameter inference of near-equal-mass compact binary mergers. However, neglecting the subdominant modes can bias the inference if the binary is significantly asymmetric, very massive, or has misaligned spins. In this work, we explore if neglecting these subdominant modes in the parameter estimation of non-spinning binary black hole mergers can bias the inference of their population-level properties such as mass and merger redshift distributions. Assuming the design sensitivity of adv"},"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":"2312.07376","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2023-12-12T15:44:28Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"3ee304f433d49301a7caa2e5998208229cb037b4f2162adac4a3a1c924976bf2","abstract_canon_sha256":"22257cb5410d2e861b1d88dd69365cd60c4fcf6dc306d409158177f11ab7cfec"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:01:27.777249Z","signature_b64":"viyu+kEhLzXuD5mq3hofddvCouAavKnyXLh+HG4lD9RaNNBjRlyH2NdH49pRSsyz5Matn2uHsAhs/Uo/LGthBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"84d6171d4b3be8d967ac27f6ce4fb60b40447d8cf7eba7e5586039ac739a47fa","last_reissued_at":"2026-07-05T09:01:27.776822Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:01:27.776822Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Impact of higher harmonics of gravitational radiation on the population inference of binary black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Aditya Vijaykumar, Mukesh Kumar Singh, Parameswaran Ajith, Shasvath J Kapadia","submitted_at":"2023-12-12T15:44:28Z","abstract_excerpt":"Templates modeling just the dominant mode of gravitational radiation are generally sufficient for the unbiased parameter inference of near-equal-mass compact binary mergers. However, neglecting the subdominant modes can bias the inference if the binary is significantly asymmetric, very massive, or has misaligned spins. In this work, we explore if neglecting these subdominant modes in the parameter estimation of non-spinning binary black hole mergers can bias the inference of their population-level properties such as mass and merger redshift distributions. Assuming the design sensitivity of adv"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2312.07376","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/2312.07376/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":"2312.07376","created_at":"2026-07-05T09:01:27.776882+00:00"},{"alias_kind":"arxiv_version","alias_value":"2312.07376v2","created_at":"2026-07-05T09:01:27.776882+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2312.07376","created_at":"2026-07-05T09:01:27.776882+00:00"},{"alias_kind":"pith_short_12","alias_value":"QTLBOHKLHPUN","created_at":"2026-07-05T09:01:27.776882+00:00"},{"alias_kind":"pith_short_16","alias_value":"QTLBOHKLHPUNSZ5M","created_at":"2026-07-05T09:01:27.776882+00:00"},{"alias_kind":"pith_short_8","alias_value":"QTLBOHKL","created_at":"2026-07-05T09:01:27.776882+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2602.11282","citing_title":"Measurement prospects for the pair-instability mass cutoff with gravitational waves","ref_index":97,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN","json":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN.json","graph_json":"https://pith.science/api/pith-number/QTLBOHKLHPUNSZ5ME73M4T5WBN/graph.json","events_json":"https://pith.science/api/pith-number/QTLBOHKLHPUNSZ5ME73M4T5WBN/events.json","paper":"https://pith.science/paper/QTLBOHKL"},"agent_actions":{"view_html":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN","download_json":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN.json","view_paper":"https://pith.science/paper/QTLBOHKL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2312.07376&json=true","fetch_graph":"https://pith.science/api/pith-number/QTLBOHKLHPUNSZ5ME73M4T5WBN/graph.json","fetch_events":"https://pith.science/api/pith-number/QTLBOHKLHPUNSZ5ME73M4T5WBN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN/action/storage_attestation","attest_author":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN/action/author_attestation","sign_citation":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN/action/citation_signature","submit_replication":"https://pith.science/pith/QTLBOHKLHPUNSZ5ME73M4T5WBN/action/replication_record"}},"created_at":"2026-07-05T09:01:27.776882+00:00","updated_at":"2026-07-05T09:01:27.776882+00:00"}