{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:G7JEAIFRSJFLXK3NRDLOJ2QQIE","short_pith_number":"pith:G7JEAIFR","schema_version":"1.0","canonical_sha256":"37d24020b1924abbab6d88d6e4ea1041266bd4589c24161bc2abdc464a98b2f0","source":{"kind":"arxiv","id":"2311.05815","version":3},"attestation_state":"computed","paper":{"title":"Potential Impact of the Sagittarius Dwarf Galaxy on the Formation of Young O-rich Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Chao Liu, Lifei Ye, Shaolan Bi, Tanda Li, Tiancheng Sun, Tobias Buck, Xianfei Zhang, Xunzhou Chen, Yaguang Li, Yaqian Wu, Yuqin Chen, Yuxi (Lucy) Lu, Zhishuai Ge","submitted_at":"2023-11-10T01:25:03Z","abstract_excerpt":"The Milky Way underwent significant transformations in its early history, characterised by violent mergers and satellite galaxy accretion. However, recent observations reveal notable star formation events over the past 4 Gyr, likely triggered by perturbations from the Sagittarius dwarf galaxy. Here, we present chemical signatures of this accretion event, using the [Fe/H] (metallicity) and [O/Fe] (oxygen abundance) ratios of thin-disc stars. In the normalised age-metallicity plane, we identify a discontinuous V-shape structure at z$_{\\rm max}$ (maximum vertical distance from the disc plane) $<$"},"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":"2311.05815","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2023-11-10T01:25:03Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"6b654fff9d0cf1f0f4541e8286c7c6d7f82130f8ea0056c2d9ebb6dc708175ea","abstract_canon_sha256":"92731f438a6b1866d04ac5b9dda2842c6bd790b3a04fadb18a442a817d3c881c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:43:34.294614Z","signature_b64":"KMD7OEDtCeAC43CN7ik0CifgO+Wc7bpbv8n2UaTy4Fvp3tYt6nEM+sz+K82e83GswiUM4upbjmpldd/FahVzDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"37d24020b1924abbab6d88d6e4ea1041266bd4589c24161bc2abdc464a98b2f0","last_reissued_at":"2026-07-05T10:43:34.294097Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:43:34.294097Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Potential Impact of the Sagittarius Dwarf Galaxy on the Formation of Young O-rich Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Chao Liu, Lifei Ye, Shaolan Bi, Tanda Li, Tiancheng Sun, Tobias Buck, Xianfei Zhang, Xunzhou Chen, Yaguang Li, Yaqian Wu, Yuqin Chen, Yuxi (Lucy) Lu, Zhishuai Ge","submitted_at":"2023-11-10T01:25:03Z","abstract_excerpt":"The Milky Way underwent significant transformations in its early history, characterised by violent mergers and satellite galaxy accretion. However, recent observations reveal notable star formation events over the past 4 Gyr, likely triggered by perturbations from the Sagittarius dwarf galaxy. Here, we present chemical signatures of this accretion event, using the [Fe/H] (metallicity) and [O/Fe] (oxygen abundance) ratios of thin-disc stars. In the normalised age-metallicity plane, we identify a discontinuous V-shape structure at z$_{\\rm max}$ (maximum vertical distance from the disc plane) $<$"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2311.05815","kind":"arxiv","version":3},"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/2311.05815/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":"2311.05815","created_at":"2026-07-05T10:43:34.294146+00:00"},{"alias_kind":"arxiv_version","alias_value":"2311.05815v3","created_at":"2026-07-05T10:43:34.294146+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2311.05815","created_at":"2026-07-05T10:43:34.294146+00:00"},{"alias_kind":"pith_short_12","alias_value":"G7JEAIFRSJFL","created_at":"2026-07-05T10:43:34.294146+00:00"},{"alias_kind":"pith_short_16","alias_value":"G7JEAIFRSJFLXK3N","created_at":"2026-07-05T10:43:34.294146+00:00"},{"alias_kind":"pith_short_8","alias_value":"G7JEAIFR","created_at":"2026-07-05T10:43:34.294146+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.06666","citing_title":"Detailed Abundance Determination of Metal-Poor Stars with X-Shooter II. - Chemically Disentangling the Halo, Disk and GSE","ref_index":145,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE","json":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE.json","graph_json":"https://pith.science/api/pith-number/G7JEAIFRSJFLXK3NRDLOJ2QQIE/graph.json","events_json":"https://pith.science/api/pith-number/G7JEAIFRSJFLXK3NRDLOJ2QQIE/events.json","paper":"https://pith.science/paper/G7JEAIFR"},"agent_actions":{"view_html":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE","download_json":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE.json","view_paper":"https://pith.science/paper/G7JEAIFR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2311.05815&json=true","fetch_graph":"https://pith.science/api/pith-number/G7JEAIFRSJFLXK3NRDLOJ2QQIE/graph.json","fetch_events":"https://pith.science/api/pith-number/G7JEAIFRSJFLXK3NRDLOJ2QQIE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE/action/storage_attestation","attest_author":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE/action/author_attestation","sign_citation":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE/action/citation_signature","submit_replication":"https://pith.science/pith/G7JEAIFRSJFLXK3NRDLOJ2QQIE/action/replication_record"}},"created_at":"2026-07-05T10:43:34.294146+00:00","updated_at":"2026-07-05T10:43:34.294146+00:00"}