{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:XZNGQ62T4HL4KGK5LQE5E24TOH","short_pith_number":"pith:XZNGQ62T","schema_version":"1.0","canonical_sha256":"be5a687b53e1d7c5195d5c09d26b9371e7b1400966417d76c2d53b2952057174","source":{"kind":"arxiv","id":"1604.03842","version":1},"attestation_state":"computed","paper":{"title":"Spectral classification and properties of the O Vz stars in the Galactic O-Star Spectroscopic Survey (GOSSS)","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Alfredo Sota, Amparo Marco, Artemio Herrero, Carolina Sabin-Sanjulian, Emilio J. Alfaro, Ignacio Negueruela, Jesus Maiz Apellaniz, Joao R. S. Leao, Julia I. Arias, Nidia I. Morrell, Nolan R. Walborn, Roberto C. Gamen, Rodolfo H. Barba, Sergio Simon-Diaz","submitted_at":"2016-04-13T15:48:12Z","abstract_excerpt":"On the basis of the Galactic O-Star Spectroscopic Survey (GOSSS), a detailed systematic investigation of the O Vz stars is presented. The currently used spectral classification criteria are rediscussed, and the Vz phenomenon is recalibrated through the addition of a quantitative criterion based on the equivalent widths of the He I 4471, He II 4542, and He II 4686 spectral lines. The GOSSS O Vz and O V populations resulting from the newly adopted spectral classification criteria are comparatively analyzed. The locations of the O Vz stars are probed, showing a concentration of the most extreme c"},"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":"1604.03842","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2016-04-13T15:48:12Z","cross_cats_sorted":[],"title_canon_sha256":"28960b08103cf687982c2ff6dfae934c868ae9ec610affa19aa651f3bfa27269","abstract_canon_sha256":"7bef4f61492f85aa7ea0314869ee78b459b102de1c949650117e6365d88dd5b4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:10:49.853145Z","signature_b64":"6FmWxyR6ilJSHvYaBKr/HrZz8PFdz91BZf35Zg3tN5zMQJyE23hyeNbW69yfWPQWOhaSXc8MA2k+jskF/QhVCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"be5a687b53e1d7c5195d5c09d26b9371e7b1400966417d76c2d53b2952057174","last_reissued_at":"2026-05-18T01:10:49.852524Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:10:49.852524Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Spectral classification and properties of the O Vz stars in the Galactic O-Star Spectroscopic Survey (GOSSS)","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Alfredo Sota, Amparo Marco, Artemio Herrero, Carolina Sabin-Sanjulian, Emilio J. Alfaro, Ignacio Negueruela, Jesus Maiz Apellaniz, Joao R. S. Leao, Julia I. Arias, Nidia I. Morrell, Nolan R. Walborn, Roberto C. Gamen, Rodolfo H. Barba, Sergio Simon-Diaz","submitted_at":"2016-04-13T15:48:12Z","abstract_excerpt":"On the basis of the Galactic O-Star Spectroscopic Survey (GOSSS), a detailed systematic investigation of the O Vz stars is presented. The currently used spectral classification criteria are rediscussed, and the Vz phenomenon is recalibrated through the addition of a quantitative criterion based on the equivalent widths of the He I 4471, He II 4542, and He II 4686 spectral lines. The GOSSS O Vz and O V populations resulting from the newly adopted spectral classification criteria are comparatively analyzed. The locations of the O Vz stars are probed, showing a concentration of the most extreme c"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1604.03842","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":""},"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":"1604.03842","created_at":"2026-05-18T01:10:49.852620+00:00"},{"alias_kind":"arxiv_version","alias_value":"1604.03842v1","created_at":"2026-05-18T01:10:49.852620+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1604.03842","created_at":"2026-05-18T01:10:49.852620+00:00"},{"alias_kind":"pith_short_12","alias_value":"XZNGQ62T4HL4","created_at":"2026-05-18T12:30:51.357362+00:00"},{"alias_kind":"pith_short_16","alias_value":"XZNGQ62T4HL4KGK5","created_at":"2026-05-18T12:30:51.357362+00:00"},{"alias_kind":"pith_short_8","alias_value":"XZNGQ62T","created_at":"2026-05-18T12:30:51.357362+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH","json":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH.json","graph_json":"https://pith.science/api/pith-number/XZNGQ62T4HL4KGK5LQE5E24TOH/graph.json","events_json":"https://pith.science/api/pith-number/XZNGQ62T4HL4KGK5LQE5E24TOH/events.json","paper":"https://pith.science/paper/XZNGQ62T"},"agent_actions":{"view_html":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH","download_json":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH.json","view_paper":"https://pith.science/paper/XZNGQ62T","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1604.03842&json=true","fetch_graph":"https://pith.science/api/pith-number/XZNGQ62T4HL4KGK5LQE5E24TOH/graph.json","fetch_events":"https://pith.science/api/pith-number/XZNGQ62T4HL4KGK5LQE5E24TOH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH/action/storage_attestation","attest_author":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH/action/author_attestation","sign_citation":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH/action/citation_signature","submit_replication":"https://pith.science/pith/XZNGQ62T4HL4KGK5LQE5E24TOH/action/replication_record"}},"created_at":"2026-05-18T01:10:49.852620+00:00","updated_at":"2026-05-18T01:10:49.852620+00:00"}