{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:PFHXE2ZYFPJ7M5FGAZJEWRASXC","short_pith_number":"pith:PFHXE2ZY","schema_version":"1.0","canonical_sha256":"794f726b382bd3f674a606524b4412b8b6bbb835a60ea323676aff266b78ef38","source":{"kind":"arxiv","id":"2007.04313","version":1},"attestation_state":"computed","paper":{"title":"Measuring gravitational-wave higher-order modes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Cameron Mills, Stephen Fairhurst","submitted_at":"2020-07-08T17:58:56Z","abstract_excerpt":"We investigate the observability of higher harmonics in gravitational wave signals emitted during the coalescence of binary black holes. We decompose each mode into an overall amplitude, dependent upon the masses and spins of the system, and an orientation-dependent term, dependent upon the inclination and polarization of the source. Using this decomposition, we investigate the significance of higher modes over the parameter space and show that the $\\ell = 3$, $m = 3$ mode is most significant across much of the sensitive band of ground-based interferometric detectors, with the $\\ell = 4$, $m ="},"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":"2007.04313","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2020-07-08T17:58:56Z","cross_cats_sorted":[],"title_canon_sha256":"c6623c04c4275316eea55488b4348e5347016501e04966f2fb9c955ffab951d7","abstract_canon_sha256":"31b6dd3b4dcb5e12aa01840bc44a0788af95770f1180cc1f2e7906dc2d4b6ecc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:09:42.036892Z","signature_b64":"9oSPHuyCsR57EEfl75y+zrmp1rfI4R4iAMAAtn/4XQe3wJK4jU9dm18uTimb/XnUIdxDLmofsFktE9BpqtC+Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"794f726b382bd3f674a606524b4412b8b6bbb835a60ea323676aff266b78ef38","last_reissued_at":"2026-07-05T02:09:42.036447Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:09:42.036447Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Measuring gravitational-wave higher-order modes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Cameron Mills, Stephen Fairhurst","submitted_at":"2020-07-08T17:58:56Z","abstract_excerpt":"We investigate the observability of higher harmonics in gravitational wave signals emitted during the coalescence of binary black holes. We decompose each mode into an overall amplitude, dependent upon the masses and spins of the system, and an orientation-dependent term, dependent upon the inclination and polarization of the source. Using this decomposition, we investigate the significance of higher modes over the parameter space and show that the $\\ell = 3$, $m = 3$ mode is most significant across much of the sensitive band of ground-based interferometric detectors, with the $\\ell = 4$, $m ="},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2007.04313","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/2007.04313/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":"2007.04313","created_at":"2026-07-05T02:09:42.036511+00:00"},{"alias_kind":"arxiv_version","alias_value":"2007.04313v1","created_at":"2026-07-05T02:09:42.036511+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2007.04313","created_at":"2026-07-05T02:09:42.036511+00:00"},{"alias_kind":"pith_short_12","alias_value":"PFHXE2ZYFPJ7","created_at":"2026-07-05T02:09:42.036511+00:00"},{"alias_kind":"pith_short_16","alias_value":"PFHXE2ZYFPJ7M5FG","created_at":"2026-07-05T02:09:42.036511+00:00"},{"alias_kind":"pith_short_8","alias_value":"PFHXE2ZY","created_at":"2026-07-05T02:09:42.036511+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":9,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.17137","citing_title":"Improving low-latency multi-messenger follow-up of neutron star-black hole mergers with mode-by-mode filtering","ref_index":42,"is_internal_anchor":false},{"citing_arxiv_id":"2508.21216","citing_title":"Persistence of post-Newtonian amplitude structure in binary black hole mergers","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2511.16879","citing_title":"Accelerating parameter estimation for parameterized tests of general relativity with gravitational-wave observations","ref_index":63,"is_internal_anchor":false},{"citing_arxiv_id":"2509.08099","citing_title":"Black Hole Spectroscopy and Tests of General Relativity with GW250114","ref_index":134,"is_internal_anchor":false},{"citing_arxiv_id":"2605.11703","citing_title":"GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors","ref_index":99,"is_internal_anchor":false},{"citing_arxiv_id":"2112.06861","citing_title":"Tests of General Relativity with GWTC-3","ref_index":138,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25582","citing_title":"Lessons from binary dynamics of inspiralling equal-mass boson-star mergers","ref_index":87,"is_internal_anchor":false},{"citing_arxiv_id":"2111.03606","citing_title":"GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run","ref_index":106,"is_internal_anchor":false},{"citing_arxiv_id":"2604.11903","citing_title":"Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and matter effects","ref_index":150,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC","json":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC.json","graph_json":"https://pith.science/api/pith-number/PFHXE2ZYFPJ7M5FGAZJEWRASXC/graph.json","events_json":"https://pith.science/api/pith-number/PFHXE2ZYFPJ7M5FGAZJEWRASXC/events.json","paper":"https://pith.science/paper/PFHXE2ZY"},"agent_actions":{"view_html":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC","download_json":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC.json","view_paper":"https://pith.science/paper/PFHXE2ZY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2007.04313&json=true","fetch_graph":"https://pith.science/api/pith-number/PFHXE2ZYFPJ7M5FGAZJEWRASXC/graph.json","fetch_events":"https://pith.science/api/pith-number/PFHXE2ZYFPJ7M5FGAZJEWRASXC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC/action/storage_attestation","attest_author":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC/action/author_attestation","sign_citation":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC/action/citation_signature","submit_replication":"https://pith.science/pith/PFHXE2ZYFPJ7M5FGAZJEWRASXC/action/replication_record"}},"created_at":"2026-07-05T02:09:42.036511+00:00","updated_at":"2026-07-05T02:09:42.036511+00:00"}