{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:CFFYWDJCAKIUUBR44D57BDA4OI","short_pith_number":"pith:CFFYWDJC","schema_version":"1.0","canonical_sha256":"114b8b0d2202914a063ce0fbf08c1c7225fd2f3d035c4417b6edb3864a37d7df","source":{"kind":"arxiv","id":"1512.05807","version":3},"attestation_state":"computed","paper":{"title":"Time-Sliced Perturbation Theory for Large Scale Structure I: General Formalism","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Diego Blas, Mathias Garny, Mikhail M. Ivanov, Sergey Sibiryakov","submitted_at":"2015-12-17T21:46:08Z","abstract_excerpt":"We present a new analytic approach to describe large scale structure formation in the mildly non-linear regime. The central object of the method is the time-dependent probability distribution function generating correlators of the cosmological observables at a given moment of time. Expanding the distribution function around the Gaussian weight we formulate a perturbative technique to calculate non-linear corrections to cosmological correlators, similar to the diagrammatic expansion in a three-dimensional Euclidean quantum field theory, with time playing the role of an external parameter. For t"},"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":"1512.05807","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2015-12-17T21:46:08Z","cross_cats_sorted":["hep-ph","hep-th"],"title_canon_sha256":"e0404e9fd7210757b73e0c0213de544ef0ca61172cb0cb13a2b374373a5b7acc","abstract_canon_sha256":"85ce67efe531bab684e0f55f41d0e809c057a4d6b25bf5af90d0f7eb7119a928"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:09:41.976528Z","signature_b64":"Nbw53u7WjdTPokzXvFoh9en3N0Knzv5JNKwCI2wgKYQFKUAFgnN893NyLN0WdktYWy4uhoL6na6ZK3lcj5ydAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"114b8b0d2202914a063ce0fbf08c1c7225fd2f3d035c4417b6edb3864a37d7df","last_reissued_at":"2026-05-18T01:09:41.975936Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:09:41.975936Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Time-Sliced Perturbation Theory for Large Scale Structure I: General Formalism","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Diego Blas, Mathias Garny, Mikhail M. Ivanov, Sergey Sibiryakov","submitted_at":"2015-12-17T21:46:08Z","abstract_excerpt":"We present a new analytic approach to describe large scale structure formation in the mildly non-linear regime. The central object of the method is the time-dependent probability distribution function generating correlators of the cosmological observables at a given moment of time. Expanding the distribution function around the Gaussian weight we formulate a perturbative technique to calculate non-linear corrections to cosmological correlators, similar to the diagrammatic expansion in a three-dimensional Euclidean quantum field theory, with time playing the role of an external parameter. For t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1512.05807","kind":"arxiv","version":3},"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":"1512.05807","created_at":"2026-05-18T01:09:41.976022+00:00"},{"alias_kind":"arxiv_version","alias_value":"1512.05807v3","created_at":"2026-05-18T01:09:41.976022+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1512.05807","created_at":"2026-05-18T01:09:41.976022+00:00"},{"alias_kind":"pith_short_12","alias_value":"CFFYWDJCAKIU","created_at":"2026-05-18T12:29:14.074870+00:00"},{"alias_kind":"pith_short_16","alias_value":"CFFYWDJCAKIUUBR4","created_at":"2026-05-18T12:29:14.074870+00:00"},{"alias_kind":"pith_short_8","alias_value":"CFFYWDJC","created_at":"2026-05-18T12:29:14.074870+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2606.26234","citing_title":"Lyman-Alpha Forest and its Cross-Correlation with High-Redshift Galaxies in Effective Field Theory at the Field Level","ref_index":145,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28172","citing_title":"Searching for primordial features with radio surveys: synergy between the power spectrum and bispectrum","ref_index":128,"is_internal_anchor":true},{"citing_arxiv_id":"2606.30713","citing_title":"Galaxy Power Spectrum at Two-Loop Order: Implications for Weak Lensing Surveys and New Physics","ref_index":84,"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":87,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI","json":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI.json","graph_json":"https://pith.science/api/pith-number/CFFYWDJCAKIUUBR44D57BDA4OI/graph.json","events_json":"https://pith.science/api/pith-number/CFFYWDJCAKIUUBR44D57BDA4OI/events.json","paper":"https://pith.science/paper/CFFYWDJC"},"agent_actions":{"view_html":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI","download_json":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI.json","view_paper":"https://pith.science/paper/CFFYWDJC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1512.05807&json=true","fetch_graph":"https://pith.science/api/pith-number/CFFYWDJCAKIUUBR44D57BDA4OI/graph.json","fetch_events":"https://pith.science/api/pith-number/CFFYWDJCAKIUUBR44D57BDA4OI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI/action/storage_attestation","attest_author":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI/action/author_attestation","sign_citation":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI/action/citation_signature","submit_replication":"https://pith.science/pith/CFFYWDJCAKIUUBR44D57BDA4OI/action/replication_record"}},"created_at":"2026-05-18T01:09:41.976022+00:00","updated_at":"2026-05-18T01:09:41.976022+00:00"}