{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:TEJXFOKBS7L4KBDDBQXSRXJYVD","short_pith_number":"pith:TEJXFOKB","schema_version":"1.0","canonical_sha256":"991372b94197d7c504630c2f28dd38a8e2973717c93f5b02b351d72bb0b424f7","source":{"kind":"arxiv","id":"1902.09558","version":2},"attestation_state":"computed","paper":{"title":"Modern stellar spectroscopy caveats","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.SR","authors_text":"Sergi Blanco-Cuaresma","submitted_at":"2019-02-25T19:00:04Z","abstract_excerpt":"Multiple codes are available to derive atmospheric parameters and individual chemical abundances from high-resolution spectra of AFGKM stars. Almost all spectroscopists have their own preferences regarding which code and method to use. But the intrinsic differences between codes and methods lead to complex systematics that depend on multiple variables such as the selected spectral regions and the radiative transfer code used. I expand iSpec, a popular open-source spectroscopic tool, to support the most well-known radiative transfer codes and assess their similarities and biases when using mult"},"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":"1902.09558","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2019-02-25T19:00:04Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"226046020b3cf4d678058be558188c5e97893aac72d9ef3a798811791dee614f","abstract_canon_sha256":"b9d73523f419d3a0e2514bfe2fa42de29128aa72ad316c56010850f4711ba6d8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:47:57.992129Z","signature_b64":"AhpWayhj7LyBvcIvSoBqqZnyjI60ZC8c6kcdE0pQGIFFzw9292G9K/JppIVkbGE72HK44X8iD8PFKqN61xCoBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"991372b94197d7c504630c2f28dd38a8e2973717c93f5b02b351d72bb0b424f7","last_reissued_at":"2026-05-17T23:47:57.991724Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:47:57.991724Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Modern stellar spectroscopy caveats","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.SR","authors_text":"Sergi Blanco-Cuaresma","submitted_at":"2019-02-25T19:00:04Z","abstract_excerpt":"Multiple codes are available to derive atmospheric parameters and individual chemical abundances from high-resolution spectra of AFGKM stars. Almost all spectroscopists have their own preferences regarding which code and method to use. But the intrinsic differences between codes and methods lead to complex systematics that depend on multiple variables such as the selected spectral regions and the radiative transfer code used. I expand iSpec, a popular open-source spectroscopic tool, to support the most well-known radiative transfer codes and assess their similarities and biases when using mult"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1902.09558","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":"1902.09558","created_at":"2026-05-17T23:47:57.991780+00:00"},{"alias_kind":"arxiv_version","alias_value":"1902.09558v2","created_at":"2026-05-17T23:47:57.991780+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1902.09558","created_at":"2026-05-17T23:47:57.991780+00:00"},{"alias_kind":"pith_short_12","alias_value":"TEJXFOKBS7L4","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_16","alias_value":"TEJXFOKBS7L4KBDD","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_8","alias_value":"TEJXFOKB","created_at":"2026-05-18T12:33:27.125529+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.21808","citing_title":"On the stellar parameter dependence of the combined Fe I and Fe II chromospheric emission-line in the wings of the Ca II K line","ref_index":53,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17005","citing_title":"Red novae, their progenitors, and remnants","ref_index":193,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD","json":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD.json","graph_json":"https://pith.science/api/pith-number/TEJXFOKBS7L4KBDDBQXSRXJYVD/graph.json","events_json":"https://pith.science/api/pith-number/TEJXFOKBS7L4KBDDBQXSRXJYVD/events.json","paper":"https://pith.science/paper/TEJXFOKB"},"agent_actions":{"view_html":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD","download_json":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD.json","view_paper":"https://pith.science/paper/TEJXFOKB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1902.09558&json=true","fetch_graph":"https://pith.science/api/pith-number/TEJXFOKBS7L4KBDDBQXSRXJYVD/graph.json","fetch_events":"https://pith.science/api/pith-number/TEJXFOKBS7L4KBDDBQXSRXJYVD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD/action/storage_attestation","attest_author":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD/action/author_attestation","sign_citation":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD/action/citation_signature","submit_replication":"https://pith.science/pith/TEJXFOKBS7L4KBDDBQXSRXJYVD/action/replication_record"}},"created_at":"2026-05-17T23:47:57.991780+00:00","updated_at":"2026-05-17T23:47:57.991780+00:00"}