{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:35XAQ4I4QJ56EGJGZFN6YPFXZO","short_pith_number":"pith:35XAQ4I4","schema_version":"1.0","canonical_sha256":"df6e08711c827be21926c95bec3cb7cba1907f335778c9aeed08adb94afb6aa7","source":{"kind":"arxiv","id":"1101.3426","version":1},"attestation_state":"computed","paper":{"title":"Microturbulent velocity from stellar spectra: a comparison between different approaches (Research Note)","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Alessio Mucciarelli (Astronomy Department, Bologna University, Italy)","submitted_at":"2011-01-18T11:48:55Z","abstract_excerpt":"Context --- The classical method to infer microturbulent velocity in stellar spectra requires that the abundances of the iron lines are not correlated with the observed equivalent widths. An alternative method, requiring the use of the expected line strength, is often used to by-pass the risk of spurious slopes due to the correlation between the errors in abundance and equivalent width. Aims --- To compare the two methods and identify pros and cons and applicability to the typical practical cases. Methods --- I performed a test with a grid of synthetic spectra, including instrumental broadenin"},"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":"1101.3426","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2011-01-18T11:48:55Z","cross_cats_sorted":[],"title_canon_sha256":"c9ac8a5b7149b8a58386287e5de3731fe9d20946c87a2f3d757cb0bb2eb9cec6","abstract_canon_sha256":"dd5d56470cddd72a7658a386755ab48234c9360d4cd40c4f94df4de908617f9b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:03:26.880614Z","signature_b64":"l69O0ALCdBK5CRo81UHYDkFGcgQTbXCLB48ZIo0rlm892r+XHygTaDqe8pYw8pVZ44MCJKTNBv3r6L/lKJ8eAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"df6e08711c827be21926c95bec3cb7cba1907f335778c9aeed08adb94afb6aa7","last_reissued_at":"2026-05-18T02:03:26.880088Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:03:26.880088Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Microturbulent velocity from stellar spectra: a comparison between different approaches (Research Note)","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Alessio Mucciarelli (Astronomy Department, Bologna University, Italy)","submitted_at":"2011-01-18T11:48:55Z","abstract_excerpt":"Context --- The classical method to infer microturbulent velocity in stellar spectra requires that the abundances of the iron lines are not correlated with the observed equivalent widths. An alternative method, requiring the use of the expected line strength, is often used to by-pass the risk of spurious slopes due to the correlation between the errors in abundance and equivalent width. Aims --- To compare the two methods and identify pros and cons and applicability to the typical practical cases. Methods --- I performed a test with a grid of synthetic spectra, including instrumental broadenin"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1101.3426","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":"1101.3426","created_at":"2026-05-18T02:03:26.880170+00:00"},{"alias_kind":"arxiv_version","alias_value":"1101.3426v1","created_at":"2026-05-18T02:03:26.880170+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1101.3426","created_at":"2026-05-18T02:03:26.880170+00:00"},{"alias_kind":"pith_short_12","alias_value":"35XAQ4I4QJ56","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_16","alias_value":"35XAQ4I4QJ56EGJG","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_8","alias_value":"35XAQ4I4","created_at":"2026-05-18T12:26:18.847500+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"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":64,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO","json":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO.json","graph_json":"https://pith.science/api/pith-number/35XAQ4I4QJ56EGJGZFN6YPFXZO/graph.json","events_json":"https://pith.science/api/pith-number/35XAQ4I4QJ56EGJGZFN6YPFXZO/events.json","paper":"https://pith.science/paper/35XAQ4I4"},"agent_actions":{"view_html":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO","download_json":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO.json","view_paper":"https://pith.science/paper/35XAQ4I4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1101.3426&json=true","fetch_graph":"https://pith.science/api/pith-number/35XAQ4I4QJ56EGJGZFN6YPFXZO/graph.json","fetch_events":"https://pith.science/api/pith-number/35XAQ4I4QJ56EGJGZFN6YPFXZO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO/action/storage_attestation","attest_author":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO/action/author_attestation","sign_citation":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO/action/citation_signature","submit_replication":"https://pith.science/pith/35XAQ4I4QJ56EGJGZFN6YPFXZO/action/replication_record"}},"created_at":"2026-05-18T02:03:26.880170+00:00","updated_at":"2026-05-18T02:03:26.880170+00:00"}