{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:J7HLBVNTB6YBKDZFVALNMECPGU","short_pith_number":"pith:J7HLBVNT","schema_version":"1.0","canonical_sha256":"4fceb0d5b30fb0150f25a816d6104f3527a06023844735f64a49a1c3e8130e0b","source":{"kind":"arxiv","id":"2404.16599","version":1},"attestation_state":"computed","paper":{"title":"Waveform systematics in gravitational-wave inference of signals from binary neutron star merger models incorporating higher order modes information","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"A. B. Yelikar, A. Z. Jan, J. Lange, R. O' Shaughnessy","submitted_at":"2024-04-25T13:26:17Z","abstract_excerpt":"Accurate information from gravitational wave signals from coalescing binary neutron stars provides essential input to downstream interpretations, including inference of the neutron star population and equation of state. However, even adopting the currently most accurate and physically motivated models available for parameter estimation (PE) of BNSs, these models remain subject to waveform modeling uncertainty: differences between these models may introduce biases in recovered source properties. In this work, we describe injection studies investigating these systematic differences between the t"},"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":"2404.16599","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2024-04-25T13:26:17Z","cross_cats_sorted":[],"title_canon_sha256":"c1dea2de0a89f533c296e20257c831035631f74d940a140ae95ba4f221398625","abstract_canon_sha256":"c53c8b1d8de0c7092ee46963a637bbc4c1ea6a5c9257f42ecdf9ae7f109f11eb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:12:09.702847Z","signature_b64":"hQsT6LnjLPGGFUfrJsIMNMTBkbnx9g1xDMwU4Y/9/hFHkGMLqXj8pkcAC2oIiHnDTE744qRSdkHHszTFv14kCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4fceb0d5b30fb0150f25a816d6104f3527a06023844735f64a49a1c3e8130e0b","last_reissued_at":"2026-07-05T08:12:09.702385Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:12:09.702385Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Waveform systematics in gravitational-wave inference of signals from binary neutron star merger models incorporating higher order modes information","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"A. B. Yelikar, A. Z. Jan, J. Lange, R. O' Shaughnessy","submitted_at":"2024-04-25T13:26:17Z","abstract_excerpt":"Accurate information from gravitational wave signals from coalescing binary neutron stars provides essential input to downstream interpretations, including inference of the neutron star population and equation of state. However, even adopting the currently most accurate and physically motivated models available for parameter estimation (PE) of BNSs, these models remain subject to waveform modeling uncertainty: differences between these models may introduce biases in recovered source properties. In this work, we describe injection studies investigating these systematic differences between the t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2404.16599","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/2404.16599/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":"2404.16599","created_at":"2026-07-05T08:12:09.702448+00:00"},{"alias_kind":"arxiv_version","alias_value":"2404.16599v1","created_at":"2026-07-05T08:12:09.702448+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2404.16599","created_at":"2026-07-05T08:12:09.702448+00:00"},{"alias_kind":"pith_short_12","alias_value":"J7HLBVNTB6YB","created_at":"2026-07-05T08:12:09.702448+00:00"},{"alias_kind":"pith_short_16","alias_value":"J7HLBVNTB6YBKDZF","created_at":"2026-07-05T08:12:09.702448+00:00"},{"alias_kind":"pith_short_8","alias_value":"J7HLBVNT","created_at":"2026-07-05T08:12:09.702448+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.27185","citing_title":"Agnostically decoding gravitational wave model deficiencies in GWTC-3","ref_index":14,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU","json":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU.json","graph_json":"https://pith.science/api/pith-number/J7HLBVNTB6YBKDZFVALNMECPGU/graph.json","events_json":"https://pith.science/api/pith-number/J7HLBVNTB6YBKDZFVALNMECPGU/events.json","paper":"https://pith.science/paper/J7HLBVNT"},"agent_actions":{"view_html":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU","download_json":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU.json","view_paper":"https://pith.science/paper/J7HLBVNT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2404.16599&json=true","fetch_graph":"https://pith.science/api/pith-number/J7HLBVNTB6YBKDZFVALNMECPGU/graph.json","fetch_events":"https://pith.science/api/pith-number/J7HLBVNTB6YBKDZFVALNMECPGU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU/action/storage_attestation","attest_author":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU/action/author_attestation","sign_citation":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU/action/citation_signature","submit_replication":"https://pith.science/pith/J7HLBVNTB6YBKDZFVALNMECPGU/action/replication_record"}},"created_at":"2026-07-05T08:12:09.702448+00:00","updated_at":"2026-07-05T08:12:09.702448+00:00"}