{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:YPH2D2IFMEZZOOUDK4N5ZME5VZ","short_pith_number":"pith:YPH2D2IF","schema_version":"1.0","canonical_sha256":"c3cfa1e9056133973a83571bdcb09dae4ba32d371fbd5a58daedd67fc88828f0","source":{"kind":"arxiv","id":"astro-ph/0611921","version":2},"attestation_state":"computed","paper":{"title":"Assembly bias in the clustering of dark matter haloes","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Liang Gao, Simon D. M. White","submitted_at":"2006-11-29T21:04:04Z","abstract_excerpt":"We use a very large simulation of structure growth in a LCDM universe -- the Millennium Simulation -- to study assembly bias, the fact that the large-scale clustering of haloes of given mass varies significantly with their assembly history. We extend earlier work based on the same simulation by superposing results for redshifts from 0 to 3, by defining a less noisy estimator of clustering amplitude, and by considering halo concentration, substructure mass fraction and spin, as well as formation time, as additional parameters. These improvements lead to results with less noise than previous stu"},"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/0611921","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-11-29T21:04:04Z","cross_cats_sorted":[],"title_canon_sha256":"ddeeb8d92a28a3deef64420fed40d52e4a35b1bc269cf168b1e6b946c480a73b","abstract_canon_sha256":"2296cae70239449c20640d3e0503482036edf95087d9e39a27230c25168035af"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:51:57.100963Z","signature_b64":"fMH5rlFDf6q1m+Hd6FrvfAkQTgbnfZZfJEFMEdlOq/p+fJJWwRRtF8adNcnFQK2i6RjaDHI3PhSc5z1Bbi6CDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c3cfa1e9056133973a83571bdcb09dae4ba32d371fbd5a58daedd67fc88828f0","last_reissued_at":"2026-07-04T15:51:57.100277Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:51:57.100277Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Assembly bias in the clustering of dark matter haloes","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Liang Gao, Simon D. M. White","submitted_at":"2006-11-29T21:04:04Z","abstract_excerpt":"We use a very large simulation of structure growth in a LCDM universe -- the Millennium Simulation -- to study assembly bias, the fact that the large-scale clustering of haloes of given mass varies significantly with their assembly history. We extend earlier work based on the same simulation by superposing results for redshifts from 0 to 3, by defining a less noisy estimator of clustering amplitude, and by considering halo concentration, substructure mass fraction and spin, as well as formation time, as additional parameters. These improvements lead to results with less noise than previous stu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0611921","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/astro-ph/0611921/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/0611921","created_at":"2026-07-04T15:51:57.100348+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0611921v2","created_at":"2026-07-04T15:51:57.100348+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0611921","created_at":"2026-07-04T15:51:57.100348+00:00"},{"alias_kind":"pith_short_12","alias_value":"YPH2D2IFMEZZ","created_at":"2026-07-04T15:51:57.100348+00:00"},{"alias_kind":"pith_short_16","alias_value":"YPH2D2IFMEZZOOUD","created_at":"2026-07-04T15:51:57.100348+00:00"},{"alias_kind":"pith_short_8","alias_value":"YPH2D2IF","created_at":"2026-07-04T15:51:57.100348+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2604.26022","citing_title":"Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos","ref_index":35,"is_internal_anchor":true},{"citing_arxiv_id":"0706.1243","citing_title":"A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies: I. Galaxy Mergers & Quasar Activity","ref_index":91,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ","json":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ.json","graph_json":"https://pith.science/api/pith-number/YPH2D2IFMEZZOOUDK4N5ZME5VZ/graph.json","events_json":"https://pith.science/api/pith-number/YPH2D2IFMEZZOOUDK4N5ZME5VZ/events.json","paper":"https://pith.science/paper/YPH2D2IF"},"agent_actions":{"view_html":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ","download_json":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ.json","view_paper":"https://pith.science/paper/YPH2D2IF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0611921&json=true","fetch_graph":"https://pith.science/api/pith-number/YPH2D2IFMEZZOOUDK4N5ZME5VZ/graph.json","fetch_events":"https://pith.science/api/pith-number/YPH2D2IFMEZZOOUDK4N5ZME5VZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ/action/storage_attestation","attest_author":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ/action/author_attestation","sign_citation":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ/action/citation_signature","submit_replication":"https://pith.science/pith/YPH2D2IFMEZZOOUDK4N5ZME5VZ/action/replication_record"}},"created_at":"2026-07-04T15:51:57.100348+00:00","updated_at":"2026-07-04T15:51:57.100348+00:00"}