{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:2PBKXEBMPAGHP4O2MTZPA7COEC","short_pith_number":"pith:2PBKXEBM","schema_version":"1.0","canonical_sha256":"d3c2ab902c780c77f1da64f2f07c4e209384673a5ae52867555c81ea481a302b","source":{"kind":"arxiv","id":"2303.08927","version":1},"attestation_state":"computed","paper":{"title":"Azimuthal C/O Variations in a Planet-Forming Disk","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"Alice S. Booth, Catherine Walsh, Edwin A. Bergin, Ewine F. van Dishoeck, Jonathan Rawlings, Kenji Furuya, L. Ilsedore Cleeves, Luke Keyte, Maria N. Drozdovskaya, Mihkel Kama, Oliver Shorttle","submitted_at":"2023-03-15T20:49:29Z","abstract_excerpt":"The elemental carbon-to-oxygen ratio (C/O) in the atmosphere of a giant planet is a promising diagnostic of that planet's formation history in a protoplanetary disk. Alongside efforts in the exoplanet community to measure C/O in planetary atmospheres, observational and theoretical studies of disks are increasingly focused on understanding how the gas-phase C/O varies both with radial location and between disks. This is mostly tied to the icelines of major volatile carriers such as CO and H2O. Using ALMA observations of CS and SO, we have unearthed evidence for an entirely novel type of C/O var"},"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":"2303.08927","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.EP","submitted_at":"2023-03-15T20:49:29Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"5c695657b345a5d7d291967a3043d819280dce98176ca4737fbedc730521a128","abstract_canon_sha256":"022e94f0d8ba2d65ffa75b11090409fd6abfd001bdc56c67fee04224792f7ec1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:51:46.906364Z","signature_b64":"eZtDdSz0bu+1o4xp3vG1YZFbtyr26oaampEcsdG6EHtf1Ljldol47HU9MVwXiLZkzQkfVJbUd9ECgUpPOfjzAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d3c2ab902c780c77f1da64f2f07c4e209384673a5ae52867555c81ea481a302b","last_reissued_at":"2026-07-05T05:51:46.905855Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:51:46.905855Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Azimuthal C/O Variations in a Planet-Forming Disk","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"Alice S. Booth, Catherine Walsh, Edwin A. Bergin, Ewine F. van Dishoeck, Jonathan Rawlings, Kenji Furuya, L. Ilsedore Cleeves, Luke Keyte, Maria N. Drozdovskaya, Mihkel Kama, Oliver Shorttle","submitted_at":"2023-03-15T20:49:29Z","abstract_excerpt":"The elemental carbon-to-oxygen ratio (C/O) in the atmosphere of a giant planet is a promising diagnostic of that planet's formation history in a protoplanetary disk. Alongside efforts in the exoplanet community to measure C/O in planetary atmospheres, observational and theoretical studies of disks are increasingly focused on understanding how the gas-phase C/O varies both with radial location and between disks. This is mostly tied to the icelines of major volatile carriers such as CO and H2O. Using ALMA observations of CS and SO, we have unearthed evidence for an entirely novel type of C/O var"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2303.08927","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/2303.08927/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":"2303.08927","created_at":"2026-07-05T05:51:46.905915+00:00"},{"alias_kind":"arxiv_version","alias_value":"2303.08927v1","created_at":"2026-07-05T05:51:46.905915+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2303.08927","created_at":"2026-07-05T05:51:46.905915+00:00"},{"alias_kind":"pith_short_12","alias_value":"2PBKXEBMPAGH","created_at":"2026-07-05T05:51:46.905915+00:00"},{"alias_kind":"pith_short_16","alias_value":"2PBKXEBMPAGHP4O2","created_at":"2026-07-05T05:51:46.905915+00:00"},{"alias_kind":"pith_short_8","alias_value":"2PBKXEBM","created_at":"2026-07-05T05:51:46.905915+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.18062","citing_title":"Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties","ref_index":60,"is_internal_anchor":false},{"citing_arxiv_id":"2605.18062","citing_title":"Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties","ref_index":60,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC","json":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC.json","graph_json":"https://pith.science/api/pith-number/2PBKXEBMPAGHP4O2MTZPA7COEC/graph.json","events_json":"https://pith.science/api/pith-number/2PBKXEBMPAGHP4O2MTZPA7COEC/events.json","paper":"https://pith.science/paper/2PBKXEBM"},"agent_actions":{"view_html":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC","download_json":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC.json","view_paper":"https://pith.science/paper/2PBKXEBM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2303.08927&json=true","fetch_graph":"https://pith.science/api/pith-number/2PBKXEBMPAGHP4O2MTZPA7COEC/graph.json","fetch_events":"https://pith.science/api/pith-number/2PBKXEBMPAGHP4O2MTZPA7COEC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC/action/storage_attestation","attest_author":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC/action/author_attestation","sign_citation":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC/action/citation_signature","submit_replication":"https://pith.science/pith/2PBKXEBMPAGHP4O2MTZPA7COEC/action/replication_record"}},"created_at":"2026-07-05T05:51:46.905915+00:00","updated_at":"2026-07-05T05:51:46.905915+00:00"}