{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:2FNU25BR32A2HONQWOAZR5YIRL","short_pith_number":"pith:2FNU25BR","schema_version":"1.0","canonical_sha256":"d15b4d7431de81a3b9b0b38198f7088ac138c65d7cfb492746ebdfa0b5a69b99","source":{"kind":"arxiv","id":"1404.0005","version":1},"attestation_state":"computed","paper":{"title":"Water Clouds in Y Dwarfs and Exoplanets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Caroline V. Morley, Didier Saumon, Jonathan J. Fortney, Katharina Lodders, Mark S. Marley, Roxana Lupu, Tom Greene","submitted_at":"2014-03-31T20:00:04Z","abstract_excerpt":"The formation of clouds affects brown dwarf and planetary atmospheres of nearly all effective temperatures. Iron and silicate condense in L dwarf atmospheres and dissipate at the L/T transition. Minor species such as sulfides and salts condense in mid-late T dwarfs. For brown dwarfs below Teff=450 K, water condenses in the upper atmosphere to form ice clouds. Currently over a dozen objects in this temperature range have been discovered, and few previous theoretical studies have addressed the effect of water clouds on brown dwarf or exoplanetary spectra. Here we present a new grid of models tha"},"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":"1404.0005","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-03-31T20:00:04Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"7f37b9f41f6966e6fcc5451c784dd52462ca61afaae35aa538989ac9afa2cb8f","abstract_canon_sha256":"2189148fbf723b76af0fc947d4f2e487b1eaaa911358b392eea94f4d968bf9b1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:43:43.662582Z","signature_b64":"pmWz5LQ8zVhRFHgDlQJkp5xuyNn4y76k3YOTfporpBtqEBEsp4DvzDaCnUZ20/1VnK/GC2WGq9stlVjX4d+oBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d15b4d7431de81a3b9b0b38198f7088ac138c65d7cfb492746ebdfa0b5a69b99","last_reissued_at":"2026-05-18T01:43:43.662155Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:43:43.662155Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Water Clouds in Y Dwarfs and Exoplanets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Caroline V. Morley, Didier Saumon, Jonathan J. Fortney, Katharina Lodders, Mark S. Marley, Roxana Lupu, Tom Greene","submitted_at":"2014-03-31T20:00:04Z","abstract_excerpt":"The formation of clouds affects brown dwarf and planetary atmospheres of nearly all effective temperatures. Iron and silicate condense in L dwarf atmospheres and dissipate at the L/T transition. Minor species such as sulfides and salts condense in mid-late T dwarfs. For brown dwarfs below Teff=450 K, water condenses in the upper atmosphere to form ice clouds. Currently over a dozen objects in this temperature range have been discovered, and few previous theoretical studies have addressed the effect of water clouds on brown dwarf or exoplanetary spectra. Here we present a new grid of models tha"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1404.0005","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":""},"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":"1404.0005","created_at":"2026-05-18T01:43:43.662209+00:00"},{"alias_kind":"arxiv_version","alias_value":"1404.0005v1","created_at":"2026-05-18T01:43:43.662209+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1404.0005","created_at":"2026-05-18T01:43:43.662209+00:00"},{"alias_kind":"pith_short_12","alias_value":"2FNU25BR32A2","created_at":"2026-05-18T12:28:09.283467+00:00"},{"alias_kind":"pith_short_16","alias_value":"2FNU25BR32A2HONQ","created_at":"2026-05-18T12:28:09.283467+00:00"},{"alias_kind":"pith_short_8","alias_value":"2FNU25BR","created_at":"2026-05-18T12:28:09.283467+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.23814","citing_title":"Integral field spectroscopy with no IFUs: combining wide-field rotational slitless spectroscopy with tomographic reconstruction","ref_index":96,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL","json":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL.json","graph_json":"https://pith.science/api/pith-number/2FNU25BR32A2HONQWOAZR5YIRL/graph.json","events_json":"https://pith.science/api/pith-number/2FNU25BR32A2HONQWOAZR5YIRL/events.json","paper":"https://pith.science/paper/2FNU25BR"},"agent_actions":{"view_html":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL","download_json":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL.json","view_paper":"https://pith.science/paper/2FNU25BR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1404.0005&json=true","fetch_graph":"https://pith.science/api/pith-number/2FNU25BR32A2HONQWOAZR5YIRL/graph.json","fetch_events":"https://pith.science/api/pith-number/2FNU25BR32A2HONQWOAZR5YIRL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL/action/storage_attestation","attest_author":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL/action/author_attestation","sign_citation":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL/action/citation_signature","submit_replication":"https://pith.science/pith/2FNU25BR32A2HONQWOAZR5YIRL/action/replication_record"}},"created_at":"2026-05-18T01:43:43.662209+00:00","updated_at":"2026-05-18T01:43:43.662209+00:00"}