{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:EXJSDNXHHQ5SN2L6XIVNVNU6RL","short_pith_number":"pith:EXJSDNXH","schema_version":"1.0","canonical_sha256":"25d321b6e73c3b26e97eba2adab69e8af27a2facd62c23475fedc644af9f28a0","source":{"kind":"arxiv","id":"2310.15224","version":2},"attestation_state":"computed","paper":{"title":"Flavor Anisotropy in the High-Energy Astrophysical Neutrino Sky","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ex","hep-ph","hep-th"],"primary_cat":"astro-ph.HE","authors_text":"Bernanda Telalovic, Mauricio Bustamante","submitted_at":"2023-10-23T18:00:01Z","abstract_excerpt":"High-energy astrophysical neutrinos, with TeV--PeV energies, offer unique insight into astrophysics and particle physics. Their incoming directions and flavor composition -- i.e., the proportion of electron, muon, and tau neutrinos in their flux -- are, individually, rewarding observables. Combined, they offer new opportunities, hitherto unexplored, that we expose for the first time. Anisotropy in the arrival directions of electron, muon, and tau neutrinos may reveal multiple populations of neutrino sources, differently distributed in the sky, and test whether neutrinos of different flavor pro"},"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":"2310.15224","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-10-23T18:00:01Z","cross_cats_sorted":["hep-ex","hep-ph","hep-th"],"title_canon_sha256":"249052385ba50c231e17797fb4290986a0beda0cafb92381cf8595e3b31566cb","abstract_canon_sha256":"c73c80047c65d2fb3bca916d489fa487d75a1310727aa2c5251d83b4f2c83b44"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:01:10.349919Z","signature_b64":"+uBfZWEir+3c9fWj7He2DTsrGAJe2uL7a0Qv6UqFkLgPigkv5lWADo32LxlltwU4qz5gdV65CFL7loGLm8D2Ag==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"25d321b6e73c3b26e97eba2adab69e8af27a2facd62c23475fedc644af9f28a0","last_reissued_at":"2026-07-05T10:01:10.349360Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:01:10.349360Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Flavor Anisotropy in the High-Energy Astrophysical Neutrino Sky","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ex","hep-ph","hep-th"],"primary_cat":"astro-ph.HE","authors_text":"Bernanda Telalovic, Mauricio Bustamante","submitted_at":"2023-10-23T18:00:01Z","abstract_excerpt":"High-energy astrophysical neutrinos, with TeV--PeV energies, offer unique insight into astrophysics and particle physics. Their incoming directions and flavor composition -- i.e., the proportion of electron, muon, and tau neutrinos in their flux -- are, individually, rewarding observables. Combined, they offer new opportunities, hitherto unexplored, that we expose for the first time. Anisotropy in the arrival directions of electron, muon, and tau neutrinos may reveal multiple populations of neutrino sources, differently distributed in the sky, and test whether neutrinos of different flavor pro"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2310.15224","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/2310.15224/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":"2310.15224","created_at":"2026-07-05T10:01:10.349431+00:00"},{"alias_kind":"arxiv_version","alias_value":"2310.15224v2","created_at":"2026-07-05T10:01:10.349431+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2310.15224","created_at":"2026-07-05T10:01:10.349431+00:00"},{"alias_kind":"pith_short_12","alias_value":"EXJSDNXHHQ5S","created_at":"2026-07-05T10:01:10.349431+00:00"},{"alias_kind":"pith_short_16","alias_value":"EXJSDNXHHQ5SN2L6","created_at":"2026-07-05T10:01:10.349431+00:00"},{"alias_kind":"pith_short_8","alias_value":"EXJSDNXH","created_at":"2026-07-05T10:01:10.349431+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2607.01339","citing_title":"Electron stability constrains neutrino time delays","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2606.17132","citing_title":"Are neutrinos Majorana? Fixed-target and high-energy astrophysical searches decide","ref_index":53,"is_internal_anchor":false},{"citing_arxiv_id":"2604.19880","citing_title":"Ultra-High-Energy Tau Neutrinos as Probes of Lorentz Invariance","ref_index":22,"is_internal_anchor":false},{"citing_arxiv_id":"2604.14409","citing_title":"Astrophysical bounds on the high-energy evolution of neutrino mixing","ref_index":62,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL","json":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL.json","graph_json":"https://pith.science/api/pith-number/EXJSDNXHHQ5SN2L6XIVNVNU6RL/graph.json","events_json":"https://pith.science/api/pith-number/EXJSDNXHHQ5SN2L6XIVNVNU6RL/events.json","paper":"https://pith.science/paper/EXJSDNXH"},"agent_actions":{"view_html":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL","download_json":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL.json","view_paper":"https://pith.science/paper/EXJSDNXH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2310.15224&json=true","fetch_graph":"https://pith.science/api/pith-number/EXJSDNXHHQ5SN2L6XIVNVNU6RL/graph.json","fetch_events":"https://pith.science/api/pith-number/EXJSDNXHHQ5SN2L6XIVNVNU6RL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL/action/storage_attestation","attest_author":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL/action/author_attestation","sign_citation":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL/action/citation_signature","submit_replication":"https://pith.science/pith/EXJSDNXHHQ5SN2L6XIVNVNU6RL/action/replication_record"}},"created_at":"2026-07-05T10:01:10.349431+00:00","updated_at":"2026-07-05T10:01:10.349431+00:00"}