{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:4RWQHRFTBZSHLYV73RG3MPABN2","short_pith_number":"pith:4RWQHRFT","schema_version":"1.0","canonical_sha256":"e46d03c4b30e6475e2bfdc4db63c016eaf939d3ceb6d21fb939c969d6b6f41f2","source":{"kind":"arxiv","id":"1206.0052","version":2},"attestation_state":"computed","paper":{"title":"Galaxy formation in WMAP1 and WMAP7 cosmologies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Bruno Henriques, Chris Short, Gerard Lemson, Michael Boylan-Kolchin, Peter Thomas, Qi Guo, Raul E. Angulo, Simon White","submitted_at":"2012-06-01T00:00:52Z","abstract_excerpt":"Using the technique of Angulo & White (2010) we scale the Millennium and Millennium-II simulations of structure growth in a LCDM universe from the cosmological parameters with which they were carried out (based on first-year results from the Wilkinson Microwave Anisotropy Probe, WMAP1) to parameters consistent with the seven-year WMAP data (WMAP7). We implement semi-analytic galaxy formation modelling on both simulations in both cosmologies to investigate how the formation, evolution and clustering of galaxies are predicted to vary with cosmological parameters. The increased matter density Ome"},"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":"1206.0052","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-06-01T00:00:52Z","cross_cats_sorted":[],"title_canon_sha256":"da447c6061da700443356fbf566812e6e11f7d069fbcb28582eda374d388a1f8","abstract_canon_sha256":"3d505a0f77119d1affb422f0cde99dbb2a0367d3e54ca7b30e5595623b8b66d5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:57:09.068668Z","signature_b64":"JfAoeijhlmwqWAmeHOsHsoo2AFkM0pu/Qndy/A07qFEuFOpu8tDe5r4CF0Qgsa8Svj3ASaBo55HV9ldlJ/zTDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e46d03c4b30e6475e2bfdc4db63c016eaf939d3ceb6d21fb939c969d6b6f41f2","last_reissued_at":"2026-05-18T01:57:09.068203Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:57:09.068203Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Galaxy formation in WMAP1 and WMAP7 cosmologies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Bruno Henriques, Chris Short, Gerard Lemson, Michael Boylan-Kolchin, Peter Thomas, Qi Guo, Raul E. Angulo, Simon White","submitted_at":"2012-06-01T00:00:52Z","abstract_excerpt":"Using the technique of Angulo & White (2010) we scale the Millennium and Millennium-II simulations of structure growth in a LCDM universe from the cosmological parameters with which they were carried out (based on first-year results from the Wilkinson Microwave Anisotropy Probe, WMAP1) to parameters consistent with the seven-year WMAP data (WMAP7). We implement semi-analytic galaxy formation modelling on both simulations in both cosmologies to investigate how the formation, evolution and clustering of galaxies are predicted to vary with cosmological parameters. The increased matter density Ome"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1206.0052","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":"1206.0052","created_at":"2026-05-18T01:57:09.068274+00:00"},{"alias_kind":"arxiv_version","alias_value":"1206.0052v2","created_at":"2026-05-18T01:57:09.068274+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1206.0052","created_at":"2026-05-18T01:57:09.068274+00:00"},{"alias_kind":"pith_short_12","alias_value":"4RWQHRFTBZSH","created_at":"2026-05-18T12:26:53.410803+00:00"},{"alias_kind":"pith_short_16","alias_value":"4RWQHRFTBZSHLYV7","created_at":"2026-05-18T12:26:53.410803+00:00"},{"alias_kind":"pith_short_8","alias_value":"4RWQHRFT","created_at":"2026-05-18T12:26:53.410803+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.08353","citing_title":"Empirical estimates of how massive galaxies can be in {\\Lambda}CDM","ref_index":16,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2","json":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2.json","graph_json":"https://pith.science/api/pith-number/4RWQHRFTBZSHLYV73RG3MPABN2/graph.json","events_json":"https://pith.science/api/pith-number/4RWQHRFTBZSHLYV73RG3MPABN2/events.json","paper":"https://pith.science/paper/4RWQHRFT"},"agent_actions":{"view_html":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2","download_json":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2.json","view_paper":"https://pith.science/paper/4RWQHRFT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1206.0052&json=true","fetch_graph":"https://pith.science/api/pith-number/4RWQHRFTBZSHLYV73RG3MPABN2/graph.json","fetch_events":"https://pith.science/api/pith-number/4RWQHRFTBZSHLYV73RG3MPABN2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2/action/storage_attestation","attest_author":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2/action/author_attestation","sign_citation":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2/action/citation_signature","submit_replication":"https://pith.science/pith/4RWQHRFTBZSHLYV73RG3MPABN2/action/replication_record"}},"created_at":"2026-05-18T01:57:09.068274+00:00","updated_at":"2026-05-18T01:57:09.068274+00:00"}