{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:J3GQLTZTJOPTWOKTBI63EHHQSC","short_pith_number":"pith:J3GQLTZT","schema_version":"1.0","canonical_sha256":"4ecd05cf334b9f3b39530a3db21cf090896e204ca09865faf65d7990dc8c84ca","source":{"kind":"arxiv","id":"2303.16295","version":1},"attestation_state":"computed","paper":{"title":"Self-consistent Models of Y Dwarf Atmospheres with Water Clouds and Disequilibrium Chemistry","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"Adam Burrows, Brianna Lacy","submitted_at":"2023-03-28T20:18:57Z","abstract_excerpt":"Y dwarfs are the coolest spectral class of brown dwarf. They have effective temperatures less than 500 K, with the coolest detection as low as ~250 K. Their spectra are shaped predominantly by gaseous water, methane, and ammonia. At the warmer end of the Y dwarf temperature range, spectral signatures of disequilibrium carbon monoxide have been observed. Cooler Y dwarfs could host water clouds in their atmospheres. Since they make up the low-mass tail of the star formation process, and are a valuable analogue to the atmospheres of giant gaseous exoplanets in a temperature range that is difficul"},"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":"2303.16295","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.EP","submitted_at":"2023-03-28T20:18:57Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"44896ae9af8ada5eeb2169679dff0142d481045d70c7530a68744d92488d04e9","abstract_canon_sha256":"fe2969c2b02dd79eee03edc9b44ae9d8763e2fed2ce6bee4c87411c8712e3a17"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:20:27.656525Z","signature_b64":"ppqXiNzJdaa+tjBmI0G3XagOgo7vsQMmI4XTDXWrXQJcRidvOkrdrwKjRyH/XyhUfqZk+68dNQXxiiOE6xFcDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4ecd05cf334b9f3b39530a3db21cf090896e204ca09865faf65d7990dc8c84ca","last_reissued_at":"2026-07-05T06:20:27.656024Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:20:27.656024Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Self-consistent Models of Y Dwarf Atmospheres with Water Clouds and Disequilibrium Chemistry","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"Adam Burrows, Brianna Lacy","submitted_at":"2023-03-28T20:18:57Z","abstract_excerpt":"Y dwarfs are the coolest spectral class of brown dwarf. They have effective temperatures less than 500 K, with the coolest detection as low as ~250 K. Their spectra are shaped predominantly by gaseous water, methane, and ammonia. At the warmer end of the Y dwarf temperature range, spectral signatures of disequilibrium carbon monoxide have been observed. Cooler Y dwarfs could host water clouds in their atmospheres. Since they make up the low-mass tail of the star formation process, and are a valuable analogue to the atmospheres of giant gaseous exoplanets in a temperature range that is difficul"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2303.16295","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/2303.16295/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":"2303.16295","created_at":"2026-07-05T06:20:27.656081+00:00"},{"alias_kind":"arxiv_version","alias_value":"2303.16295v1","created_at":"2026-07-05T06:20:27.656081+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2303.16295","created_at":"2026-07-05T06:20:27.656081+00:00"},{"alias_kind":"pith_short_12","alias_value":"J3GQLTZTJOPT","created_at":"2026-07-05T06:20:27.656081+00:00"},{"alias_kind":"pith_short_16","alias_value":"J3GQLTZTJOPTWOKT","created_at":"2026-07-05T06:20:27.656081+00:00"},{"alias_kind":"pith_short_8","alias_value":"J3GQLTZT","created_at":"2026-07-05T06:20:27.656081+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.14026","citing_title":"Next-Generation Atmosphere Models for Giant Planets with Application to Coupled Interior Composition and Spectral Evolution I: Cloudless Models with Equilibrium Chemistry","ref_index":36,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC","json":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC.json","graph_json":"https://pith.science/api/pith-number/J3GQLTZTJOPTWOKTBI63EHHQSC/graph.json","events_json":"https://pith.science/api/pith-number/J3GQLTZTJOPTWOKTBI63EHHQSC/events.json","paper":"https://pith.science/paper/J3GQLTZT"},"agent_actions":{"view_html":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC","download_json":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC.json","view_paper":"https://pith.science/paper/J3GQLTZT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2303.16295&json=true","fetch_graph":"https://pith.science/api/pith-number/J3GQLTZTJOPTWOKTBI63EHHQSC/graph.json","fetch_events":"https://pith.science/api/pith-number/J3GQLTZTJOPTWOKTBI63EHHQSC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC/action/storage_attestation","attest_author":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC/action/author_attestation","sign_citation":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC/action/citation_signature","submit_replication":"https://pith.science/pith/J3GQLTZTJOPTWOKTBI63EHHQSC/action/replication_record"}},"created_at":"2026-07-05T06:20:27.656081+00:00","updated_at":"2026-07-05T06:20:27.656081+00:00"}