{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:XU2MIGWCXADUNE2HYHZH4JK2ER","short_pith_number":"pith:XU2MIGWC","schema_version":"1.0","canonical_sha256":"bd34c41ac2b807469347c1f27e255a24679dd1b99a9cb7948b4972d432a4964f","source":{"kind":"arxiv","id":"2602.16562","version":2},"attestation_state":"computed","paper":{"title":"Testing non-circular black hole spacetime with X-ray reflection","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Cosimo Bambi, Leda Gao, Swarnim Shashank","submitted_at":"2026-02-18T16:03:08Z","abstract_excerpt":"X-ray reflection spectroscopy is a powerful tool for testing the Kerr hypothesis and probing the strong gravity regime around accreting black holes. Most tests of General Relativity (GR) assume that the spacetime around a black hole is circular, meaning the metric possesses a specific symmetry structure common to the Kerr solution. However, deviations from circularity are predicted by various modified gravity theories and non-vacuum General Relativity solutions. In this work, we test a specific non-circular metric constructed based on a locality principle, where the deviation from the Kerr spa"},"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":"2602.16562","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2026-02-18T16:03:08Z","cross_cats_sorted":[],"title_canon_sha256":"906f6dd891bcaefbd4d4e2216babd1c6ba1fb058055b9612ea4f521431e5d8cc","abstract_canon_sha256":"4c1ac3d9a2ffe855933f4b54cf110f213ec12946eab41c20d2c9985c192eac33"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-06-05T00:13:45.577174Z","signature_b64":"EFH3UUT98rIeyATWX9PgxGsNCC0sxvSOu+CEzT18BYBJRWRoH9ie/VdP8WwIPJoWepgX37ODprM7F5j6z88CBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bd34c41ac2b807469347c1f27e255a24679dd1b99a9cb7948b4972d432a4964f","last_reissued_at":"2026-06-05T00:13:45.576553Z","signature_status":"signed_v1","first_computed_at":"2026-06-05T00:13:45.576553Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Testing non-circular black hole spacetime with X-ray reflection","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Cosimo Bambi, Leda Gao, Swarnim Shashank","submitted_at":"2026-02-18T16:03:08Z","abstract_excerpt":"X-ray reflection spectroscopy is a powerful tool for testing the Kerr hypothesis and probing the strong gravity regime around accreting black holes. Most tests of General Relativity (GR) assume that the spacetime around a black hole is circular, meaning the metric possesses a specific symmetry structure common to the Kerr solution. However, deviations from circularity are predicted by various modified gravity theories and non-vacuum General Relativity solutions. In this work, we test a specific non-circular metric constructed based on a locality principle, where the deviation from the Kerr spa"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2602.16562","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/2602.16562/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":"2602.16562","created_at":"2026-06-05T00:13:45.576640+00:00"},{"alias_kind":"arxiv_version","alias_value":"2602.16562v2","created_at":"2026-06-05T00:13:45.576640+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2602.16562","created_at":"2026-06-05T00:13:45.576640+00:00"},{"alias_kind":"pith_short_12","alias_value":"XU2MIGWCXADU","created_at":"2026-06-05T00:13:45.576640+00:00"},{"alias_kind":"pith_short_16","alias_value":"XU2MIGWCXADUNE2H","created_at":"2026-06-05T00:13:45.576640+00:00"},{"alias_kind":"pith_short_8","alias_value":"XU2MIGWC","created_at":"2026-06-05T00:13:45.576640+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.03797","citing_title":"Iron K$\\alpha$ signatures from accretion disks around fermionic dark matter cores","ref_index":26,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER","json":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER.json","graph_json":"https://pith.science/api/pith-number/XU2MIGWCXADUNE2HYHZH4JK2ER/graph.json","events_json":"https://pith.science/api/pith-number/XU2MIGWCXADUNE2HYHZH4JK2ER/events.json","paper":"https://pith.science/paper/XU2MIGWC"},"agent_actions":{"view_html":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER","download_json":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER.json","view_paper":"https://pith.science/paper/XU2MIGWC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2602.16562&json=true","fetch_graph":"https://pith.science/api/pith-number/XU2MIGWCXADUNE2HYHZH4JK2ER/graph.json","fetch_events":"https://pith.science/api/pith-number/XU2MIGWCXADUNE2HYHZH4JK2ER/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER/action/storage_attestation","attest_author":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER/action/author_attestation","sign_citation":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER/action/citation_signature","submit_replication":"https://pith.science/pith/XU2MIGWCXADUNE2HYHZH4JK2ER/action/replication_record"}},"created_at":"2026-06-05T00:13:45.576640+00:00","updated_at":"2026-06-05T00:13:45.576640+00:00"}