{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:KTVHKSSTOGRTQWBLQKLDYX234D","short_pith_number":"pith:KTVHKSST","schema_version":"1.0","canonical_sha256":"54ea754a5371a338582b82963c5f5be0ea68e7721686b1c4771fa15146a8671c","source":{"kind":"arxiv","id":"1306.3417","version":3},"attestation_state":"computed","paper":{"title":"Testing the Hadronuclear Origin of PeV Neutrinos Observed with IceCube","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Brian C. Lacki (IAS), Kohta Murase (IAS), Markus Ahlers (UW-Madison)","submitted_at":"2013-06-14T14:58:59Z","abstract_excerpt":"We consider implications of the IceCube excess for hadronuclear (pp) scenarios of neutrino sources such as galaxy clusters/groups and star-forming galaxies. Since the observed neutrino flux is comparable to the diffuse gamma-ray background flux obtained by Fermi, we place new, strong upper limits on the source spectral index, {\\Gamma}<2.1-2.2. In addition, the new IceCube data imply that these sources contribute at least 30%-40% of the diffuse gamma-ray background in the 100 GeV range and even ~100% for softer spectra. Our results, which are insensitive to details of the pp source models, are "},"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":"1306.3417","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2013-06-14T14:58:59Z","cross_cats_sorted":["astro-ph.CO","hep-ph"],"title_canon_sha256":"dfb7777ada7c6eda56a69b018bbc026b36b3a41d7e1a40c57a6d3003afbe1195","abstract_canon_sha256":"d7c16ebd92dad5982a7d9df8a76a139c0eb1ed1262a167be01260f4adcf1ade0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:03:54.719250Z","signature_b64":"S6+00wDyY7lVgLrErPne6+Lu+aIKuINkR+uS2hIB9lBJ8GMMGjQkXUdE2GJRqVJL7FhtC6bZMecoXC0Yr/BrAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"54ea754a5371a338582b82963c5f5be0ea68e7721686b1c4771fa15146a8671c","last_reissued_at":"2026-05-18T03:03:54.718737Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:03:54.718737Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Testing the Hadronuclear Origin of PeV Neutrinos Observed with IceCube","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Brian C. Lacki (IAS), Kohta Murase (IAS), Markus Ahlers (UW-Madison)","submitted_at":"2013-06-14T14:58:59Z","abstract_excerpt":"We consider implications of the IceCube excess for hadronuclear (pp) scenarios of neutrino sources such as galaxy clusters/groups and star-forming galaxies. Since the observed neutrino flux is comparable to the diffuse gamma-ray background flux obtained by Fermi, we place new, strong upper limits on the source spectral index, {\\Gamma}<2.1-2.2. In addition, the new IceCube data imply that these sources contribute at least 30%-40% of the diffuse gamma-ray background in the 100 GeV range and even ~100% for softer spectra. Our results, which are insensitive to details of the pp source models, are "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1306.3417","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":""},"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":"1306.3417","created_at":"2026-05-18T03:03:54.718818+00:00"},{"alias_kind":"arxiv_version","alias_value":"1306.3417v3","created_at":"2026-05-18T03:03:54.718818+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1306.3417","created_at":"2026-05-18T03:03:54.718818+00:00"},{"alias_kind":"pith_short_12","alias_value":"KTVHKSSTOGRT","created_at":"2026-05-18T12:27:51.066281+00:00"},{"alias_kind":"pith_short_16","alias_value":"KTVHKSSTOGRTQWBL","created_at":"2026-05-18T12:27:51.066281+00:00"},{"alias_kind":"pith_short_8","alias_value":"KTVHKSST","created_at":"2026-05-18T12:27:51.066281+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"1907.11926","citing_title":"Potential Dark Matter Signals at Neutrino Telescopes","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"2404.15944","citing_title":"IceCube Results and Perspective for Neutrinos from LHAASO Sources","ref_index":30,"is_internal_anchor":true},{"citing_arxiv_id":"2603.15754","citing_title":"Single-source-class interpretation of the diffuse astrophysical neutrino flux","ref_index":53,"is_internal_anchor":true},{"citing_arxiv_id":"2512.00660","citing_title":"Particle Astrophysics with High and Ultrahigh Energy Neutrinos","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2601.11203","citing_title":"Little Red Dots as Hidden Neutrino Sources","ref_index":61,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D","json":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D.json","graph_json":"https://pith.science/api/pith-number/KTVHKSSTOGRTQWBLQKLDYX234D/graph.json","events_json":"https://pith.science/api/pith-number/KTVHKSSTOGRTQWBLQKLDYX234D/events.json","paper":"https://pith.science/paper/KTVHKSST"},"agent_actions":{"view_html":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D","download_json":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D.json","view_paper":"https://pith.science/paper/KTVHKSST","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1306.3417&json=true","fetch_graph":"https://pith.science/api/pith-number/KTVHKSSTOGRTQWBLQKLDYX234D/graph.json","fetch_events":"https://pith.science/api/pith-number/KTVHKSSTOGRTQWBLQKLDYX234D/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D/action/storage_attestation","attest_author":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D/action/author_attestation","sign_citation":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D/action/citation_signature","submit_replication":"https://pith.science/pith/KTVHKSSTOGRTQWBLQKLDYX234D/action/replication_record"}},"created_at":"2026-05-18T03:03:54.718818+00:00","updated_at":"2026-05-18T03:03:54.718818+00:00"}