{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:WNPTP2PRWUP7VLAFYTG4LTO5TN","short_pith_number":"pith:WNPTP2PR","schema_version":"1.0","canonical_sha256":"b35f37e9f1b51ffaac05c4cdc5cddd9b7f6bcc8341601b905ac0aa5224bbc063","source":{"kind":"arxiv","id":"2409.03852","version":2},"attestation_state":"computed","paper":{"title":"Searching for Additional Planets in TESS Multi-Planet Systems: Testing Empirical Models Based on Kepler Data","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.EP","authors_text":"Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Jamie Dietrich","submitted_at":"2024-09-05T18:29:00Z","abstract_excerpt":"Multi-planet system architectures are frequently used to constrain possible formation and evolutionary pathways of observed exoplanets. Therefore, understanding the predictive and descriptive power of empirical models of these systems is critical to understanding their formation histories. Additionally, if empirical models can reproduce architectures over a range of scales, transit and radial velocity observations can be more easily and effectively used to inform future microlensing, astrometric, and direct imaging surveys. We analyze 52 TESS multi-planet systems previously studied using Dynam"},"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":"2409.03852","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.EP","submitted_at":"2024-09-05T18:29:00Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"bc078abad2f66de99bd61c16ce8f322c997a81e5dde78cddaef5305e32c2b819","abstract_canon_sha256":"af5cae35422096694b77e64f6ef1d5eba6d3ff5484552468bc64e56f2cf6edc3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:49:34.860045Z","signature_b64":"Uv0j1u9VpVgK1THYFX6mYMqX/9kE1/k+AD90fgqrGTf0aELmHASowletH7fhhSSIynx0rqDRtZtYmJE0eJdxBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b35f37e9f1b51ffaac05c4cdc5cddd9b7f6bcc8341601b905ac0aa5224bbc063","last_reissued_at":"2026-07-05T10:49:34.859599Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:49:34.859599Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Searching for Additional Planets in TESS Multi-Planet Systems: Testing Empirical Models Based on Kepler Data","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.EP","authors_text":"Caleb K. Harada, Courtney D. Dressing, Emma V. Turtelboom, Jamie Dietrich","submitted_at":"2024-09-05T18:29:00Z","abstract_excerpt":"Multi-planet system architectures are frequently used to constrain possible formation and evolutionary pathways of observed exoplanets. Therefore, understanding the predictive and descriptive power of empirical models of these systems is critical to understanding their formation histories. Additionally, if empirical models can reproduce architectures over a range of scales, transit and radial velocity observations can be more easily and effectively used to inform future microlensing, astrometric, and direct imaging surveys. We analyze 52 TESS multi-planet systems previously studied using Dynam"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2409.03852","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/2409.03852/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":"2409.03852","created_at":"2026-07-05T10:49:34.859658+00:00"},{"alias_kind":"arxiv_version","alias_value":"2409.03852v2","created_at":"2026-07-05T10:49:34.859658+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2409.03852","created_at":"2026-07-05T10:49:34.859658+00:00"},{"alias_kind":"pith_short_12","alias_value":"WNPTP2PRWUP7","created_at":"2026-07-05T10:49:34.859658+00:00"},{"alias_kind":"pith_short_16","alias_value":"WNPTP2PRWUP7VLAF","created_at":"2026-07-05T10:49:34.859658+00:00"},{"alias_kind":"pith_short_8","alias_value":"WNPTP2PR","created_at":"2026-07-05T10:49:34.859658+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.06413","citing_title":"Confirmation of a non-transiting planet in the habitable zone of the nearby M dwarf L 98-59","ref_index":139,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN","json":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN.json","graph_json":"https://pith.science/api/pith-number/WNPTP2PRWUP7VLAFYTG4LTO5TN/graph.json","events_json":"https://pith.science/api/pith-number/WNPTP2PRWUP7VLAFYTG4LTO5TN/events.json","paper":"https://pith.science/paper/WNPTP2PR"},"agent_actions":{"view_html":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN","download_json":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN.json","view_paper":"https://pith.science/paper/WNPTP2PR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2409.03852&json=true","fetch_graph":"https://pith.science/api/pith-number/WNPTP2PRWUP7VLAFYTG4LTO5TN/graph.json","fetch_events":"https://pith.science/api/pith-number/WNPTP2PRWUP7VLAFYTG4LTO5TN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN/action/storage_attestation","attest_author":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN/action/author_attestation","sign_citation":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN/action/citation_signature","submit_replication":"https://pith.science/pith/WNPTP2PRWUP7VLAFYTG4LTO5TN/action/replication_record"}},"created_at":"2026-07-05T10:49:34.859658+00:00","updated_at":"2026-07-05T10:49:34.859658+00:00"}