{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:YQXFS2UNOIDBRS4F62XTR5DAGO","short_pith_number":"pith:YQXFS2UN","schema_version":"1.0","canonical_sha256":"c42e596a8d720618cb85f6af38f46033b8d1a392056177c95f4a3c1c97daad0a","source":{"kind":"arxiv","id":"1705.01988","version":1},"attestation_state":"computed","paper":{"title":"Revisiting HOD model assumptions: the impact of AGN feedback and assembly bias","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Carlton Baugh, John Helly, Nuala McCullagh, Peder Norberg, Shaun Cole, Violeta Gonzalez-Perez","submitted_at":"2017-05-01T15:59:50Z","abstract_excerpt":"The standard Halo Occupation Distribution (HOD) models were originally developed based on results from semi-analytic and hydrodynamical galaxy formation models. Those models have since progressed, in particular to include AGN feedback to match the galaxy luminosity function in a universe with the observed baryon fraction. AGN feedback affects the relationship between galaxy stellar mass and luminosity, in particular making the relationship non-monotonic. For matched number density samples, galaxies in luminosity-threshold samples occupy a different range of halo masses from those in stellar-ma"},"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":"1705.01988","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-05-01T15:59:50Z","cross_cats_sorted":[],"title_canon_sha256":"d80f09d8944a080015059d95e4c9956f6523f1192b94681928f47fbfe33b7e45","abstract_canon_sha256":"22098d765233348fbcc10ffabaa8db35fdc1b0ae8453e6f30ba57d46f45590eb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:45:00.927761Z","signature_b64":"7YtE2VyR0KFakFpTrIdJmTTzWqI5zeYQp8deDAjIjI5/CP322jZF2JpCDRfUiV1hPvLb5icCK42my3oAwFQVBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c42e596a8d720618cb85f6af38f46033b8d1a392056177c95f4a3c1c97daad0a","last_reissued_at":"2026-05-18T00:45:00.927291Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:45:00.927291Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Revisiting HOD model assumptions: the impact of AGN feedback and assembly bias","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Carlton Baugh, John Helly, Nuala McCullagh, Peder Norberg, Shaun Cole, Violeta Gonzalez-Perez","submitted_at":"2017-05-01T15:59:50Z","abstract_excerpt":"The standard Halo Occupation Distribution (HOD) models were originally developed based on results from semi-analytic and hydrodynamical galaxy formation models. Those models have since progressed, in particular to include AGN feedback to match the galaxy luminosity function in a universe with the observed baryon fraction. AGN feedback affects the relationship between galaxy stellar mass and luminosity, in particular making the relationship non-monotonic. For matched number density samples, galaxies in luminosity-threshold samples occupy a different range of halo masses from those in stellar-ma"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1705.01988","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":"1705.01988","created_at":"2026-05-18T00:45:00.927362+00:00"},{"alias_kind":"arxiv_version","alias_value":"1705.01988v1","created_at":"2026-05-18T00:45:00.927362+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1705.01988","created_at":"2026-05-18T00:45:00.927362+00:00"},{"alias_kind":"pith_short_12","alias_value":"YQXFS2UNOIDB","created_at":"2026-05-18T12:31:56.362134+00:00"},{"alias_kind":"pith_short_16","alias_value":"YQXFS2UNOIDBRS4F","created_at":"2026-05-18T12:31:56.362134+00:00"},{"alias_kind":"pith_short_8","alias_value":"YQXFS2UN","created_at":"2026-05-18T12:31:56.362134+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.05561","citing_title":"What can galaxy clustering really tell us about the galaxy-halo connections?","ref_index":94,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO","json":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO.json","graph_json":"https://pith.science/api/pith-number/YQXFS2UNOIDBRS4F62XTR5DAGO/graph.json","events_json":"https://pith.science/api/pith-number/YQXFS2UNOIDBRS4F62XTR5DAGO/events.json","paper":"https://pith.science/paper/YQXFS2UN"},"agent_actions":{"view_html":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO","download_json":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO.json","view_paper":"https://pith.science/paper/YQXFS2UN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1705.01988&json=true","fetch_graph":"https://pith.science/api/pith-number/YQXFS2UNOIDBRS4F62XTR5DAGO/graph.json","fetch_events":"https://pith.science/api/pith-number/YQXFS2UNOIDBRS4F62XTR5DAGO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO/action/storage_attestation","attest_author":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO/action/author_attestation","sign_citation":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO/action/citation_signature","submit_replication":"https://pith.science/pith/YQXFS2UNOIDBRS4F62XTR5DAGO/action/replication_record"}},"created_at":"2026-05-18T00:45:00.927362+00:00","updated_at":"2026-05-18T00:45:00.927362+00:00"}