{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:YA3ZYGAYECMLSCG2EIUDSMN2DX","short_pith_number":"pith:YA3ZYGAY","schema_version":"1.0","canonical_sha256":"c0379c18182098b908da22283931ba1dc92aa7d60874ea3afbf586b2d7ea96ec","source":{"kind":"arxiv","id":"1206.1324","version":2},"attestation_state":"computed","paper":{"title":"A Conditional Luminosity Function Model of the Cosmic Far-Infrared Background Anisotropy Power Spectrum","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Asantha Cooray, Francesco De Bernardis","submitted_at":"2012-06-06T20:00:03Z","abstract_excerpt":"The cosmic far-infrared background (CFIRB) is expected to be generated by faint, dusty star-forming galaxies during the peak epoch of galaxy formation. The anisotropy power spectrum of the CFIRB captures the spatial distribution of these galaxies in dark matter halos and the spatial distribution of dark matter halos in the large-scale structure. Existing halo models of CFIRB anisotropy power spectrum are either incomplete or lead to halo model parameters that are inconsistent with the galaxy distribution selected at other wavelengths. Here we present a conditional luminosity function approach "},"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":"1206.1324","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-06-06T20:00:03Z","cross_cats_sorted":[],"title_canon_sha256":"05efb50c524e2fd038fe38c66fb186936a37f03daa7a8f82346b54f3ee94ba37","abstract_canon_sha256":"cefb8c0ba615402884613124ef68fe44454165d1d68d9aca4d0e1efb956412f1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:57:01.341309Z","signature_b64":"tcN+q1HU/ZkJTrNSwor+5OVuWpmlZP6K18cx6AstcMSWznMQI52M2RHSKB9NiRCOX0SM7C/CSFZBPYBmHLUTDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c0379c18182098b908da22283931ba1dc92aa7d60874ea3afbf586b2d7ea96ec","last_reissued_at":"2026-05-18T01:57:01.340758Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:57:01.340758Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Conditional Luminosity Function Model of the Cosmic Far-Infrared Background Anisotropy Power Spectrum","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Asantha Cooray, Francesco De Bernardis","submitted_at":"2012-06-06T20:00:03Z","abstract_excerpt":"The cosmic far-infrared background (CFIRB) is expected to be generated by faint, dusty star-forming galaxies during the peak epoch of galaxy formation. The anisotropy power spectrum of the CFIRB captures the spatial distribution of these galaxies in dark matter halos and the spatial distribution of dark matter halos in the large-scale structure. Existing halo models of CFIRB anisotropy power spectrum are either incomplete or lead to halo model parameters that are inconsistent with the galaxy distribution selected at other wavelengths. Here we present a conditional luminosity function approach "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1206.1324","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":""},"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":"1206.1324","created_at":"2026-05-18T01:57:01.340861+00:00"},{"alias_kind":"arxiv_version","alias_value":"1206.1324v2","created_at":"2026-05-18T01:57:01.340861+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1206.1324","created_at":"2026-05-18T01:57:01.340861+00:00"},{"alias_kind":"pith_short_12","alias_value":"YA3ZYGAYECML","created_at":"2026-05-18T12:27:27.928770+00:00"},{"alias_kind":"pith_short_16","alias_value":"YA3ZYGAYECMLSCG2","created_at":"2026-05-18T12:27:27.928770+00:00"},{"alias_kind":"pith_short_8","alias_value":"YA3ZYGAY","created_at":"2026-05-18T12:27:27.928770+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2506.13851","citing_title":"Interstellar dust production, destruction and effects of dust depletion in galaxies","ref_index":265,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX","json":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX.json","graph_json":"https://pith.science/api/pith-number/YA3ZYGAYECMLSCG2EIUDSMN2DX/graph.json","events_json":"https://pith.science/api/pith-number/YA3ZYGAYECMLSCG2EIUDSMN2DX/events.json","paper":"https://pith.science/paper/YA3ZYGAY"},"agent_actions":{"view_html":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX","download_json":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX.json","view_paper":"https://pith.science/paper/YA3ZYGAY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1206.1324&json=true","fetch_graph":"https://pith.science/api/pith-number/YA3ZYGAYECMLSCG2EIUDSMN2DX/graph.json","fetch_events":"https://pith.science/api/pith-number/YA3ZYGAYECMLSCG2EIUDSMN2DX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX/action/storage_attestation","attest_author":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX/action/author_attestation","sign_citation":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX/action/citation_signature","submit_replication":"https://pith.science/pith/YA3ZYGAYECMLSCG2EIUDSMN2DX/action/replication_record"}},"created_at":"2026-05-18T01:57:01.340861+00:00","updated_at":"2026-05-18T01:57:01.340861+00:00"}