{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:2AJ72UQ3KWSUZNF2VWVS4TFZWF","short_pith_number":"pith:2AJ72UQ3","schema_version":"1.0","canonical_sha256":"d013fd521b55a54cb4baadab2e4cb9b1791ceae34e550ce67df95f17d477cc2b","source":{"kind":"arxiv","id":"2001.11412","version":1},"attestation_state":"computed","paper":{"title":"Setting the cornerstone for the IMRPhenomX family of models for gravitational waves from compact binaries: The dominant harmonic for non-precessing quasi-circular black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"gr-qc","authors_text":"Antoni Ramos-Buades, Cecilio Garcia-Quiros, Geraint Pratten, Hector Estelles, Marta Colleoni, Rafel Jaume, Sascha Husa","submitted_at":"2020-01-30T15:46:20Z","abstract_excerpt":"In this paper we present IMRPhenomXAS, a thorough overhaul of the IMRPhenomD [1,2] waveform model, which describes the dominant $l=2, \\:| m | = 2$ spherical harmonic mode of non-precessing coalescing black holes in terms of piecewise closed form expressions in the frequency domain. Improvements include in particular the accurate treatment of unequal spin effects, and the inclusion of extreme mass ratio waveforms. IMRPhenomD has previously been extended to approximately include spin precession [3] and subdominant spherical harmonics [4], and with its extensions it has become a standard tool in "},"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":"2001.11412","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2020-01-30T15:46:20Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"a45a89b03b0e0bcd19ab048c551fea9f0f6fbd295d7eaad6cbbf828f49850293","abstract_canon_sha256":"6e41254acd49d6d0d77e3b13c4c1d0fa562e4c17f0ba4ccd52cd822fdad9c54d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:33:58.417530Z","signature_b64":"Pw/ajoNcyUO04J0EypGU+r7rWb3GTBNDt9CbVK7Mcp7M1Ke292MR/fKDdej8izf3RqajTSVxCqv9c4fReHGjCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d013fd521b55a54cb4baadab2e4cb9b1791ceae34e550ce67df95f17d477cc2b","last_reissued_at":"2026-07-05T01:33:58.417096Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:33:58.417096Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Setting the cornerstone for the IMRPhenomX family of models for gravitational waves from compact binaries: The dominant harmonic for non-precessing quasi-circular black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"gr-qc","authors_text":"Antoni Ramos-Buades, Cecilio Garcia-Quiros, Geraint Pratten, Hector Estelles, Marta Colleoni, Rafel Jaume, Sascha Husa","submitted_at":"2020-01-30T15:46:20Z","abstract_excerpt":"In this paper we present IMRPhenomXAS, a thorough overhaul of the IMRPhenomD [1,2] waveform model, which describes the dominant $l=2, \\:| m | = 2$ spherical harmonic mode of non-precessing coalescing black holes in terms of piecewise closed form expressions in the frequency domain. Improvements include in particular the accurate treatment of unequal spin effects, and the inclusion of extreme mass ratio waveforms. IMRPhenomD has previously been extended to approximately include spin precession [3] and subdominant spherical harmonics [4], and with its extensions it has become a standard tool in "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2001.11412","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/2001.11412/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":"2001.11412","created_at":"2026-07-05T01:33:58.417152+00:00"},{"alias_kind":"arxiv_version","alias_value":"2001.11412v1","created_at":"2026-07-05T01:33:58.417152+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2001.11412","created_at":"2026-07-05T01:33:58.417152+00:00"},{"alias_kind":"pith_short_12","alias_value":"2AJ72UQ3KWSU","created_at":"2026-07-05T01:33:58.417152+00:00"},{"alias_kind":"pith_short_16","alias_value":"2AJ72UQ3KWSUZNF2","created_at":"2026-07-05T01:33:58.417152+00:00"},{"alias_kind":"pith_short_8","alias_value":"2AJ72UQ3","created_at":"2026-07-05T01:33:58.417152+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":18,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.11705","citing_title":"Horizon absorption in eccentric precessing binary