{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:KB65NBWYX6AJCIDRY44AD45DSW","short_pith_number":"pith:KB65NBWY","schema_version":"1.0","canonical_sha256":"507dd686d8bf80912071c73801f3a395b74071a255c032a7b2552d9c0a762f1b","source":{"kind":"arxiv","id":"1110.2694","version":2},"attestation_state":"computed","paper":{"title":"Metallicity of M dwarfs II. A comparative study of photometric metallicity scales","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"C. Nat\\'ario, C. S. Fernandes, F. Allard, N. C. Santos, S. Udry, T. Forveille, V. Neves, X. Bonfils, X. Delfosse","submitted_at":"2011-10-12T16:43:08Z","abstract_excerpt":"Stellar parameters are not easily derived from M dwarf spectra, which are dominated by complex bands of diatomic and triatomic molecules and not well described at the line by line level by atmospheric models. M dwarf metallicities are therefore most commonly derived through less direct techniques. Several recent publications propose calibrations that provide the metallicity of an M dwarf from its Ks band absolute magnitude and its V-Ks color, but disagree at the \\pm0.1 dex level. We compare these calibrations on a sample of 23 M dwarfs, which we select as wide (> 5 arcsec) companions of F-, G-"},"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":"1110.2694","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2011-10-12T16:43:08Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"9ec1788c2d69b42465f9dd8d8c2c0577e40dc21c69742144fd406430ae2c1cf3","abstract_canon_sha256":"502497eaf9c9ab2c6081ee2163dfa8a61089bea589b31c08566e8edd6898d636"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:00:13.136499Z","signature_b64":"weOqHczBt1Nkucsf10SyQ3r3meNVYN4u9FoHpkKdxzNuIXOmVQElilOXkfN2XzCCPT3S3CVgF56YlWQDmSOAAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"507dd686d8bf80912071c73801f3a395b74071a255c032a7b2552d9c0a762f1b","last_reissued_at":"2026-05-18T02:00:13.135950Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:00:13.135950Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Metallicity of M dwarfs II. A comparative study of photometric metallicity scales","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"C. Nat\\'ario, C. S. Fernandes, F. Allard, N. C. Santos, S. Udry, T. Forveille, V. Neves, X. Bonfils, X. Delfosse","submitted_at":"2011-10-12T16:43:08Z","abstract_excerpt":"Stellar parameters are not easily derived from M dwarf spectra, which are dominated by complex bands of diatomic and triatomic molecules and not well described at the line by line level by atmospheric models. M dwarf metallicities are therefore most commonly derived through less direct techniques. Several recent publications propose calibrations that provide the metallicity of an M dwarf from its Ks band absolute magnitude and its V-Ks color, but disagree at the \\pm0.1 dex level. We compare these calibrations on a sample of 23 M dwarfs, which we select as wide (> 5 arcsec) companions of F-, G-"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1110.2694","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":"1110.2694","created_at":"2026-05-18T02:00:13.136040+00:00"},{"alias_kind":"arxiv_version","alias_value":"1110.2694v2","created_at":"2026-05-18T02:00:13.136040+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1110.2694","created_at":"2026-05-18T02:00:13.136040+00:00"},{"alias_kind":"pith_short_12","alias_value":"KB65NBWYX6AJ","created_at":"2026-05-18T12:26:32.869790+00:00"},{"alias_kind":"pith_short_16","alias_value":"KB65NBWYX6AJCIDR","created_at":"2026-05-18T12:26:32.869790+00:00"},{"alias_kind":"pith_short_8","alias_value":"KB65NBWY","created_at":"2026-05-18T12:26:32.869790+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.18131","citing_title":"Inferring stellar metallicity and elemental abundances from kinematic and spectroscopic data using machine learning -- Implications for exoplanet host stars","ref_index":39,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW","json":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW.json","graph_json":"https://pith.science/api/pith-number/KB65NBWYX6AJCIDRY44AD45DSW/graph.json","events_json":"https://pith.science/api/pith-number/KB65NBWYX6AJCIDRY44AD45DSW/events.json","paper":"https://pith.science/paper/KB65NBWY"},"agent_actions":{"view_html":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW","download_json":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW.json","view_paper":"https://pith.science/paper/KB65NBWY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1110.2694&json=true","fetch_graph":"https://pith.science/api/pith-number/KB65NBWYX6AJCIDRY44AD45DSW/graph.json","fetch_events":"https://pith.science/api/pith-number/KB65NBWYX6AJCIDRY44AD45DSW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW/action/storage_attestation","attest_author":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW/action/author_attestation","sign_citation":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW/action/citation_signature","submit_replication":"https://pith.science/pith/KB65NBWYX6AJCIDRY44AD45DSW/action/replication_record"}},"created_at":"2026-05-18T02:00:13.136040+00:00","updated_at":"2026-05-18T02:00:13.136040+00:00"}