{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:PO7X2BNPUYTGW5L6GKJX7MZ3C4","short_pith_number":"pith:PO7X2BNP","schema_version":"1.0","canonical_sha256":"7bbf7d05afa6266b757e32937fb33b17100ccd6b0f716a192fd03c1428ef7d5d","source":{"kind":"arxiv","id":"2108.02232","version":1},"attestation_state":"computed","paper":{"title":"Detection of new Extreme BL Lac objects with H.E.S.S. and Swift XRT","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Angel Priyana Noel, David A. Sanchez (for the H.E.S.S., Fermi-LAT Collaborations), Manuel Meyer, Mathieu de Bony de Lavergne, Tomas Bylund","submitted_at":"2021-08-04T18:24:16Z","abstract_excerpt":"Extreme high synchrotron peaked blazars (EHBLs) are amongst the most powerful accelerators found in nature. Usually the synchrotron peak frequency of an EHBL is above $10^{17}\\,$Hz, i.e., lies in the range of medium to hard X-rays making them ideal sources to study particle acceleration and radiative processes. EHBL objects are commonly observed at energies beyond several TeV, making them also powerful probes of gamma-ray absorption in the intergalactic medium. During the last decade, several attempts have been made to increase the number of EHBL detected at TeV energies and probe their spectr"},"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":"2108.02232","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-08-04T18:24:16Z","cross_cats_sorted":[],"title_canon_sha256":"7d9c49bc0303d46c13400666756a58e43587c70e6a8229dcf8cdc3a51800479b","abstract_canon_sha256":"2e7f5eec4c6c1d1c6229b03cfb5ce09bbc4f18d78603da10f378ae9474f7b8cb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:59:13.039584Z","signature_b64":"y5/Oi/kWKDgraORdPjYnXuh7nZfjn8Y6S7zpOEp/BhwN+uH1h3zLrjvnH47rL8/mdx2+jS1qSXCSlJ4dcm55Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7bbf7d05afa6266b757e32937fb33b17100ccd6b0f716a192fd03c1428ef7d5d","last_reissued_at":"2026-07-05T04:59:13.039153Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:59:13.039153Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Detection of new Extreme BL Lac objects with H.E.S.S. and Swift XRT","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Angel Priyana Noel, David A. Sanchez (for the H.E.S.S., Fermi-LAT Collaborations), Manuel Meyer, Mathieu de Bony de Lavergne, Tomas Bylund","submitted_at":"2021-08-04T18:24:16Z","abstract_excerpt":"Extreme high synchrotron peaked blazars (EHBLs) are amongst the most powerful accelerators found in nature. Usually the synchrotron peak frequency of an EHBL is above $10^{17}\\,$Hz, i.e., lies in the range of medium to hard X-rays making them ideal sources to study particle acceleration and radiative processes. EHBL objects are commonly observed at energies beyond several TeV, making them also powerful probes of gamma-ray absorption in the intergalactic medium. During the last decade, several attempts have been made to increase the number of EHBL detected at TeV energies and probe their spectr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2108.02232","kind":"arxiv","version":1},"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/2108.02232/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":"2108.02232","created_at":"2026-07-05T04:59:13.039211+00:00"},{"alias_kind":"arxiv_version","alias_value":"2108.02232v1","created_at":"2026-07-05T04:59:13.039211+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2108.02232","created_at":"2026-07-05T04:59:13.039211+00:00"},{"alias_kind":"pith_short_12","alias_value":"PO7X2BNPUYTG","created_at":"2026-07-05T04:59:13.039211+00:00"},{"alias_kind":"pith_short_16","alias_value":"PO7X2BNPUYTGW5L6","created_at":"2026-07-05T04:59:13.039211+00:00"},{"alias_kind":"pith_short_8","alias_value":"PO7X2BNP","created_at":"2026-07-05T04:59:13.039211+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.10407","citing_title":"Fermi-Large Area Telescope Detection of Very High Energy (>100 GeV) Emission from Compton-Dominated Blazars","ref_index":94,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4","json":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4.json","graph_json":"https://pith.science/api/pith-number/PO7X2BNPUYTGW5L6GKJX7MZ3C4/graph.json","events_json":"https://pith.science/api/pith-number/PO7X2BNPUYTGW5L6GKJX7MZ3C4/events.json","paper":"https://pith.science/paper/PO7X2BNP"},"agent_actions":{"view_html":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4","download_json":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4.json","view_paper":"https://pith.science/paper/PO7X2BNP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2108.02232&json=true","fetch_graph":"https://pith.science/api/pith-number/PO7X2BNPUYTGW5L6GKJX7MZ3C4/graph.json","fetch_events":"https://pith.science/api/pith-number/PO7X2BNPUYTGW5L6GKJX7MZ3C4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4/action/storage_attestation","attest_author":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4/action/author_attestation","sign_citation":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4/action/citation_signature","submit_replication":"https://pith.science/pith/PO7X2BNPUYTGW5L6GKJX7MZ3C4/action/replication_record"}},"created_at":"2026-07-05T04:59:13.039211+00:00","updated_at":"2026-07-05T04:59:13.039211+00:00"}