{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:USYW4NSMDUU562TAS454ZC3VYO","short_pith_number":"pith:USYW4NSM","schema_version":"1.0","canonical_sha256":"a4b16e364c1d29df6a60973bcc8b75c3a00c955df81f5d97c9e4253d270c9b24","source":{"kind":"arxiv","id":"1107.5576","version":2},"attestation_state":"computed","paper":{"title":"Blazars as Ultra-High-Energy Cosmic-Ray Sources: Implications for TeV Gamma-Ray Observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"Charles D. Dermer, Giulia Migliori, Hajime Takami, Kohta Murase","submitted_at":"2011-07-27T19:57:59Z","abstract_excerpt":"The spectra of BL Lac objects and Fanaroff-Riley I radio galaxies are commonly explained by the one-zone leptonic synchrotron self-Compton (SSC) model. Spectral modeling of correlated multiwavelength data gives the comoving magnetic field strength, the bulk outflow Lorentz factor and the emission region size. Assuming the validity of the SSC model, the Hillas condition shows that only in rare cases can such sources accelerate protons to much above 10^19 eV, so > 10^20 eV ultra-high-energy cosmic rays (UHECRs) are likely to be heavy ions if powered by this type of radio-loud active galactic nuc"},"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":"1107.5576","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2011-07-27T19:57:59Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"e0d69772ea77b50ac43c4adb40e52fc0ff5fc94833ce71fc4e0986ceada75412","abstract_canon_sha256":"84eecfe9ac2f0ccff73ae81e107529e6e52e1cb5fdc0bc55794bfa8c242f0727"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:59:25.396673Z","signature_b64":"VgNLmOeNUZg2MCZ+gk/u2JC0b1/V1lLW9U4IBD9C2p7HkiujUZR2g48aw4bWKx4MhwllaZr6O+RXTfN67lysBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a4b16e364c1d29df6a60973bcc8b75c3a00c955df81f5d97c9e4253d270c9b24","last_reissued_at":"2026-05-18T03:59:25.395961Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:59:25.395961Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Blazars as Ultra-High-Energy Cosmic-Ray Sources: Implications for TeV Gamma-Ray Observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"Charles D. Dermer, Giulia Migliori, Hajime Takami, Kohta Murase","submitted_at":"2011-07-27T19:57:59Z","abstract_excerpt":"The spectra of BL Lac objects and Fanaroff-Riley I radio galaxies are commonly explained by the one-zone leptonic synchrotron self-Compton (SSC) model. Spectral modeling of correlated multiwavelength data gives the comoving magnetic field strength, the bulk outflow Lorentz factor and the emission region size. Assuming the validity of the SSC model, the Hillas condition shows that only in rare cases can such sources accelerate protons to much above 10^19 eV, so > 10^20 eV ultra-high-energy cosmic rays (UHECRs) are likely to be heavy ions if powered by this type of radio-loud active galactic nuc"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1107.5576","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":""},"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":"1107.5576","created_at":"2026-05-18T03:59:25.396082+00:00"},{"alias_kind":"arxiv_version","alias_value":"1107.5576v2","created_at":"2026-05-18T03:59:25.396082+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1107.5576","created_at":"2026-05-18T03:59:25.396082+00:00"},{"alias_kind":"pith_short_12","alias_value":"USYW4NSMDUU5","created_at":"2026-05-18T12:26:42.757692+00:00"},{"alias_kind":"pith_short_16","alias_value":"USYW4NSMDUU562TA","created_at":"2026-05-18T12:26:42.757692+00:00"},{"alias_kind":"pith_short_8","alias_value":"USYW4NSM","created_at":"2026-05-18T12:26:42.757692+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"1907.07737","citing_title":"The Southern Wide-Field Gamma-Ray Observatory (SWGO): A Next-Generation Ground-Based Survey Instrument for VHE Gamma-Ray Astronomy","ref_index":73,"is_internal_anchor":true},{"citing_arxiv_id":"2405.17409","citing_title":"Ultraheavy Ultrahigh-Energy Cosmic Rays","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2511.08153","citing_title":"Study of Flat Spectrum Radio Quasars and BL Lacertae Objects as Sources of Diffusive Ultra High-Energy Cosmic Rays","ref_index":65,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO","json":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO.json","graph_json":"https://pith.science/api/pith-number/USYW4NSMDUU562TAS454ZC3VYO/graph.json","events_json":"https://pith.science/api/pith-number/USYW4NSMDUU562TAS454ZC3VYO/events.json","paper":"https://pith.science/paper/USYW4NSM"},"agent_actions":{"view_html":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO","download_json":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO.json","view_paper":"https://pith.science/paper/USYW4NSM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1107.5576&json=true","fetch_graph":"https://pith.science/api/pith-number/USYW4NSMDUU562TAS454ZC3VYO/graph.json","fetch_events":"https://pith.science/api/pith-number/USYW4NSMDUU562TAS454ZC3VYO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO/action/storage_attestation","attest_author":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO/action/author_attestation","sign_citation":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO/action/citation_signature","submit_replication":"https://pith.science/pith/USYW4NSMDUU562TAS454ZC3VYO/action/replication_record"}},"created_at":"2026-05-18T03:59:25.396082+00:00","updated_at":"2026-05-18T03:59:25.396082+00:00"}