{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:HPJL2CWTDXVFWHTCUF6KFJ4YYS","short_pith_number":"pith:HPJL2CWT","schema_version":"1.0","canonical_sha256":"3bd2bd0ad31dea5b1e62a17ca2a798c4b83ab8cd3632ecea1fca4f5ed3c66d1b","source":{"kind":"arxiv","id":"1608.06390","version":2},"attestation_state":"computed","paper":{"title":"Non-LTE line formation of Fe in late-type stars - III. 3D non-LTE analysis of metal-poor stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. M. Amarsi, K. Lind, M. Asplund, P. S. Barklem, R. Collet","submitted_at":"2016-08-23T05:47:35Z","abstract_excerpt":"As one of the most important elements in astronomy, iron abundance determinations need to be as accurate as possible. We investigate the accuracy of spectroscopic iron abundance analyses using archetypal metal-poor stars. We perform detailed 3D non-LTE radiative transfer calculations based on 3D hydrodynamic Stagger model atmospheres, and employ a new model atom that includes new quantum-mechanical neutral hydrogen collisional rate coefficients. With the exception of the red giant HD122563, we find that the 3D non-LTE models achieve Fe i/Fe ii excitation and ionization balance as well as not h"},"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":"1608.06390","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2016-08-23T05:47:35Z","cross_cats_sorted":[],"title_canon_sha256":"6f7f9e60b2e39dfcecd6cf7b6c7f278a37a3879b1d033259163e03f56cbc4fd6","abstract_canon_sha256":"0caff34d1ad2b3b7debdb4309ba101dcd4fb811716e857b9b471c9d822603f83"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:04:41.011800Z","signature_b64":"BHU7C8zbaryah4xDl1bBrGJ25D2QTsgYnSWcGvL3b0cgNwSEHex6mOLDHuwW3xuJ1b8PzeYvwPyxiJrs+Eg+BQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3bd2bd0ad31dea5b1e62a17ca2a798c4b83ab8cd3632ecea1fca4f5ed3c66d1b","last_reissued_at":"2026-05-18T01:04:41.010982Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:04:41.010982Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Non-LTE line formation of Fe in late-type stars - III. 3D non-LTE analysis of metal-poor stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. M. Amarsi, K. Lind, M. Asplund, P. S. Barklem, R. Collet","submitted_at":"2016-08-23T05:47:35Z","abstract_excerpt":"As one of the most important elements in astronomy, iron abundance determinations need to be as accurate as possible. We investigate the accuracy of spectroscopic iron abundance analyses using archetypal metal-poor stars. We perform detailed 3D non-LTE radiative transfer calculations based on 3D hydrodynamic Stagger model atmospheres, and employ a new model atom that includes new quantum-mechanical neutral hydrogen collisional rate coefficients. With the exception of the red giant HD122563, we find that the 3D non-LTE models achieve Fe i/Fe ii excitation and ionization balance as well as not h"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1608.06390","kind":"arxiv","version":2},"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":"1608.06390","created_at":"2026-05-18T01:04:41.011142+00:00"},{"alias_kind":"arxiv_version","alias_value":"1608.06390v2","created_at":"2026-05-18T01:04:41.011142+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1608.06390","created_at":"2026-05-18T01:04:41.011142+00:00"},{"alias_kind":"pith_short_12","alias_value":"HPJL2CWTDXVF","created_at":"2026-05-18T12:30:19.053100+00:00"},{"alias_kind":"pith_short_16","alias_value":"HPJL2CWTDXVFWHTC","created_at":"2026-05-18T12:30:19.053100+00:00"},{"alias_kind":"pith_short_8","alias_value":"HPJL2CWT","created_at":"2026-05-18T12:30:19.053100+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.05154","citing_title":"Three Extremely Metal-Poor stars: discovery of a new CEMP-no star","ref_index":224,"is_internal_anchor":true},{"citing_arxiv_id":"2605.11074","citing_title":"Observational Signatures and Constraints on the Intermediate Neutron-Capture Process. The Case of the CEMP star TYC 6044-714-1 (RAVE J094921.8-161722)","ref_index":155,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS","json":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS.json","graph_json":"https://pith.science/api/pith-number/HPJL2CWTDXVFWHTCUF6KFJ4YYS/graph.json","events_json":"https://pith.science/api/pith-number/HPJL2CWTDXVFWHTCUF6KFJ4YYS/events.json","paper":"https://pith.science/paper/HPJL2CWT"},"agent_actions":{"view_html":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS","download_json":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS.json","view_paper":"https://pith.science/paper/HPJL2CWT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1608.06390&json=true","fetch_graph":"https://pith.science/api/pith-number/HPJL2CWTDXVFWHTCUF6KFJ4YYS/graph.json","fetch_events":"https://pith.science/api/pith-number/HPJL2CWTDXVFWHTCUF6KFJ4YYS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS/action/storage_attestation","attest_author":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS/action/author_attestation","sign_citation":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS/action/citation_signature","submit_replication":"https://pith.science/pith/HPJL2CWTDXVFWHTCUF6KFJ4YYS/action/replication_record"}},"created_at":"2026-05-18T01:04:41.011142+00:00","updated_at":"2026-05-18T01:04:41.011142+00:00"}