{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:Z6RCSCAB7WKI74CMEDQIUUGXRN","short_pith_number":"pith:Z6RCSCAB","schema_version":"1.0","canonical_sha256":"cfa2290801fd948ff04c20e08a50d78b7c71fa61494cec81431be44c1ea93bbe","source":{"kind":"arxiv","id":"2407.08518","version":2},"attestation_state":"computed","paper":{"title":"Precise Bolometric Luminosities and Effective Temperatures of 23 late-T and Y dwarfs Obtained with JWST","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Adam C. Schneider, Federico Marocco, J. Davy Kirkpatrick, Mark S. Marley, Michael C. Cushing, Richard L. Smart, Sagnick Mukherjee, Samuel A. Beiler","submitted_at":"2024-07-11T14:05:32Z","abstract_excerpt":"We present infrared spectral energy distributions of 23 late-type T and Y dwarfs obtained with the James Webb Space Telescope. The spectral energy distributions consist of NIRSpec PRISM and MIRI LRS spectra covering the $\\sim$1--12 $\\mu$m wavelength range at $\\lambda/ \\Delta \\lambda \\approx 100$ and broadband photometry at 15, 18, and 21 $\\mu$m. The spectra exhibit absorption features common to these objects including H$_2$O, CH$_4$, CO, CO$_2$, and NH$_3$. Interestingly, while the spectral morphology changes relatively smoothly with spectral type at $\\lambda < 3$ $\\mu$m and $\\lambda > 8$ $\\mu"},"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":"2407.08518","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2024-07-11T14:05:32Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"997a7b8d8495325b41fadabb2bd986a1097114803ba58efe3fdf1648fbc3554f","abstract_canon_sha256":"350dbf4a0dd29ebc68edf54b2c5c54031e4625a75638e9e3a0a751aad1996c40"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:45:52.474953Z","signature_b64":"JyPreQCnHTUu/SkvvfJ4bI74Z/7RahQwoud6xgsyHjE3LlK1Tft1gZ3buK1kMpvyPqOteoCXherPYdHprjnnCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cfa2290801fd948ff04c20e08a50d78b7c71fa61494cec81431be44c1ea93bbe","last_reissued_at":"2026-07-05T08:45:52.474544Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:45:52.474544Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Precise Bolometric Luminosities and Effective Temperatures of 23 late-T and Y dwarfs Obtained with JWST","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Adam C. Schneider, Federico Marocco, J. Davy Kirkpatrick, Mark S. Marley, Michael C. Cushing, Richard L. Smart, Sagnick Mukherjee, Samuel A. Beiler","submitted_at":"2024-07-11T14:05:32Z","abstract_excerpt":"We present infrared spectral energy distributions of 23 late-type T and Y dwarfs obtained with the James Webb Space Telescope. The spectral energy distributions consist of NIRSpec PRISM and MIRI LRS spectra covering the $\\sim$1--12 $\\mu$m wavelength range at $\\lambda/ \\Delta \\lambda \\approx 100$ and broadband photometry at 15, 18, and 21 $\\mu$m. The spectra exhibit absorption features common to these objects including H$_2$O, CH$_4$, CO, CO$_2$, and NH$_3$. Interestingly, while the spectral morphology changes relatively smoothly with spectral type at $\\lambda < 3$ $\\mu$m and $\\lambda > 8$ $\\mu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2407.08518","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/2407.08518/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":"2407.08518","created_at":"2026-07-05T08:45:52.474601+00:00"},{"alias_kind":"arxiv_version","alias_value":"2407.08518v2","created_at":"2026-07-05T08:45:52.474601+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2407.08518","created_at":"2026-07-05T08:45:52.474601+00:00"},{"alias_kind":"pith_short_12","alias_value":"Z6RCSCAB7WKI","created_at":"2026-07-05T08:45:52.474601+00:00"},{"alias_kind":"pith_short_16","alias_value":"Z6RCSCAB7WKI74CM","created_at":"2026-07-05T08:45:52.474601+00:00"},{"alias_kind":"pith_short_8","alias_value":"Z6RCSCAB","created_at":"2026-07-05T08:45:52.474601+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.07461","citing_title":"A clear detection of proper motion confirms that the claimed $\\mathbf{z\\simeq32}$ galaxy candidate, \"Capotauro'', is a Y-type brown dwarf","ref_index":117,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN","json":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN.json","graph_json":"https://pith.science/api/pith-number/Z6RCSCAB7WKI74CMEDQIUUGXRN/graph.json","events_json":"https://pith.science/api/pith-number/Z6RCSCAB7WKI74CMEDQIUUGXRN/events.json","paper":"https://pith.science/paper/Z6RCSCAB"},"agent_actions":{"view_html":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN","download_json":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN.json","view_paper":"https://pith.science/paper/Z6RCSCAB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2407.08518&json=true","fetch_graph":"https://pith.science/api/pith-number/Z6RCSCAB7WKI74CMEDQIUUGXRN/graph.json","fetch_events":"https://pith.science/api/pith-number/Z6RCSCAB7WKI74CMEDQIUUGXRN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN/action/storage_attestation","attest_author":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN/action/author_attestation","sign_citation":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN/action/citation_signature","submit_replication":"https://pith.science/pith/Z6RCSCAB7WKI74CMEDQIUUGXRN/action/replication_record"}},"created_at":"2026-07-05T08:45:52.474601+00:00","updated_at":"2026-07-05T08:45:52.474601+00:00"}