{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:D7PGHT2O57U52RNYFXIYQM3SWA","short_pith_number":"pith:D7PGHT2O","schema_version":"1.0","canonical_sha256":"1fde63cf4eefe9dd45b82dd1883372b026a3f87d42537c84dea17aa9310d3304","source":{"kind":"arxiv","id":"2105.12380","version":1},"attestation_state":"computed","paper":{"title":"Multiplicity of Galactic Luminous Blue Variable stars","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Lobel, B. Miszalski, C. Lanthermann, D. Hutsem\\'ekers, E. Gosset, H. Sana, J. Kluska, L. Mahy, M. Reggiani, R. Manick","submitted_at":"2021-05-26T07:50:45Z","abstract_excerpt":"Context. Luminous Blue Variables (LBVs) are thought to be in a transitory phase between O stars on the main-sequence and the Wolf-Rayet stage. Recent studies suggest that they might be formed through binary interaction. Only a few are known in binary systems but their multiplicity fraction is uncertain. Aims. This study aims at deriving the binary fraction among the Galactic (confirmed and candidate) LBV population. We combine multi-epoch spectroscopy and long-baseline interferometry. Methods. We use cross-correlation to measure their radial velocities. We identify spectroscopic binaries throu"},"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":"2105.12380","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2021-05-26T07:50:45Z","cross_cats_sorted":[],"title_canon_sha256":"2103d0844808257df86c10f103a8a54c33491cd9ba65195c230b72e4ee5f95b9","abstract_canon_sha256":"c0c6d1b7a2bb5e6d406bcdc720d7bc3b77a8e6728b28c8725ac294c87c82610e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:42:42.296502Z","signature_b64":"p/IvREDSEAq28S3wEwohDW1jZ4pPimkW2L9QIO5sKxErX0pCYI2TnFo1XPbq5J7aOyCJ3AhkdEB0kE+glG8+AA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1fde63cf4eefe9dd45b82dd1883372b026a3f87d42537c84dea17aa9310d3304","last_reissued_at":"2026-07-05T03:42:42.296064Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:42:42.296064Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Multiplicity of Galactic Luminous Blue Variable stars","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Lobel, B. Miszalski, C. Lanthermann, D. Hutsem\\'ekers, E. Gosset, H. Sana, J. Kluska, L. Mahy, M. Reggiani, R. Manick","submitted_at":"2021-05-26T07:50:45Z","abstract_excerpt":"Context. Luminous Blue Variables (LBVs) are thought to be in a transitory phase between O stars on the main-sequence and the Wolf-Rayet stage. Recent studies suggest that they might be formed through binary interaction. Only a few are known in binary systems but their multiplicity fraction is uncertain. Aims. This study aims at deriving the binary fraction among the Galactic (confirmed and candidate) LBV population. We combine multi-epoch spectroscopy and long-baseline interferometry. Methods. We use cross-correlation to measure their radial velocities. We identify spectroscopic binaries throu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2105.12380","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/2105.12380/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":"2105.12380","created_at":"2026-07-05T03:42:42.296131+00:00"},{"alias_kind":"arxiv_version","alias_value":"2105.12380v1","created_at":"2026-07-05T03:42:42.296131+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2105.12380","created_at":"2026-07-05T03:42:42.296131+00:00"},{"alias_kind":"pith_short_12","alias_value":"D7PGHT2O57U5","created_at":"2026-07-05T03:42:42.296131+00:00"},{"alias_kind":"pith_short_16","alias_value":"D7PGHT2O57U52RNY","created_at":"2026-07-05T03:42:42.296131+00:00"},{"alias_kind":"pith_short_8","alias_value":"D7PGHT2O","created_at":"2026-07-05T03:42:42.296131+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07068","citing_title":"Unveiling the Milky Way with a Gaia DR3 census of OB-type stars within 2 kpc. I. Tracing local Galactic structure, massive star-forming regions and core-collapse supernova progenitors","ref_index":11,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA","json":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA.json","graph_json":"https://pith.science/api/pith-number/D7PGHT2O57U52RNYFXIYQM3SWA/graph.json","events_json":"https://pith.science/api/pith-number/D7PGHT2O57U52RNYFXIYQM3SWA/events.json","paper":"https://pith.science/paper/D7PGHT2O"},"agent_actions":{"view_html":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA","download_json":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA.json","view_paper":"https://pith.science/paper/D7PGHT2O","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2105.12380&json=true","fetch_graph":"https://pith.science/api/pith-number/D7PGHT2O57U52RNYFXIYQM3SWA/graph.json","fetch_events":"https://pith.science/api/pith-number/D7PGHT2O57U52RNYFXIYQM3SWA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA/action/storage_attestation","attest_author":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA/action/author_attestation","sign_citation":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA/action/citation_signature","submit_replication":"https://pith.science/pith/D7PGHT2O57U52RNYFXIYQM3SWA/action/replication_record"}},"created_at":"2026-07-05T03:42:42.296131+00:00","updated_at":"2026-07-05T03:42:42.296131+00:00"}