{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:JG5DO45SRHLBQM7WVX5ABFXI7T","short_pith_number":"pith:JG5DO45S","schema_version":"1.0","canonical_sha256":"49ba3773b289d61833f6adfa0096e8fcd727e4cfd4255e2dcdff620783951fa5","source":{"kind":"arxiv","id":"1307.4812","version":3},"attestation_state":"computed","paper":{"title":"Astrophysical signatures of boson stars: quasinormal modes and inspiral resonances","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Caio F. B. Macedo, Lu\\'is C. B. Crispino, Paolo Pani, Vitor Cardoso","submitted_at":"2013-07-18T01:52:28Z","abstract_excerpt":"Compact bosonic field configurations, or boson stars, are promising dark matter candidates which have been invoked as an alternative description for the supermassive compact objects in active galactic nuclei. Boson stars can be comparable in size and mass to supermassive black holes and they are hard to distinguish by electromagnetic observations. However, boson stars do not possess an event horizon and their global spacetime structure is different from that of a black hole. This leaves a characteristic imprint in the gravitational-wave emission, which can be used as a discriminant between bla"},"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":"1307.4812","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2013-07-18T01:52:28Z","cross_cats_sorted":[],"title_canon_sha256":"c70d1acc597ce0c98ab1455eef544698adbf1c71cd0bd35672e960f437193acc","abstract_canon_sha256":"a270ca929cc38567d78373c608003be6e534cc053944ec260b5abd9a14165925"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:12:21.935111Z","signature_b64":"SlwZtbKxb1GaopBtKx2S9TCYYEzc466eU97Vyebc8zqDDop6d/O++xjv50TON8eXYqzGPUbUSNjs/9m3UExZAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"49ba3773b289d61833f6adfa0096e8fcd727e4cfd4255e2dcdff620783951fa5","last_reissued_at":"2026-05-18T03:12:21.934235Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:12:21.934235Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Astrophysical signatures of boson stars: quasinormal modes and inspiral resonances","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Caio F. B. Macedo, Lu\\'is C. B. Crispino, Paolo Pani, Vitor Cardoso","submitted_at":"2013-07-18T01:52:28Z","abstract_excerpt":"Compact bosonic field configurations, or boson stars, are promising dark matter candidates which have been invoked as an alternative description for the supermassive compact objects in active galactic nuclei. Boson stars can be comparable in size and mass to supermassive black holes and they are hard to distinguish by electromagnetic observations. However, boson stars do not possess an event horizon and their global spacetime structure is different from that of a black hole. This leaves a characteristic imprint in the gravitational-wave emission, which can be used as a discriminant between bla"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1307.4812","kind":"arxiv","version":3},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"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":"1307.4812","created_at":"2026-05-18T03:12:21.934379+00:00"},{"alias_kind":"arxiv_version","alias_value":"1307.4812v3","created_at":"2026-05-18T03:12:21.934379+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1307.4812","created_at":"2026-05-18T03:12:21.934379+00:00"},{"alias_kind":"pith_short_12","alias_value":"JG5DO45SRHLB","created_at":"2026-05-18T12:27:49.015174+00:00"},{"alias_kind":"pith_short_16","alias_value":"JG5DO45SRHLBQM7W","created_at":"2026-05-18T12:27:49.015174+00:00"},{"alias_kind":"pith_short_8","alias_value":"JG5DO45S","created_at":"2026-05-18T12:27:49.015174+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":8,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.09563","citing_title":"Light Rings, Accretion Disks and Shadows of Hayward Boson Stars","ref_index":75,"is_internal_anchor":true},{"citing_arxiv_id":"1904.05363","citing_title":"Testing the nature of dark compact objects: a status report","ref_index":86,"is_internal_anchor":false},{"citing_arxiv_id":"2605.09521","citing_title":"Bayesian Analysis of Massive Boson Star Models for Sagittarius A* Using Near-Infrared Astrometry Data","ref_index":41,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25582","citing_title":"Lessons from binary dynamics of inspiralling equal-mass boson-star mergers","ref_index":66,"is_internal_anchor":false},{"citing_arxiv_id":"2604.21883","citing_title":"Testing solitonic boson star interpretations of Sagittarius A* with near-infrared flare astrometry","ref_index":7,"is_internal_anchor":false},{"citing_arxiv_id":"2604.18680","citing_title":"Beyond Three Terms: Continued Fractions for Rotating Black Holes in Modified Gravity","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2604.11893","citing_title":"Relativistic signatures of scalar dark matter in extreme-mass-ratio inspirals","ref_index":86,"is_internal_anchor":false},{"citing_arxiv_id":"2604.06009","citing_title":"Are Black Holes Fuzzballs? Probing Horizon-Scale Structure with LISA","ref_index":74,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T","json":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T.json","graph_json":"https://pith.science/api/pith-number/JG5DO45SRHLBQM7WVX5ABFXI7T/graph.json","events_json":"https://pith.science/api/pith-number/JG5DO45SRHLBQM7WVX5ABFXI7T/events.json","paper":"https://pith.science/paper/JG5DO45S"},"agent_actions":{"view_html":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T","download_json":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T.json","view_paper":"https://pith.science/paper/JG5DO45S","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1307.4812&json=true","fetch_graph":"https://pith.science/api/pith-number/JG5DO45SRHLBQM7WVX5ABFXI7T/graph.json","fetch_events":"https://pith.science/api/pith-number/JG5DO45SRHLBQM7WVX5ABFXI7T/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T/action/storage_attestation","attest_author":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T/action/author_attestation","sign_citation":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T/action/citation_signature","submit_replication":"https://pith.science/pith/JG5DO45SRHLBQM7WVX5ABFXI7T/action/replication_record"}},"created_at":"2026-05-18T03:12:21.934379+00:00","updated_at":"2026-05-18T03:12:21.934379+00:00"}