{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:DCGC35LHIOTD6MWLKHAIGJZSUY","short_pith_number":"pith:DCGC35LH","schema_version":"1.0","canonical_sha256":"188c2df56743a63f32cb51c0832732a637194b6c383916eabd649961b0aa8760","source":{"kind":"arxiv","id":"2408.15949","version":2},"attestation_state":"computed","paper":{"title":"Probing Lorentz invariance with a high-energy neutrino flare","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ex","hep-ph","hep-th"],"primary_cat":"astro-ph.HE","authors_text":"Alexander S. Sakharov, John Ellis, Mauricio Bustamante, Rostislav Konoplich","submitted_at":"2024-08-28T17:08:18Z","abstract_excerpt":"Time-of-flight measurements of high-energy astrophysical neutrinos can be used to probe Lorentz invariance, a pillar of modern physics. If Lorentz-invariance violation (LIV) occurs, it could cause neutrinos to slow down, with the delay scaling linearly or quadratically with their energy. We introduce non-parametric statistical methods designed to detect LIV-induced distortions in the temporal structure of a high-energy neutrino flare as it travels to Earth from a distant astrophysical source, independently of the intrinsic timing properties of the source. Our approach, illustrated using the 20"},"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":"2408.15949","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-08-28T17:08:18Z","cross_cats_sorted":["gr-qc","hep-ex","hep-ph","hep-th"],"title_canon_sha256":"ebb164b7d136ffe5ad997b7f523a054f0032c1401d4f119e654debcdf16ada1f","abstract_canon_sha256":"c19ed02089add28923c138d710c6ab2b391d5790eae4e39a354e379be2e7fe07"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:29:01.312426Z","signature_b64":"KbzXHwejH/C38giDnqLoqxrF3qNm1nnsR/oIBHZ/xMzvPCMgsAHpp7Q7uOeqGI3n4EU7Zw3XSOjjoCTkA8hPCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"188c2df56743a63f32cb51c0832732a637194b6c383916eabd649961b0aa8760","last_reissued_at":"2026-07-05T11:29:01.311652Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:29:01.311652Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing Lorentz invariance with a high-energy neutrino flare","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ex","hep-ph","hep-th"],"primary_cat":"astro-ph.HE","authors_text":"Alexander S. Sakharov, John Ellis, Mauricio Bustamante, Rostislav Konoplich","submitted_at":"2024-08-28T17:08:18Z","abstract_excerpt":"Time-of-flight measurements of high-energy astrophysical neutrinos can be used to probe Lorentz invariance, a pillar of modern physics. If Lorentz-invariance violation (LIV) occurs, it could cause neutrinos to slow down, with the delay scaling linearly or quadratically with their energy. We introduce non-parametric statistical methods designed to detect LIV-induced distortions in the temporal structure of a high-energy neutrino flare as it travels to Earth from a distant astrophysical source, independently of the intrinsic timing properties of the source. Our approach, illustrated using the 20"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2408.15949","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/2408.15949/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":"2408.15949","created_at":"2026-07-05T11:29:01.311746+00:00"},{"alias_kind":"arxiv_version","alias_value":"2408.15949v2","created_at":"2026-07-05T11:29:01.311746+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2408.15949","created_at":"2026-07-05T11:29:01.311746+00:00"},{"alias_kind":"pith_short_12","alias_value":"DCGC35LHIOTD","created_at":"2026-07-05T11:29:01.311746+00:00"},{"alias_kind":"pith_short_16","alias_value":"DCGC35LHIOTD6MWL","created_at":"2026-07-05T11:29:01.311746+00:00"},{"alias_kind":"pith_short_8","alias_value":"DCGC35LH","created_at":"2026-07-05T11:29:01.311746+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2607.01339","citing_title":"Electron stability constrains neutrino time delays","ref_index":16,"is_internal_anchor":false},{"citing_arxiv_id":"2604.19880","citing_title":"Ultra-High-Energy Tau Neutrinos as Probes of Lorentz Invariance","ref_index":23,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY","json":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY.json","graph_json":"https://pith.science/api/pith-number/DCGC35LHIOTD6MWLKHAIGJZSUY/graph.json","events_json":"https://pith.science/api/pith-number/DCGC35LHIOTD6MWLKHAIGJZSUY/events.json","paper":"https://pith.science/paper/DCGC35LH"},"agent_actions":{"view_html":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY","download_json":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY.json","view_paper":"https://pith.science/paper/DCGC35LH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2408.15949&json=true","fetch_graph":"https://pith.science/api/pith-number/DCGC35LHIOTD6MWLKHAIGJZSUY/graph.json","fetch_events":"https://pith.science/api/pith-number/DCGC35LHIOTD6MWLKHAIGJZSUY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY/action/storage_attestation","attest_author":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY/action/author_attestation","sign_citation":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY/action/citation_signature","submit_replication":"https://pith.science/pith/DCGC35LHIOTD6MWLKHAIGJZSUY/action/replication_record"}},"created_at":"2026-07-05T11:29:01.311746+00:00","updated_at":"2026-07-05T11:29:01.311746+00:00"}