{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:CXW6XKPESVOIFDBZJ5U3HPNQ2A","short_pith_number":"pith:CXW6XKPE","schema_version":"1.0","canonical_sha256":"15edeba9e4955c828c394f69b3bdb0d0289e7ac1be99c00bc9d626eb301fc120","source":{"kind":"arxiv","id":"2406.07610","version":3},"attestation_state":"computed","paper":{"title":"Regularizing infrared divergences in de Sitter spacetime: Loops, dimensional regularization, and cutoffs","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","hep-ph"],"primary_cat":"hep-th","authors_text":"Ellie Hughes, Gonzalo A. Palma, Javier Huenupi, Spyros Sypsas","submitted_at":"2024-06-11T18:00:01Z","abstract_excerpt":"Correlation functions of light scalar fields in de Sitter spacetime, computed via standard perturbation theory, often exhibit secular growth characterized by time-dependent divergent terms in the form of powers of $\\ln a(t)$, where $a(t)$ is the scale factor describing cosmic expansion. It is widely believed that loop corrections further enhance this secular growth. We argue that this is not necessarily the case: Loop corrections can be systematically handled using standard perturbative techniques, such as dimensional regularization, without introducing new $\\ln a(t)$ terms. We focus on a cano"},"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":"2406.07610","kind":"arxiv","version":3},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"hep-th","submitted_at":"2024-06-11T18:00:01Z","cross_cats_sorted":["astro-ph.CO","hep-ph"],"title_canon_sha256":"c376410f02764e50800604d13cc4e7e51d66e116d5568987096ca075c9ba8790","abstract_canon_sha256":"eecb2d7c0e33a420b536fb23d9a5a805b4e8ef652405d24c95038ff138265d2d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:56:21.528627Z","signature_b64":"UdOqoZoD9HNvym1OKcn2IvWjHokf7jyIURWOGy1ImuBMlNA+vOfKnqkktwudeoqj3vD/THt91w0fi5LpuGNLAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"15edeba9e4955c828c394f69b3bdb0d0289e7ac1be99c00bc9d626eb301fc120","last_reissued_at":"2026-07-05T09:56:21.528198Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:56:21.528198Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Regularizing infrared divergences in de Sitter spacetime: Loops, dimensional regularization, and cutoffs","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","hep-ph"],"primary_cat":"hep-th","authors_text":"Ellie Hughes, Gonzalo A. Palma, Javier Huenupi, Spyros Sypsas","submitted_at":"2024-06-11T18:00:01Z","abstract_excerpt":"Correlation functions of light scalar fields in de Sitter spacetime, computed via standard perturbation theory, often exhibit secular growth characterized by time-dependent divergent terms in the form of powers of $\\ln a(t)$, where $a(t)$ is the scale factor describing cosmic expansion. It is widely believed that loop corrections further enhance this secular growth. We argue that this is not necessarily the case: Loop corrections can be systematically handled using standard perturbative techniques, such as dimensional regularization, without introducing new $\\ln a(t)$ terms. We focus on a cano"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2406.07610","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2406.07610/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":"2406.07610","created_at":"2026-07-05T09:56:21.528254+00:00"},{"alias_kind":"arxiv_version","alias_value":"2406.07610v3","created_at":"2026-07-05T09:56:21.528254+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2406.07610","created_at":"2026-07-05T09:56:21.528254+00:00"},{"alias_kind":"pith_short_12","alias_value":"CXW6XKPESVOI","created_at":"2026-07-05T09:56:21.528254+00:00"},{"alias_kind":"pith_short_16","alias_value":"CXW6XKPESVOIFDBZ","created_at":"2026-07-05T09:56:21.528254+00:00"},{"alias_kind":"pith_short_8","alias_value":"CXW6XKPE","created_at":"2026-07-05T09:56:21.528254+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2511.23076","citing_title":"Scalar field effective potentials in de Sitter spacetime","ref_index":30,"is_internal_anchor":false},{"citing_arxiv_id":"2509.02696","citing_title":"Unitary and Analytic Renormalisation of Cosmological Correlators","ref_index":39,"is_internal_anchor":false},{"citing_arxiv_id":"2605.11096","citing_title":"Stochastic inflation from a non-equilibrium renormalization group","ref_index":24,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A","json":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A.json","graph_json":"https://pith.science/api/pith-number/CXW6XKPESVOIFDBZJ5U3HPNQ2A/graph.json","events_json":"https://pith.science/api/pith-number/CXW6XKPESVOIFDBZJ5U3HPNQ2A/events.json","paper":"https://pith.science/paper/CXW6XKPE"},"agent_actions":{"view_html":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A","download_json":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A.json","view_paper":"https://pith.science/paper/CXW6XKPE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2406.07610&json=true","fetch_graph":"https://pith.science/api/pith-number/CXW6XKPESVOIFDBZJ5U3HPNQ2A/graph.json","fetch_events":"https://pith.science/api/pith-number/CXW6XKPESVOIFDBZJ5U3HPNQ2A/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A/action/storage_attestation","attest_author":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A/action/author_attestation","sign_citation":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A/action/citation_signature","submit_replication":"https://pith.science/pith/CXW6XKPESVOIFDBZJ5U3HPNQ2A/action/replication_record"}},"created_at":"2026-07-05T09:56:21.528254+00:00","updated_at":"2026-07-05T09:56:21.528254+00:00"}