{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:U6AEIRZAF6QAE2XAHCMG7HQ4WM","short_pith_number":"pith:U6AEIRZA","schema_version":"1.0","canonical_sha256":"a7804447202fa0026ae038986f9e1cb30b69606fd47e256cef50714dacb175ed","source":{"kind":"arxiv","id":"2503.08190","version":1},"attestation_state":"computed","paper":{"title":"Another one (BH+OB pair) bites the dust","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Gregor Rauw (ULiege), Yael Naze","submitted_at":"2025-03-11T08:54:48Z","abstract_excerpt":"Most (or possibly all) massive stars reside in multiple systems. From stellar evolution models, numerous systems with an OB star coupled to a black hole would be expected to exist. There have been several claimed detections of such pairs in recent years and this is notably the case of HD96670. Using high-quality photometry and spectroscopy in the optical range, we revisited the HD96670 system. We also examined complementary X-ray observations to provide a broader view of the system properties. The TESS light curves of HD96670 clearly show eclipses, ruling out the black hole companion scenario."},"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":"2503.08190","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2025-03-11T08:54:48Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"3298e81058629ee4c8fee37897ba517527e1f2840a7842fc0962544c4092122d","abstract_canon_sha256":"7794904fdf99ca12fbcd9d41b18bc17014e18f15baa46f20afb2fbfc1edb4d57"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:28:53.421770Z","signature_b64":"xSIpMNQC7ak15E3JwFvTtYh0OSwhwL2aEzuzYEbC7qxWYnZBgjQPLL2j7X64Pl+O4SIOE2YYi2qsHVHci5ikBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a7804447202fa0026ae038986f9e1cb30b69606fd47e256cef50714dacb175ed","last_reissued_at":"2026-07-05T10:28:53.421194Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:28:53.421194Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Another one (BH+OB pair) bites the dust","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Gregor Rauw (ULiege), Yael Naze","submitted_at":"2025-03-11T08:54:48Z","abstract_excerpt":"Most (or possibly all) massive stars reside in multiple systems. From stellar evolution models, numerous systems with an OB star coupled to a black hole would be expected to exist. There have been several claimed detections of such pairs in recent years and this is notably the case of HD96670. Using high-quality photometry and spectroscopy in the optical range, we revisited the HD96670 system. We also examined complementary X-ray observations to provide a broader view of the system properties. The TESS light curves of HD96670 clearly show eclipses, ruling out the black hole companion scenario."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2503.08190","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/2503.08190/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":"2503.08190","created_at":"2026-07-05T10:28:53.421256+00:00"},{"alias_kind":"arxiv_version","alias_value":"2503.08190v1","created_at":"2026-07-05T10:28:53.421256+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2503.08190","created_at":"2026-07-05T10:28:53.421256+00:00"},{"alias_kind":"pith_short_12","alias_value":"U6AEIRZAF6QA","created_at":"2026-07-05T10:28:53.421256+00:00"},{"alias_kind":"pith_short_16","alias_value":"U6AEIRZAF6QAE2XA","created_at":"2026-07-05T10:28:53.421256+00:00"},{"alias_kind":"pith_short_8","alias_value":"U6AEIRZA","created_at":"2026-07-05T10:28:53.421256+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.05421","citing_title":"The IACOB project XVIII. Prevalence of short-period binaries among Galactic helium rich O-type stars","ref_index":175,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM","json":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM.json","graph_json":"https://pith.science/api/pith-number/U6AEIRZAF6QAE2XAHCMG7HQ4WM/graph.json","events_json":"https://pith.science/api/pith-number/U6AEIRZAF6QAE2XAHCMG7HQ4WM/events.json","paper":"https://pith.science/paper/U6AEIRZA"},"agent_actions":{"view_html":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM","download_json":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM.json","view_paper":"https://pith.science/paper/U6AEIRZA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2503.08190&json=true","fetch_graph":"https://pith.science/api/pith-number/U6AEIRZAF6QAE2XAHCMG7HQ4WM/graph.json","fetch_events":"https://pith.science/api/pith-number/U6AEIRZAF6QAE2XAHCMG7HQ4WM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM/action/storage_attestation","attest_author":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM/action/author_attestation","sign_citation":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM/action/citation_signature","submit_replication":"https://pith.science/pith/U6AEIRZAF6QAE2XAHCMG7HQ4WM/action/replication_record"}},"created_at":"2026-07-05T10:28:53.421256+00:00","updated_at":"2026-07-05T10:28:53.421256+00:00"}