{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:I4BA6XOWSXLUF3MMRUM4ASQOO2","short_pith_number":"pith:I4BA6XOW","schema_version":"1.0","canonical_sha256":"47020f5dd695d742ed8c8d19c04a0e76a7017ce0dfc6351374c630a2b1e956ed","source":{"kind":"arxiv","id":"2411.02508","version":1},"attestation_state":"computed","paper":{"title":"Hubble Space Telescope survey of Magellanic Cloud star clusters. Binaries among the split main sequences of NGC 1818, NGC 1850, and NGC 2164","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. F. Marino, A. P. Milone, C. He, C. Li, E. Bortolan, E. Dondoglio, E. J. Nastasio, E. P. Lagioia, F. D'Antona, F. Dell'Agli, F. Muratore, G. Cordoni, L. Deng, M. Bernizzoni, M. Tailo, M. V. Legnardi, P. Ventura, T. Ziliotto","submitted_at":"2024-11-04T19:00:07Z","abstract_excerpt":"Nearly all star clusters younger than ~600 Myr exhibit extended main sequence turn offs and split main sequences (MSs) in their color-magnitude diagrams. Works based on both photometry and spectroscopy have firmly demonstrated that the red MS is composed of fast-rotating stars, whereas blue MS stars are slow rotators. Nevertheless, the mechanism responsible for the formation of stellar populations with varying rotation rates remains a topic of debate. Potential mechanisms proposed for the split MS include binary interactions, early evolution of pre-main sequence stars, and the merging of binar"},"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":"2411.02508","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2024-11-04T19:00:07Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"ea89ad81187c6dfe90b09baf768a0b1fb038654209e9bfd0e32a786872817aa0","abstract_canon_sha256":"40fd59b4ef77ded2ba37b2bc217a3961825254a6117e302fc8a2bf09399011a8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:47:23.319657Z","signature_b64":"lvDX5GiB7jSafTsY0aXNrKJqyfQJPWuNn/a6qUlbKTSRpyCUqe26QmlfRWdSprIPsEs4WRIhPOIAPHVBtNIUBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"47020f5dd695d742ed8c8d19c04a0e76a7017ce0dfc6351374c630a2b1e956ed","last_reissued_at":"2026-07-05T09:47:23.318822Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:47:23.318822Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Hubble Space Telescope survey of Magellanic Cloud star clusters. Binaries among the split main sequences of NGC 1818, NGC 1850, and NGC 2164","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. F. Marino, A. P. Milone, C. He, C. Li, E. Bortolan, E. Dondoglio, E. J. Nastasio, E. P. Lagioia, F. D'Antona, F. Dell'Agli, F. Muratore, G. Cordoni, L. Deng, M. Bernizzoni, M. Tailo, M. V. Legnardi, P. Ventura, T. Ziliotto","submitted_at":"2024-11-04T19:00:07Z","abstract_excerpt":"Nearly all star clusters younger than ~600 Myr exhibit extended main sequence turn offs and split main sequences (MSs) in their color-magnitude diagrams. Works based on both photometry and spectroscopy have firmly demonstrated that the red MS is composed of fast-rotating stars, whereas blue MS stars are slow rotators. Nevertheless, the mechanism responsible for the formation of stellar populations with varying rotation rates remains a topic of debate. Potential mechanisms proposed for the split MS include binary interactions, early evolution of pre-main sequence stars, and the merging of binar"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2411.02508","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/2411.02508/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":"2411.02508","created_at":"2026-07-05T09:47:23.319071+00:00"},{"alias_kind":"arxiv_version","alias_value":"2411.02508v1","created_at":"2026-07-05T09:47:23.319071+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2411.02508","created_at":"2026-07-05T09:47:23.319071+00:00"},{"alias_kind":"pith_short_12","alias_value":"I4BA6XOWSXLU","created_at":"2026-07-05T09:47:23.319071+00:00"},{"alias_kind":"pith_short_16","alias_value":"I4BA6XOWSXLUF3MM","created_at":"2026-07-05T09:47:23.319071+00:00"},{"alias_kind":"pith_short_8","alias_value":"I4BA6XOW","created_at":"2026-07-05T09:47:23.319071+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.09217","citing_title":"Fast-rotating A- and F-type stars with H{\\alpha} emissions in NGC 3532, candidate UV-dim stars?","ref_index":69,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2","json":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2.json","graph_json":"https://pith.science/api/pith-number/I4BA6XOWSXLUF3MMRUM4ASQOO2/graph.json","events_json":"https://pith.science/api/pith-number/I4BA6XOWSXLUF3MMRUM4ASQOO2/events.json","paper":"https://pith.science/paper/I4BA6XOW"},"agent_actions":{"view_html":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2","download_json":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2.json","view_paper":"https://pith.science/paper/I4BA6XOW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2411.02508&json=true","fetch_graph":"https://pith.science/api/pith-number/I4BA6XOWSXLUF3MMRUM4ASQOO2/graph.json","fetch_events":"https://pith.science/api/pith-number/I4BA6XOWSXLUF3MMRUM4ASQOO2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2/action/storage_attestation","attest_author":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2/action/author_attestation","sign_citation":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2/action/citation_signature","submit_replication":"https://pith.science/pith/I4BA6XOWSXLUF3MMRUM4ASQOO2/action/replication_record"}},"created_at":"2026-07-05T09:47:23.319071+00:00","updated_at":"2026-07-05T09:47:23.319071+00:00"}