{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:BS3EVKWKX4OSTOUN5PJJ4KPB4Q","short_pith_number":"pith:BS3EVKWK","schema_version":"1.0","canonical_sha256":"0cb64aaacabf1d29ba8debd29e29e1e412334ea4f8f248da5af62790b484d10c","source":{"kind":"arxiv","id":"2010.14867","version":2},"attestation_state":"computed","paper":{"title":"HADES RV Programme with HARPS-N at TNG XII. The abundance signature of M dwarf stars with planets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"A. Bignamini, A. F. Lanza, A. Maggio, A. Petralia, A. Sozzetti, A. Su\\'arez-Mascare\\~no, B. Toledo-Padr\\'on, C. Di Maio, D. Locci, E. Covino, E. Herrero, E. Molinari, E. Poretti, G. Micela, G. Piotto, G. Scandariato, I. Pagano, I. Ribas, J. C. Morales, J. I. Gonz\\'alez Hern\\'andez, J. Maldonado, K. Biazzo, L. Affer, M. Baratella, M. Perger, M. Pinamonti, R. Claudi, R. Rebolo, S. Desidera, V. D'Orazi","submitted_at":"2020-10-28T10:25:29Z","abstract_excerpt":"Most of our current knowledge on planet formation is still based on the analysis of main-sequence, solar-type stars. Conversely, detailed chemical studies of large samples of M-dwarf planet hosts are still missing. We develop for the first time a methodology to determine stellar abundances of elements others than iron for M dwarf stars from high-resolution, optical spectra. Our methodology is based on the use of principal component analysis and sparse Bayesian's methods. We made use of a set of M dwarfs orbiting around an FGK primary with known abundances to train our methods. We applied our m"},"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":"2010.14867","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2020-10-28T10:25:29Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"435a3e9aa769e8166b2128c86249c0e7685afc39c5c71ef7531259fd7d759d9b","abstract_canon_sha256":"49d1f9a942bcc60a2641a434c8363f4a334f2d06ecc83d2ac583b8bb7ef80383"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:03:51.545170Z","signature_b64":"o2G5/9DF5prhVrTGChZ4w27rBTN5c4AcfIC5nshqvohSlKZHwcPKHGZSseNf200Yx6jc79z7zHfouY4fOctfCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0cb64aaacabf1d29ba8debd29e29e1e412334ea4f8f248da5af62790b484d10c","last_reissued_at":"2026-07-05T02:03:51.544708Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:03:51.544708Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"HADES RV Programme with HARPS-N at TNG XII. The abundance signature of M dwarf stars with planets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"A. Bignamini, A. F. Lanza, A. Maggio, A. Petralia, A. Sozzetti, A. Su\\'arez-Mascare\\~no, B. Toledo-Padr\\'on, C. Di Maio, D. Locci, E. Covino, E. Herrero, E. Molinari, E. Poretti, G. Micela, G. Piotto, G. Scandariato, I. Pagano, I. Ribas, J. C. Morales, J. I. Gonz\\'alez Hern\\'andez, J. Maldonado, K. Biazzo, L. Affer, M. Baratella, M. Perger, M. Pinamonti, R. Claudi, R. Rebolo, S. Desidera, V. D'Orazi","submitted_at":"2020-10-28T10:25:29Z","abstract_excerpt":"Most of our current knowledge on planet formation is still based on the analysis of main-sequence, solar-type stars. Conversely, detailed chemical studies of large samples of M-dwarf planet hosts are still missing. We develop for the first time a methodology to determine stellar abundances of elements others than iron for M dwarf stars from high-resolution, optical spectra. Our methodology is based on the use of principal component analysis and sparse Bayesian's methods. We made use of a set of M dwarfs orbiting around an FGK primary with known abundances to train our methods. We applied our m"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2010.14867","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2010.14867/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":"2010.14867","created_at":"2026-07-05T02:03:51.544766+00:00"},{"alias_kind":"arxiv_version","alias_value":"2010.14867v2","created_at":"2026-07-05T02:03:51.544766+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2010.14867","created_at":"2026-07-05T02:03:51.544766+00:00"},{"alias_kind":"pith_short_12","alias_value":"BS3EVKWKX4OS","created_at":"2026-07-05T02:03:51.544766+00:00"},{"alias_kind":"pith_short_16","alias_value":"BS3EVKWKX4OSTOUN","created_at":"2026-07-05T02:03:51.544766+00:00"},{"alias_kind":"pith_short_8","alias_value":"BS3EVKWK","created_at":"2026-07-05T02:03:51.544766+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.11674","citing_title":"Unstable magnetospheric accretion on the T Tauri star TW Hya","ref_index":229,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q","json":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q.json","graph_json":"https://pith.science/api/pith-number/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/graph.json","events_json":"https://pith.science/api/pith-number/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/events.json","paper":"https://pith.science/paper/BS3EVKWK"},"agent_actions":{"view_html":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q","download_json":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q.json","view_paper":"https://pith.science/paper/BS3EVKWK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2010.14867&json=true","fetch_graph":"https://pith.science/api/pith-number/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/graph.json","fetch_events":"https://pith.science/api/pith-number/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/action/storage_attestation","attest_author":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/action/author_attestation","sign_citation":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/action/citation_signature","submit_replication":"https://pith.science/pith/BS3EVKWKX4OSTOUN5PJJ4KPB4Q/action/replication_record"}},"created_at":"2026-07-05T02:03:51.544766+00:00","updated_at":"2026-07-05T02:03:51.544766+00:00"}