black hole inspirals and its importance for gravitational wave data analysis","ref_index":145,"is_internal_anchor":false},{"citing_arxiv_id":"2606.04810","citing_title":"Fast gravitational waveform models for quasi-circular coalescences of neutron star--black hole binaries","ref_index":64,"is_internal_anchor":false},{"citing_arxiv_id":"2606.28156","citing_title":"Joint inference of line-of-sight acceleration and orbital eccentricity in neutron-star--black-hole binaries","ref_index":117,"is_internal_anchor":false},{"citing_arxiv_id":"2509.04028","citing_title":"Primordial black holes versus their impersonators at gravitational wave observatories","ref_index":92,"is_internal_anchor":false},{"citing_arxiv_id":"2510.02515","citing_title":"Neural Post-Einsteinian Test of General Relativity with the Third Gravitational-Wave Transient Catalog","ref_index":75,"is_internal_anchor":false},{"citing_arxiv_id":"2510.16113","citing_title":"Post-adiabatic self-force waveforms: slowly spinning primary and precessing secondary","ref_index":164,"is_internal_anchor":false},{"citing_arxiv_id":"2511.10522","citing_title":"Learning Post-Newtonian Corrections from Numerical Relativity","ref_index":32,"is_internal_anchor":false},{"citing_arxiv_id":"2512.10344","citing_title":"Improved Identification of Strongly Lensed Gravitational Waves with Host Galaxy Locations","ref_index":49,"is_internal_anchor":false},{"citing_arxiv_id":"2512.09978","citing_title":"Gravitational-wave parameter estimation to the Moon and back: massive binaries and the case of GW231123","ref_index":63,"is_internal_anchor":false},{"citing_arxiv_id":"2601.04276","citing_title":"Search for Precessing Binary Black Holes in Advanced LIGO's Third Observing Run using Harmonic Decomposition","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2108.01045","citing_title":"GWTC-2.1: Deep Extended Catalog of Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2010.14529","citing_title":"Tests of General Relativity with Binary Black Holes from the second LIGO-Virgo Gravitational-Wave Transient Catalog","ref_index":113,"is_internal_anchor":false},{"citing_arxiv_id":"2004.06503","citing_title":"Computationally efficient models for the dominant and sub-dominant harmonic modes of precessing binary black holes","ref_index":16,"is_internal_anchor":false},{"citing_arxiv_id":"2605.11703","citing_title":"GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors","ref_index":211,"is_internal_anchor":false},{"citing_arxiv_id":"2112.06861","citing_title":"Tests of General Relativity with GWTC-3","ref_index":111,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25582","citing_title":"Lessons from binary dynamics of inspiralling equal-mass boson-star mergers","ref_index":83,"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":98,"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":124,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF","json":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF.json","graph_json":"https://pith.science/api/pith-number/2AJ72UQ3KWSUZNF2VWVS4TFZWF/graph.json","events_json":"https://pith.science/api/pith-number/2AJ72UQ3KWSUZNF2VWVS4TFZWF/events.json","paper":"https://pith.science/paper/2AJ72UQ3"},"agent_actions":{"view_html":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF","download_json":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF.json","view_paper":"https://pith.science/paper/2AJ72UQ3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2001.11412&json=true","fetch_graph":"https://pith.science/api/pith-number/2AJ72UQ3KWSUZNF2VWVS4TFZWF/graph.json","fetch_events":"https://pith.science/api/pith-number/2AJ72UQ3KWSUZNF2VWVS4TFZWF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF/action/storage_attestation","attest_author":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF/action/author_attestation","sign_citation":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF/action/citation_signature","submit_replication":"https://pith.science/pith/2AJ72UQ3KWSUZNF2VWVS4TFZWF/action/replication_record"}},"created_at":"2026-07-05T01:33:58.417152+00:00","updated_at":"2026-07-05T01:33:58.417152+00:00"}