{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:3AEJ6CBGKIVE44ZX2C7NVD2R63","short_pith_number":"pith:3AEJ6CBG","schema_version":"1.0","canonical_sha256":"d8089f0826522a4e7337d0beda8f51f6d56257b790c0686ead2b74dff3cfe59b","source":{"kind":"arxiv","id":"2202.06301","version":1},"attestation_state":"computed","paper":{"title":"A new estimation of astrometric exoplanet detection limits in the habitable zone around nearby stars","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.IM","astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"Anne-Marie Lagrange, Nad\\`ege Meunier","submitted_at":"2022-02-13T12:50:37Z","abstract_excerpt":"Astrometry is less sensitive to stellar activity than the radial velocity technique when attempting to detect Earth mass planets in the habitable zone of solar-type stars. This is due to a smaller number of physical processes affecting the signal, and a larger ratio of the amplitude of the planetary signal to the stellar signal. A few high-precision astrometric missions have therefore been proposed over the past two decades. We aim to re-estimate the detection limits in astrometry for the nearby stars which are the main targets proposed for the THEIA astrometric mission, the most elaborate mis"},"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":"2202.06301","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.EP","submitted_at":"2022-02-13T12:50:37Z","cross_cats_sorted":["astro-ph.IM","astro-ph.SR"],"title_canon_sha256":"484cf4ff02859c0c9938374f79093ead40c301d2c17e12f1ee2aec87c5d76208","abstract_canon_sha256":"1a438c9676e8506c7d7d0257354e756120c755d4c8c8d0b4f6ad418849c3cca3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:09:48.209478Z","signature_b64":"G2RxAtdzg/Z5oAsQNo2utAamd0rotXlUyAfrIOpeIIdTeVnsAkVrK4h4Ym/xzjraWCrDeDP5S1Pr4NgQLYtRAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d8089f0826522a4e7337d0beda8f51f6d56257b790c0686ead2b74dff3cfe59b","last_reissued_at":"2026-07-05T04:09:48.208925Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:09:48.208925Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A new estimation of astrometric exoplanet detection limits in the habitable zone around nearby stars","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.IM","astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"Anne-Marie Lagrange, Nad\\`ege Meunier","submitted_at":"2022-02-13T12:50:37Z","abstract_excerpt":"Astrometry is less sensitive to stellar activity than the radial velocity technique when attempting to detect Earth mass planets in the habitable zone of solar-type stars. This is due to a smaller number of physical processes affecting the signal, and a larger ratio of the amplitude of the planetary signal to the stellar signal. A few high-precision astrometric missions have therefore been proposed over the past two decades. We aim to re-estimate the detection limits in astrometry for the nearby stars which are the main targets proposed for the THEIA astrometric mission, the most elaborate mis"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2202.06301","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2202.06301/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":"2202.06301","created_at":"2026-07-05T04:09:48.208995+00:00"},{"alias_kind":"arxiv_version","alias_value":"2202.06301v1","created_at":"2026-07-05T04:09:48.208995+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2202.06301","created_at":"2026-07-05T04:09:48.208995+00:00"},{"alias_kind":"pith_short_12","alias_value":"3AEJ6CBGKIVE","created_at":"2026-07-05T04:09:48.208995+00:00"},{"alias_kind":"pith_short_16","alias_value":"3AEJ6CBGKIVE44ZX","created_at":"2026-07-05T04:09:48.208995+00:00"},{"alias_kind":"pith_short_8","alias_value":"3AEJ6CBG","created_at":"2026-07-05T04:09:48.208995+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.18464","citing_title":"Modeling Doppler Shifts in Radial-Velocity Data with Deep Learning toward Earth-mass Exoplanet Detection","ref_index":263,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63","json":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63.json","graph_json":"https://pith.science/api/pith-number/3AEJ6CBGKIVE44ZX2C7NVD2R63/graph.json","events_json":"https://pith.science/api/pith-number/3AEJ6CBGKIVE44ZX2C7NVD2R63/events.json","paper":"https://pith.science/paper/3AEJ6CBG"},"agent_actions":{"view_html":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63","download_json":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63.json","view_paper":"https://pith.science/paper/3AEJ6CBG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2202.06301&json=true","fetch_graph":"https://pith.science/api/pith-number/3AEJ6CBGKIVE44ZX2C7NVD2R63/graph.json","fetch_events":"https://pith.science/api/pith-number/3AEJ6CBGKIVE44ZX2C7NVD2R63/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63/action/storage_attestation","attest_author":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63/action/author_attestation","sign_citation":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63/action/citation_signature","submit_replication":"https://pith.science/pith/3AEJ6CBGKIVE44ZX2C7NVD2R63/action/replication_record"}},"created_at":"2026-07-05T04:09:48.208995+00:00","updated_at":"2026-07-05T04:09:48.208995+00:00"}