{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:7ZK3IQMBAYV4U4MD2EZPNJMIEB","short_pith_number":"pith:7ZK3IQMB","schema_version":"1.0","canonical_sha256":"fe55b44181062bca7183d132f6a5882063f40181178c6df96ee01c6ef7d6b18d","source":{"kind":"arxiv","id":"0909.4302","version":2},"attestation_state":"computed","paper":{"title":"Assembly bias and the dynamical structure of dark matter halos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Andreas Faltenbacher, Simon D. M. White","submitted_at":"2009-09-24T13:21:11Z","abstract_excerpt":"Based on the Millennium Simulation we examine assembly bias for the halo properties: shape, triaxiality, concentration, spin, shape of the velocity ellipsoid and velocity anisotropy. For consistency we determine all these properties using the same set of particles, namely all gravitationally self-bound particles belonging to the most massive sub-structure of a given friends-of-friends halo. We confirm that near-spherical and high-spin halos show enhanced clustering. The opposite is true for strongly aspherical and low-spin halos. Further, below the typical collapse mass, M*, more concentrated "},"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":"0909.4302","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-09-24T13:21:11Z","cross_cats_sorted":[],"title_canon_sha256":"4a1e0b84e6bf29fdcdbcf12c56d0908f3f5dbb9fcf8298fc048103c7de323517","abstract_canon_sha256":"440adb3ada2e7d2f013a5a6c75e84cafdd28e09330d80ddebaf0fa7d6757186f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:34:27.903039Z","signature_b64":"uAaLt/+2Yv7JuxvdM6Iqg3Ap3lOQyC4eKN8Hc+z3OxrDoXNGRHEvIImceBoJkoAIY7v6FfQJixqVskTSMT6ZAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fe55b44181062bca7183d132f6a5882063f40181178c6df96ee01c6ef7d6b18d","last_reissued_at":"2026-05-18T02:34:27.902420Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:34:27.902420Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Assembly bias and the dynamical structure of dark matter halos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Andreas Faltenbacher, Simon D. M. White","submitted_at":"2009-09-24T13:21:11Z","abstract_excerpt":"Based on the Millennium Simulation we examine assembly bias for the halo properties: shape, triaxiality, concentration, spin, shape of the velocity ellipsoid and velocity anisotropy. For consistency we determine all these properties using the same set of particles, namely all gravitationally self-bound particles belonging to the most massive sub-structure of a given friends-of-friends halo. We confirm that near-spherical and high-spin halos show enhanced clustering. The opposite is true for strongly aspherical and low-spin halos. Further, below the typical collapse mass, M*, more concentrated "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0909.4302","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":"0909.4302","created_at":"2026-05-18T02:34:27.902512+00:00"},{"alias_kind":"arxiv_version","alias_value":"0909.4302v2","created_at":"2026-05-18T02:34:27.902512+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0909.4302","created_at":"2026-05-18T02:34:27.902512+00:00"},{"alias_kind":"pith_short_12","alias_value":"7ZK3IQMBAYV4","created_at":"2026-05-18T12:25:58.837520+00:00"},{"alias_kind":"pith_short_16","alias_value":"7ZK3IQMBAYV4U4MD","created_at":"2026-05-18T12:25:58.837520+00:00"},{"alias_kind":"pith_short_8","alias_value":"7ZK3IQMB","created_at":"2026-05-18T12:25:58.837520+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.26022","citing_title":"Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos","ref_index":36,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB","json":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB.json","graph_json":"https://pith.science/api/pith-number/7ZK3IQMBAYV4U4MD2EZPNJMIEB/graph.json","events_json":"https://pith.science/api/pith-number/7ZK3IQMBAYV4U4MD2EZPNJMIEB/events.json","paper":"https://pith.science/paper/7ZK3IQMB"},"agent_actions":{"view_html":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB","download_json":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB.json","view_paper":"https://pith.science/paper/7ZK3IQMB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0909.4302&json=true","fetch_graph":"https://pith.science/api/pith-number/7ZK3IQMBAYV4U4MD2EZPNJMIEB/graph.json","fetch_events":"https://pith.science/api/pith-number/7ZK3IQMBAYV4U4MD2EZPNJMIEB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB/action/storage_attestation","attest_author":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB/action/author_attestation","sign_citation":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB/action/citation_signature","submit_replication":"https://pith.science/pith/7ZK3IQMBAYV4U4MD2EZPNJMIEB/action/replication_record"}},"created_at":"2026-05-18T02:34:27.902512+00:00","updated_at":"2026-05-18T02:34:27.902512+00:00"}