{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:MSDO6FPKBFTS5RXJ4QJDEUGQQS","short_pith_number":"pith:MSDO6FPK","schema_version":"1.0","canonical_sha256":"6486ef15ea09672ec6e9e4123250d08485fa8c43d082fd3f0f2c04f4e372b3c2","source":{"kind":"arxiv","id":"2503.00102","version":2},"attestation_state":"computed","paper":{"title":"The Physical Properties and Morphologies of Faint Dusty Star-forming Galaxies Identified with JWST","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Amy J. Barger, Lennox L. Cowie, Michael J. Nicandro Rosenthal, Stephen J. McKay","submitted_at":"2025-02-28T19:00:00Z","abstract_excerpt":"We identify a sample of 234 dusty star-forming galaxies (DSFGs) in the A2744 and GOODS-S fields using JWST/NIRCam-selected galaxies as priors for SCUBA-2 measurements. This method provides a large number of galaxies both above an 850$\\,\\mathrm{\\mu}$m flux of 2 mJy (47 bright DSFGs) and below (187 faint DSFGs), representing the largest sample of individually identified (i.e., not stacked) faint DSFGs to date. We observe that the NIRCam F444W and F150W fluxes are tightly correlated with redshift, with fainter sources lying at higher redshifts, suggesting that the observed near-infrared flux may "},"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":"2503.00102","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2025-02-28T19:00:00Z","cross_cats_sorted":[],"title_canon_sha256":"4fb7ea3f6b56b1daad85bd485582035c4877ca1b30a2370d49279a34bf336f7b","abstract_canon_sha256":"5f043b577ffd37c81442bb45b4a242167ccfc585790bcd327f6c5d1c4c1ebf0b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:33:20.907979Z","signature_b64":"F0EHtn+DtrOyvQLVTTfqZmY1HB+/AMAShkSneKAoFYCQykbOWCdcGegFhYr3UNMOJuINfrhn7b16J0jhXEFeAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6486ef15ea09672ec6e9e4123250d08485fa8c43d082fd3f0f2c04f4e372b3c2","last_reissued_at":"2026-07-05T11:33:20.907540Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:33:20.907540Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Physical Properties and Morphologies of Faint Dusty Star-forming Galaxies Identified with JWST","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Amy J. Barger, Lennox L. Cowie, Michael J. Nicandro Rosenthal, Stephen J. McKay","submitted_at":"2025-02-28T19:00:00Z","abstract_excerpt":"We identify a sample of 234 dusty star-forming galaxies (DSFGs) in the A2744 and GOODS-S fields using JWST/NIRCam-selected galaxies as priors for SCUBA-2 measurements. This method provides a large number of galaxies both above an 850$\\,\\mathrm{\\mu}$m flux of 2 mJy (47 bright DSFGs) and below (187 faint DSFGs), representing the largest sample of individually identified (i.e., not stacked) faint DSFGs to date. We observe that the NIRCam F444W and F150W fluxes are tightly correlated with redshift, with fainter sources lying at higher redshifts, suggesting that the observed near-infrared flux may "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2503.00102","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/2503.00102/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":"2503.00102","created_at":"2026-07-05T11:33:20.907603+00:00"},{"alias_kind":"arxiv_version","alias_value":"2503.00102v2","created_at":"2026-07-05T11:33:20.907603+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2503.00102","created_at":"2026-07-05T11:33:20.907603+00:00"},{"alias_kind":"pith_short_12","alias_value":"MSDO6FPKBFTS","created_at":"2026-07-05T11:33:20.907603+00:00"},{"alias_kind":"pith_short_16","alias_value":"MSDO6FPKBFTS5RXJ","created_at":"2026-07-05T11:33:20.907603+00:00"},{"alias_kind":"pith_short_8","alias_value":"MSDO6FPK","created_at":"2026-07-05T11:33:20.907603+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2506.11601","citing_title":"Unveiling a Population of Strong Galaxy-Galaxy Lensed Faint Dusty Star-Forming Galaxies","ref_index":53,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS","json":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS.json","graph_json":"https://pith.science/api/pith-number/MSDO6FPKBFTS5RXJ4QJDEUGQQS/graph.json","events_json":"https://pith.science/api/pith-number/MSDO6FPKBFTS5RXJ4QJDEUGQQS/events.json","paper":"https://pith.science/paper/MSDO6FPK"},"agent_actions":{"view_html":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS","download_json":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS.json","view_paper":"https://pith.science/paper/MSDO6FPK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2503.00102&json=true","fetch_graph":"https://pith.science/api/pith-number/MSDO6FPKBFTS5RXJ4QJDEUGQQS/graph.json","fetch_events":"https://pith.science/api/pith-number/MSDO6FPKBFTS5RXJ4QJDEUGQQS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS/action/storage_attestation","attest_author":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS/action/author_attestation","sign_citation":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS/action/citation_signature","submit_replication":"https://pith.science/pith/MSDO6FPKBFTS5RXJ4QJDEUGQQS/action/replication_record"}},"created_at":"2026-07-05T11:33:20.907603+00:00","updated_at":"2026-07-05T11:33:20.907603+00:00"}