{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:AYLLSLSNL3WPJWE4Z4W7QZVZ5C","short_pith_number":"pith:AYLLSLSN","schema_version":"1.0","canonical_sha256":"0616b92e4d5eecf4d89ccf2df866b9e8a7c1b141f754f242dda3dac562a94aeb","source":{"kind":"arxiv","id":"2402.18481","version":2},"attestation_state":"computed","paper":{"title":"Towards a precision calculation of $N_{\\rm eff}$ in the Standard Model III: Improved estimate of NLO contributions to the collision integral","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"hep-ph","authors_text":"Luca Paolo Wiggering, Marco Drewes, Michael Klasen, Yannis Georis, Yvonne Y. Y. Wong","submitted_at":"2024-02-28T17:00:49Z","abstract_excerpt":"We compute the dominant QED correction to the neutrino-electron interaction rate in the vicinity of neutrino decoupling in the early universe, and estimate its impact on the effective number of neutrino species $N_{\\rm eff}$ in cosmic microwave background anisotropy observations. We find that the correction to the interaction rate is at the sub-percent level, consistent with a recent estimate by Jackson and Laine. Relative to that work we include the electron mass in our computations, but restrict our analysis to the enhanced $t$-channel contributions. The fractional change in $N_{\\rm eff}^{\\r"},"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":"2402.18481","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"hep-ph","submitted_at":"2024-02-28T17:00:49Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"5995e412d6fc0561e9bceb8662a1beee13e307723881183d1363439304950e59","abstract_canon_sha256":"d45d4a536b3cf05325d4168e9bed1997f2ecfe646195ed6a310ab9ca26506028"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:31:48.760678Z","signature_b64":"Yh2TwjI07d9kftYp/IWMJJfq2nuaZCR/GcOVXnuMzqSG6WvM9XPYJNCMcK5VMV/9xHnUhdrAF/PEqFWu3wauBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0616b92e4d5eecf4d89ccf2df866b9e8a7c1b141f754f242dda3dac562a94aeb","last_reissued_at":"2026-07-05T08:31:48.760173Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:31:48.760173Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Towards a precision calculation of $N_{\\rm eff}$ in the Standard Model III: Improved estimate of NLO contributions to the collision integral","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"hep-ph","authors_text":"Luca Paolo Wiggering, Marco Drewes, Michael Klasen, Yannis Georis, Yvonne Y. Y. Wong","submitted_at":"2024-02-28T17:00:49Z","abstract_excerpt":"We compute the dominant QED correction to the neutrino-electron interaction rate in the vicinity of neutrino decoupling in the early universe, and estimate its impact on the effective number of neutrino species $N_{\\rm eff}$ in cosmic microwave background anisotropy observations. We find that the correction to the interaction rate is at the sub-percent level, consistent with a recent estimate by Jackson and Laine. Relative to that work we include the electron mass in our computations, but restrict our analysis to the enhanced $t$-channel contributions. The fractional change in $N_{\\rm eff}^{\\r"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2402.18481","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/2402.18481/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":"2402.18481","created_at":"2026-07-05T08:31:48.760227+00:00"},{"alias_kind":"arxiv_version","alias_value":"2402.18481v2","created_at":"2026-07-05T08:31:48.760227+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2402.18481","created_at":"2026-07-05T08:31:48.760227+00:00"},{"alias_kind":"pith_short_12","alias_value":"AYLLSLSNL3WP","created_at":"2026-07-05T08:31:48.760227+00:00"},{"alias_kind":"pith_short_16","alias_value":"AYLLSLSNL3WPJWE4","created_at":"2026-07-05T08:31:48.760227+00:00"},{"alias_kind":"pith_short_8","alias_value":"AYLLSLSN","created_at":"2026-07-05T08:31:48.760227+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2607.01226","citing_title":"Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation","ref_index":279,"is_internal_anchor":false},{"citing_arxiv_id":"2605.18716","citing_title":"Recoupled Dark Radiation reconciling CMB and DESI BAO measurements","ref_index":59,"is_internal_anchor":false},{"citing_arxiv_id":"2506.23290","citing_title":"Type II Seesaw Leptogenesis in a Majoron background","ref_index":230,"is_internal_anchor":false},{"citing_arxiv_id":"2508.00798","citing_title":"Gravitational waves from axion inflation in the gradient expansion formalism. Part I. Pure axion inflation","ref_index":116,"is_internal_anchor":false},{"citing_arxiv_id":"2509.25013","citing_title":"Gravitational waves from axion inflation in the gradient expansion formalism. Part II. Fermionic axion inflation","ref_index":72,"is_internal_anchor":false},{"citing_arxiv_id":"2503.14744","citing_title":"Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape","ref_index":51,"is_internal_anchor":false},{"citing_arxiv_id":"2604.20768","citing_title":"Primordial Magnetogenesis and Gravitational Waves from ALP-assisted Phase Transition","ref_index":149,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C","json":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C.json","graph_json":"https://pith.science/api/pith-number/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/graph.json","events_json":"https://pith.science/api/pith-number/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/events.json","paper":"https://pith.science/paper/AYLLSLSN"},"agent_actions":{"view_html":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C","download_json":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C.json","view_paper":"https://pith.science/paper/AYLLSLSN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2402.18481&json=true","fetch_graph":"https://pith.science/api/pith-number/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/graph.json","fetch_events":"https://pith.science/api/pith-number/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/action/storage_attestation","attest_author":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/action/author_attestation","sign_citation":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/action/citation_signature","submit_replication":"https://pith.science/pith/AYLLSLSNL3WPJWE4Z4W7QZVZ5C/action/replication_record"}},"created_at":"2026-07-05T08:31:48.760227+00:00","updated_at":"2026-07-05T08:31:48.760227+00:00"}