{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:OD3QRESD2TXD53NISTC7VEVNTQ","short_pith_number":"pith:OD3QRESD","schema_version":"1.0","canonical_sha256":"70f7089243d4ee3eeda894c5fa92ad9c3cbab24d911b217ec4f91a9172ac814e","source":{"kind":"arxiv","id":"2305.11228","version":2},"attestation_state":"computed","paper":{"title":"Leading Loops in Cosmological Correlators","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc"],"primary_cat":"hep-th","authors_text":"Ciaran McCulloch, Enrico Pajer, Mang Hei Gordon Lee","submitted_at":"2023-05-18T18:00:20Z","abstract_excerpt":"Cosmological correlators from inflation are often generated at tree level and hence loop contributions are bounded to be small corrections by perturbativity. Here we discuss a scenario where this is not the case. Recently, it has been shown that for any number of scalar fields of any mass, the parity-odd trispectrum of a massless scalar must vanish in the limit of exact scale invariance due to unitarity and the choice of initial state. By carefully handling UV-divergences, we show that the one-loop contribution is non-vanishing and hence leading. Surprisingly, the one-loop parity-odd trispectr"},"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":"2305.11228","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-th","submitted_at":"2023-05-18T18:00:20Z","cross_cats_sorted":["astro-ph.CO","gr-qc"],"title_canon_sha256":"370275da14c77025556222fbe5c18954993f1ebc1541b526cfc78546327b7cf9","abstract_canon_sha256":"f44ec5e8bfa304bccb00ad173a774e770f6b185698d2478944080f9235096e38"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:09:48.355723Z","signature_b64":"DkKSnFx0XflLHlBprrn4e9U567BzVOxJrVzSjMPzRb9Zcr4p9+VDs10UON2IdH+qT2o8gMj9+nsZLPBxCGqUDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"70f7089243d4ee3eeda894c5fa92ad9c3cbab24d911b217ec4f91a9172ac814e","last_reissued_at":"2026-07-05T07:09:48.353842Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:09:48.353842Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Leading Loops in Cosmological Correlators","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc"],"primary_cat":"hep-th","authors_text":"Ciaran McCulloch, Enrico Pajer, Mang Hei Gordon Lee","submitted_at":"2023-05-18T18:00:20Z","abstract_excerpt":"Cosmological correlators from inflation are often generated at tree level and hence loop contributions are bounded to be small corrections by perturbativity. Here we discuss a scenario where this is not the case. Recently, it has been shown that for any number of scalar fields of any mass, the parity-odd trispectrum of a massless scalar must vanish in the limit of exact scale invariance due to unitarity and the choice of initial state. By carefully handling UV-divergences, we show that the one-loop contribution is non-vanishing and hence leading. Surprisingly, the one-loop parity-odd trispectr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2305.11228","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/2305.11228/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":"2305.11228","created_at":"2026-07-05T07:09:48.354690+00:00"},{"alias_kind":"arxiv_version","alias_value":"2305.11228v2","created_at":"2026-07-05T07:09:48.354690+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2305.11228","created_at":"2026-07-05T07:09:48.354690+00:00"},{"alias_kind":"pith_short_12","alias_value":"OD3QRESD2TXD","created_at":"2026-07-05T07:09:48.354690+00:00"},{"alias_kind":"pith_short_16","alias_value":"OD3QRESD2TXD53NI","created_at":"2026-07-05T07:09:48.354690+00:00"},{"alias_kind":"pith_short_8","alias_value":"OD3QRESD","created_at":"2026-07-05T07:09:48.354690+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06679","citing_title":"Classical conformal invariance and superhorizon dynamics in de Sitter","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2606.07467","citing_title":"Stochastic scalar-tensor inflation and beyond","ref_index":113,"is_internal_anchor":false},{"citing_arxiv_id":"2605.28054","citing_title":"Fermionic Bubble Loop in Cosmological Collider Revisited: Exact signals from spectral and Mellin-Barnes methods","ref_index":105,"is_internal_anchor":false},{"citing_arxiv_id":"2505.16071","citing_title":"A Match Made in Heaven: Linking Observables in Inflationary Cosmology","ref_index":65,"is_internal_anchor":false},{"citing_arxiv_id":"2509.02696","citing_title":"Unitary and Analytic Renormalisation of Cosmological Correlators","ref_index":22,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26421","citing_title":"On the simplicity of de Sitter correlators","ref_index":52,"is_internal_anchor":false},{"citing_arxiv_id":"2604.09765","citing_title":"Multi-soft theorems for cosmological correlators: Background wave method for scalars & gravitons","ref_index":41,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ","json":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ.json","graph_json":"https://pith.science/api/pith-number/OD3QRESD2TXD53NISTC7VEVNTQ/graph.json","events_json":"https://pith.science/api/pith-number/OD3QRESD2TXD53NISTC7VEVNTQ/events.json","paper":"https://pith.science/paper/OD3QRESD"},"agent_actions":{"view_html":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ","download_json":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ.json","view_paper":"https://pith.science/paper/OD3QRESD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2305.11228&json=true","fetch_graph":"https://pith.science/api/pith-number/OD3QRESD2TXD53NISTC7VEVNTQ/graph.json","fetch_events":"https://pith.science/api/pith-number/OD3QRESD2TXD53NISTC7VEVNTQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ/action/storage_attestation","attest_author":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ/action/author_attestation","sign_citation":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ/action/citation_signature","submit_replication":"https://pith.science/pith/OD3QRESD2TXD53NISTC7VEVNTQ/action/replication_record"}},"created_at":"2026-07-05T07:09:48.354690+00:00","updated_at":"2026-07-05T07:09:48.354690+00:00"}