{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:KJLI2VFA2AIS72SG4VEIZUIKPI","short_pith_number":"pith:KJLI2VFA","schema_version":"1.0","canonical_sha256":"52568d54a0d0112fea46e5488cd10a7a0a5e60edd49be6e6a544de2a9d55d60b","source":{"kind":"arxiv","id":"2604.02111","version":3},"attestation_state":"computed","paper":{"title":"Multiplicity of Massive stars in the Milky Way (M3W). I. Project description, UNWIND, application to GLS 11 448, and DIB catalog","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"The binary GLS 11 448 contains two O3.5 II(f*) stars with evolutionary masses of 70 and 76 solar masses, the highest measured for O stars.","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. Pellerin, E. Madero Fuentes, G. Holgado, J. A. Molina-Calzada, J. I. Arias, J. Ma\\'iz Apell\\'aniz, M. Abdul-Masih, R. C. Gamen, R. H. Barb\\'a, S. Rosu, S. Sim\\'on-D\\'iaz","submitted_at":"2026-04-02T14:45:42Z","abstract_excerpt":"(ABRIDGED BUT NOT TOO FAR) Multiplicity is ubiquitous among massive stars and its understanding is constrained by the sample of well-determined orbits. The immediate goal of M3W is to significantly increase the number of massive multiple systems with well-determined orbits and masses. We will address issues such as multiplicity statistics, the mass function in clusters and the field, the properties of binaries with compact companions and gravitational-wave progenitors, the origin and characteristics of runaways and their 3-D motions, the use of apsidal motion as a probe of stellar interiors, a"},"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":true},"canonical_record":{"source":{"id":"2604.02111","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2026-04-02T14:45:42Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"962f24cb1a6296872f1064679244ba5b688f6b440b21a9dccaa3bdee4d8cd75e","abstract_canon_sha256":"d0acd3f93b75fd4e6b7d1198e8377b5fb10885e983e3e31b6d1914225e1682d9"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-23T01:23:35.233106Z","signature_b64":"x26AT9MZGlWlyWyPB36bRNe+fRqobePvwTTF7TCmokUe5FAD1RzLkLAeQziUlTKxc5BrHB7wCKrbODtMgMIeDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"52568d54a0d0112fea46e5488cd10a7a0a5e60edd49be6e6a544de2a9d55d60b","last_reissued_at":"2026-07-23T01:23:35.232092Z","signature_status":"signed_v1","first_computed_at":"2026-07-23T01:23:35.232092Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Multiplicity of Massive stars in the Milky Way (M3W). I. Project description, UNWIND, application to GLS 11 448, and DIB catalog","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"The binary GLS 11 448 contains two O3.5 II(f*) stars with evolutionary masses of 70 and 76 solar masses, the highest measured for O stars.","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. Pellerin, E. Madero Fuentes, G. Holgado, J. A. Molina-Calzada, J. I. Arias, J. Ma\\'iz Apell\\'aniz, M. Abdul-Masih, R. C. Gamen, R. H. Barb\\'a, S. Rosu, S. Sim\\'on-D\\'iaz","submitted_at":"2026-04-02T14:45:42Z","abstract_excerpt":"(ABRIDGED BUT NOT TOO FAR) Multiplicity is ubiquitous among massive stars and its understanding is constrained by the sample of well-determined orbits. The immediate goal of M3W is to significantly increase the number of massive multiple systems with well-determined orbits and masses. We will address issues such as multiplicity statistics, the mass function in clusters and the field, the properties of binaries with compact companions and gravitational-wave progenitors, the origin and characteristics of runaways and their 3-D motions, the use of apsidal motion as a probe of stellar interiors, a"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"The Aa and Ab components of GLS 11 448, both classified as O3.5 II(f*), are the two most massive O stars ever detected according to the evolutionary masses of 70±10 M⊙ and 76±11 M⊙ determined in this paper.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"Evolutionary masses rest on the assumption that standard stellar evolution tracks apply without major revision to these very massive, rapidly rotating O stars; the disentangling also assumes the UNWIND algorithm can cleanly separate the spectra without residual contamination from wind or circumstellar material.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"M3W reports a new orbit and evolutionary masses of 70 and 76 solar masses for the O3.5 components of GLS 11 448 plus a library of 631 diffuse interstellar bands including 119 new identifications.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"The binary GLS 11 448 contains two O3.5 II(f*) stars with evolutionary masses of 70 and 76 solar masses, the highest measured for O stars.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"f64cbe1ad129c5468d734d21c965a43e6f362686ac0699bc3cf5563b22ae718c"},"source":{"id":"2604.02111","kind":"arxiv","version":3},"verdict":{"id":"505f4657-4142-4b58-af10-d40fe04e78c0","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-13T21:03:01.826553Z","strongest_claim":"The Aa and Ab components of GLS 11 448, both classified as O3.5 II(f*), are the two most massive O stars ever detected according to the evolutionary masses of 70±10 M⊙ and 76±11 M⊙ determined in this paper.","one_line_summary":"M3W reports a new orbit and evolutionary masses of 70 and 76 solar masses for the O3.5 components of GLS 11 448 plus a library of 631 diffuse interstellar bands including 119 new identifications.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"Evolutionary masses rest on the assumption that standard stellar evolution tracks apply without major revision to these very massive, rapidly rotating O stars; the disentangling also assumes the UNWIND algorithm can cleanly separate the spectra without residual contamination from wind or circumstellar material.","pith_extraction_headline":"The binary GLS 11 448 contains two O3.5 II(f*) stars with evolutionary masses of 70 and 76 solar masses, the highest measured for O stars."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.02111/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":3,"snapshot_sha256":"d4f443e719fef1c4d414b83bfa687ee42d8c22c4478657d0663fd4b04d8b5b3b"},"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":"2604.02111","created_at":"2026-07-23T01:23:35.232558+00:00"},{"alias_kind":"arxiv_version","alias_value":"2604.02111v3","created_at":"2026-07-23T01:23:35.232558+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2604.02111","created_at":"2026-07-23T01:23:35.232558+00:00"},{"alias_kind":"pith_short_12","alias_value":"KJLI2VFA2AIS","created_at":"2026-07-23T01:23:35.232558+00:00"},{"alias_kind":"pith_short_16","alias_value":"KJLI2VFA2AIS72SG","created_at":"2026-07-23T01:23:35.232558+00:00"},{"alias_kind":"pith_short_8","alias_value":"KJLI2VFA","created_at":"2026-07-23T01:23:35.232558+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":147,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":3,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI","json":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI.json","graph_json":"https://pith.science/api/pith-number/KJLI2VFA2AIS72SG4VEIZUIKPI/graph.json","events_json":"https://pith.science/api/pith-number/KJLI2VFA2AIS72SG4VEIZUIKPI/events.json","paper":"https://pith.science/paper/KJLI2VFA"},"agent_actions":{"view_html":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI","download_json":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI.json","view_paper":"https://pith.science/paper/KJLI2VFA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2604.02111&json=true","fetch_graph":"https://pith.science/api/pith-number/KJLI2VFA2AIS72SG4VEIZUIKPI/graph.json","fetch_events":"https://pith.science/api/pith-number/KJLI2VFA2AIS72SG4VEIZUIKPI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI/action/storage_attestation","attest_author":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI/action/author_attestation","sign_citation":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI/action/citation_signature","submit_replication":"https://pith.science/pith/KJLI2VFA2AIS72SG4VEIZUIKPI/action/replication_record"}},"created_at":"2026-07-23T01:23:35.232558+00:00","updated_at":"2026-07-23T01:23:35.232558+00:00"}