{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:LFOGVFRQZRPZ6BWF4FC3CCQ4C6","short_pith_number":"pith:LFOGVFRQ","schema_version":"1.0","canonical_sha256":"595c6a9630cc5f9f06c5e145b10a1c178807fe4241741f9181d6031b614d6b4c","source":{"kind":"arxiv","id":"astro-ph/0609548","version":1},"attestation_state":"computed","paper":{"title":"What do we learn from IRAC observations of galaxies at 2 < z < 3.5?","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Alan F. M. Moorwood, Giovanni G. Fazio, Gregory Rudnick, Hans-Walter Rix, Huub Rottgering, Ivo Labbe, Jiasheng Huang, Marijn Franx, Natascha M. Forster Schreiber, Paul van der Werf, Pieter G. van Dokkum, Stijn Wuyts","submitted_at":"2006-09-19T20:02:58Z","abstract_excerpt":"We analyze very deep HST, VLT and Spitzer photometry of galaxies at 2<z<3.5 in the Hubble Deep Field South. The sample is selected from the deepest public K-band imaging currently available. We show that the rest-frame U-V vs V-J color-color diagram is a powerful diagnostic of the stellar populations of distant galaxies. Galaxies with red rest-frame U-V colors are generally red in rest-frame V-J as well. However, at a given U-V color a range in V-J colors exists, and we show that this allows us to distinguish young, dusty galaxies from old, passively evolving galaxies. We quantify the effects "},"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":"astro-ph/0609548","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-09-19T20:02:58Z","cross_cats_sorted":[],"title_canon_sha256":"f5ead8ab6f7e1937679ef3f279947383849fe44d9a1c6e26a474a17b0fa00596","abstract_canon_sha256":"bbb09e1914b37f297b0ce343065fde06bb20f45054287ee8a50c60631ec52391"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:28:38.055010Z","signature_b64":"Z5757UpbA+98IKyHbcYWPGF+ew+2SDtVsm6ZNzXVgOlHP/1aFaIzViwEevGckyYMBRrBl4xz/ZH0MjdegXEICw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"595c6a9630cc5f9f06c5e145b10a1c178807fe4241741f9181d6031b614d6b4c","last_reissued_at":"2026-07-04T15:28:38.054668Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:28:38.054668Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"What do we learn from IRAC observations of galaxies at 2 < z < 3.5?","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Alan F. M. Moorwood, Giovanni G. Fazio, Gregory Rudnick, Hans-Walter Rix, Huub Rottgering, Ivo Labbe, Jiasheng Huang, Marijn Franx, Natascha M. Forster Schreiber, Paul van der Werf, Pieter G. van Dokkum, Stijn Wuyts","submitted_at":"2006-09-19T20:02:58Z","abstract_excerpt":"We analyze very deep HST, VLT and Spitzer photometry of galaxies at 2<z<3.5 in the Hubble Deep Field South. The sample is selected from the deepest public K-band imaging currently available. We show that the rest-frame U-V vs V-J color-color diagram is a powerful diagnostic of the stellar populations of distant galaxies. Galaxies with red rest-frame U-V colors are generally red in rest-frame V-J as well. However, at a given U-V color a range in V-J colors exists, and we show that this allows us to distinguish young, dusty galaxies from old, passively evolving galaxies. We quantify the effects "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0609548","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/astro-ph/0609548/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":"astro-ph/0609548","created_at":"2026-07-04T15:28:38.054725+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0609548v1","created_at":"2026-07-04T15:28:38.054725+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0609548","created_at":"2026-07-04T15:28:38.054725+00:00"},{"alias_kind":"pith_short_12","alias_value":"LFOGVFRQZRPZ","created_at":"2026-07-04T15:28:38.054725+00:00"},{"alias_kind":"pith_short_16","alias_value":"LFOGVFRQZRPZ6BWF","created_at":"2026-07-04T15:28:38.054725+00:00"},{"alias_kind":"pith_short_8","alias_value":"LFOGVFRQ","created_at":"2026-07-04T15:28:38.054725+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.07818","citing_title":"The DESI View of the Faint Radio Source Population in LoTSS DR2","ref_index":94,"is_internal_anchor":true},{"citing_arxiv_id":"2606.21651","citing_title":"Resolved Ages and Stellar Metallicities in Progenitors of Milky Way Analogs: A Closer Look at their Star Formation Histories since $z=5$","ref_index":6,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6","json":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6.json","graph_json":"https://pith.science/api/pith-number/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/graph.json","events_json":"https://pith.science/api/pith-number/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/events.json","paper":"https://pith.science/paper/LFOGVFRQ"},"agent_actions":{"view_html":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6","download_json":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6.json","view_paper":"https://pith.science/paper/LFOGVFRQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0609548&json=true","fetch_graph":"https://pith.science/api/pith-number/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/graph.json","fetch_events":"https://pith.science/api/pith-number/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/action/storage_attestation","attest_author":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/action/author_attestation","sign_citation":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/action/citation_signature","submit_replication":"https://pith.science/pith/LFOGVFRQZRPZ6BWF4FC3CCQ4C6/action/replication_record"}},"created_at":"2026-07-04T15:28:38.054725+00:00","updated_at":"2026-07-04T15:28:38.054725+00:00"}