{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:Y4DMIA2KOJFEAUHDRHDYS3B3O6","short_pith_number":"pith:Y4DMIA2K","schema_version":"1.0","canonical_sha256":"c706c4034a724a4050e389c7896c3b77becb3eca5f03b03ab6e8bb7fd2f82070","source":{"kind":"arxiv","id":"1402.5916","version":1},"attestation_state":"computed","paper":{"title":"Renormalized Halo Bias","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Daniel Baumann, Daniel Green, Matias Zaldarriaga, Valentin Assassi","submitted_at":"2014-02-24T18:50:18Z","abstract_excerpt":"This paper provides a systematic study of renormalization in models of halo biasing. Building on work of McDonald, we show that Eulerian biasing is only consistent with renormalization if non-local terms and higher-derivative contributions are included in the biasing model. We explicitly determine the complete list of required bias parameters for Gaussian initial conditions, up to quartic order in the dark matter density contrast and at leading order in derivatives. At quadratic order, this means including the gravitational tidal tensor, while at cubic order the velocity potential appears as a"},"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":"1402.5916","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2014-02-24T18:50:18Z","cross_cats_sorted":["hep-th"],"title_canon_sha256":"cf043bcc5d721971efdc435db64a3ac974ef7e57ea35d61b685de228c75856cd","abstract_canon_sha256":"eab8834652c66f6af0fd70c3a6642afd13f0c98d661a76a34bd170434ce9c19e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:44:28.911083Z","signature_b64":"XnmTIxmVpofOHgrS3YpZC0Anc3LhuJYtNNOo6fvrQU05Kc60++C0VxWpH1iNWcPSVPP9rF8p4biSfxWzf74bCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c706c4034a724a4050e389c7896c3b77becb3eca5f03b03ab6e8bb7fd2f82070","last_reissued_at":"2026-05-18T01:44:28.910599Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:44:28.910599Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Renormalized Halo Bias","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Daniel Baumann, Daniel Green, Matias Zaldarriaga, Valentin Assassi","submitted_at":"2014-02-24T18:50:18Z","abstract_excerpt":"This paper provides a systematic study of renormalization in models of halo biasing. Building on work of McDonald, we show that Eulerian biasing is only consistent with renormalization if non-local terms and higher-derivative contributions are included in the biasing model. We explicitly determine the complete list of required bias parameters for Gaussian initial conditions, up to quartic order in the dark matter density contrast and at leading order in derivatives. At quadratic order, this means including the gravitational tidal tensor, while at cubic order the velocity potential appears as a"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1402.5916","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":"1402.5916","created_at":"2026-05-18T01:44:28.910671+00:00"},{"alias_kind":"arxiv_version","alias_value":"1402.5916v1","created_at":"2026-05-18T01:44:28.910671+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1402.5916","created_at":"2026-05-18T01:44:28.910671+00:00"},{"alias_kind":"pith_short_12","alias_value":"Y4DMIA2KOJFE","created_at":"2026-05-18T12:28:57.508820+00:00"},{"alias_kind":"pith_short_16","alias_value":"Y4DMIA2KOJFEAUHD","created_at":"2026-05-18T12:28:57.508820+00:00"},{"alias_kind":"pith_short_8","alias_value":"Y4DMIA2K","created_at":"2026-05-18T12:28:57.508820+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2408.03036","citing_title":"Modeling and measuring the anisotropic halo 3-point correlation function: a coordinated study","ref_index":62,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21436","citing_title":"Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum","ref_index":214,"is_internal_anchor":true},{"citing_arxiv_id":"2411.12021","citing_title":"DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars","ref_index":139,"is_internal_anchor":true},{"citing_arxiv_id":"2511.20757","citing_title":"Reanalyzing DESI DR1: 2. Constraints on Dark Energy, Spatial Curvature, and Neutrino Masses","ref_index":84,"is_internal_anchor":true},{"citing_arxiv_id":"2604.26915","citing_title":"Testing Scale-Dependent Modified Gravity with DESI DR1","ref_index":46,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08895","citing_title":"FolpsD: combining EFT and phenomenological approaches for joint power spectrum and bispectrum analyses","ref_index":7,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6","json":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6.json","graph_json":"https://pith.science/api/pith-number/Y4DMIA2KOJFEAUHDRHDYS3B3O6/graph.json","events_json":"https://pith.science/api/pith-number/Y4DMIA2KOJFEAUHDRHDYS3B3O6/events.json","paper":"https://pith.science/paper/Y4DMIA2K"},"agent_actions":{"view_html":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6","download_json":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6.json","view_paper":"https://pith.science/paper/Y4DMIA2K","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1402.5916&json=true","fetch_graph":"https://pith.science/api/pith-number/Y4DMIA2KOJFEAUHDRHDYS3B3O6/graph.json","fetch_events":"https://pith.science/api/pith-number/Y4DMIA2KOJFEAUHDRHDYS3B3O6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6/action/storage_attestation","attest_author":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6/action/author_attestation","sign_citation":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6/action/citation_signature","submit_replication":"https://pith.science/pith/Y4DMIA2KOJFEAUHDRHDYS3B3O6/action/replication_record"}},"created_at":"2026-05-18T01:44:28.910671+00:00","updated_at":"2026-05-18T01:44:28.910671+00:00"}