{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:PVJUW3EGDI74MFEMIIAMGM3UUV","short_pith_number":"pith:PVJUW3EG","schema_version":"1.0","canonical_sha256":"7d534b6c861a3fc6148c4200c33374a56d82f50864b3744eb145ddf4afcc7298","source":{"kind":"arxiv","id":"2111.04135","version":1},"attestation_state":"computed","paper":{"title":"Population inference of spin-induced quadrupole moments as a probe for non-black hole compact binaries","license":"http://creativecommons.org/publicdomain/zero/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Abhirup Ghosh, Anuradha Gupta, Archisman Ghosh, K. G. Arun, Muhammed Saleem, N. V. Krishnendu, W. Del Pozzo","submitted_at":"2021-11-07T17:51:04Z","abstract_excerpt":"Gravitational-wave (GW) measurements of physical effects such as spin-induced quadrupole moments can distinguish binaries consisting of black holes from non-black hole binaries. While these effects may be poorly constrained for single-event inferences with the second-generation detectors, combining information from multiple detections can help uncover features of non-black hole binaries. The spin-induced quadrupole moment has specific predictions for different types of compact objects, and a generalized formalism must consider a population where different types of compact objects co-exist. 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":"2111.04135","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/publicdomain/zero/1.0/","primary_cat":"gr-qc","submitted_at":"2021-11-07T17:51:04Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"c86618ae24dd5de66f9bd3dc8149d271c354e46942af178dac6fd561684a3b67","abstract_canon_sha256":"10260b6f43d9800a15b45ce2f89247a77464cb31c09220d2b03d59dc019d7927"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:29:27.017636Z","signature_b64":"IwwkaIrAzJ24dI0JF9rcD81+bwPHULJAQsu+PZIX4NS98AT83vCtxSOvP+eiJ0CB16FkvU9eYt2agFq1hmpNBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7d534b6c861a3fc6148c4200c33374a56d82f50864b3744eb145ddf4afcc7298","last_reissued_at":"2026-07-05T04:29:27.017171Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:29:27.017171Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Population inference of spin-induced quadrupole moments as a probe for non-black hole compact binaries","license":"http://creativecommons.org/publicdomain/zero/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Abhirup Ghosh, Anuradha Gupta, Archisman Ghosh, K. G. Arun, Muhammed Saleem, N. V. Krishnendu, W. Del Pozzo","submitted_at":"2021-11-07T17:51:04Z","abstract_excerpt":"Gravitational-wave (GW) measurements of physical effects such as spin-induced quadrupole moments can distinguish binaries consisting of black holes from non-black hole binaries. While these effects may be poorly constrained for single-event inferences with the second-generation detectors, combining information from multiple detections can help uncover features of non-black hole binaries. The spin-induced quadrupole moment has specific predictions for different types of compact objects, and a generalized formalism must consider a population where different types of compact objects co-exist. In "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2111.04135","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/2111.04135/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":"2111.04135","created_at":"2026-07-05T04:29:27.017229+00:00"},{"alias_kind":"arxiv_version","alias_value":"2111.04135v1","created_at":"2026-07-05T04:29:27.017229+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2111.04135","created_at":"2026-07-05T04:29:27.017229+00:00"},{"alias_kind":"pith_short_12","alias_value":"PVJUW3EGDI74","created_at":"2026-07-05T04:29:27.017229+00:00"},{"alias_kind":"pith_short_16","alias_value":"PVJUW3EGDI74MFEM","created_at":"2026-07-05T04:29:27.017229+00:00"},{"alias_kind":"pith_short_8","alias_value":"PVJUW3EG","created_at":"2026-07-05T04:29:27.017229+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2112.06861","citing_title":"Tests of General Relativity with GWTC-3","ref_index":239,"is_internal_anchor":false},{"citing_arxiv_id":"2604.09828","citing_title":"Testing the Kerr hypothesis beyond the quadrupole with GW241011","ref_index":25,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV","json":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV.json","graph_json":"https://pith.science/api/pith-number/PVJUW3EGDI74MFEMIIAMGM3UUV/graph.json","events_json":"https://pith.science/api/pith-number/PVJUW3EGDI74MFEMIIAMGM3UUV/events.json","paper":"https://pith.science/paper/PVJUW3EG"},"agent_actions":{"view_html":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV","download_json":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV.json","view_paper":"https://pith.science/paper/PVJUW3EG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2111.04135&json=true","fetch_graph":"https://pith.science/api/pith-number/PVJUW3EGDI74MFEMIIAMGM3UUV/graph.json","fetch_events":"https://pith.science/api/pith-number/PVJUW3EGDI74MFEMIIAMGM3UUV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV/action/storage_attestation","attest_author":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV/action/author_attestation","sign_citation":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV/action/citation_signature","submit_replication":"https://pith.science/pith/PVJUW3EGDI74MFEMIIAMGM3UUV/action/replication_record"}},"created_at":"2026-07-05T04:29:27.017229+00:00","updated_at":"2026-07-05T04:29:27.017229+00:00"}