{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:ECUOPQNWHIOODHIAYWVCR45D6A","short_pith_number":"pith:ECUOPQNW","schema_version":"1.0","canonical_sha256":"20a8e7c1b63a1ce19d00c5aa28f3a3f0109e6887735e06fbeb3b01fdf454f398","source":{"kind":"arxiv","id":"2404.18595","version":1},"attestation_state":"computed","paper":{"title":"The population of Galactic supernova remnants in the TeV range","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Constantin Steppa, Dominique Meyer, Kathrin Egberts, Pierre Cristofari, Rowan Batzofin","submitted_at":"2024-04-29T11:11:00Z","abstract_excerpt":"Supernova remnants (SNRs) are likely to be significant sources of cosmic rays up to the knee of the local cosmic-ray (CR) spectrum. They produce gamma-rays in the very-high-energy (VHE) ($E>0.1$ TeV) range via: hadronic interactions with the interstellar medium and leptonic interactions with soft photons. Current observations have lead to the detection of about a dozen of VHE SNRs and future instruments should increase this number. The details of particle acceleration at SNRs, and of the mechanisms producing VHE gamma-rays at SNRs are poorly understood. We aim to study the population of SNRs d"},"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":"2404.18595","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-04-29T11:11:00Z","cross_cats_sorted":[],"title_canon_sha256":"719373065587b1c14284cdbc1733bf6f81bcaff381848d3d704481b2ea0daf92","abstract_canon_sha256":"8bfd44bd7e4d83b6414d338e154f2ff07c3c98ff16219f8c47aca96c12170c40"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:47:19.412477Z","signature_b64":"8oXilM6I/Omk+L4+ZQp6AtLxwJrwfCg+AOuU7fY0Kq9P9xCTSODDDELKhW8PdEs6xiylIE8TF6gNwwc8UjyCCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"20a8e7c1b63a1ce19d00c5aa28f3a3f0109e6887735e06fbeb3b01fdf454f398","last_reissued_at":"2026-07-05T08:47:19.411968Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:47:19.411968Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The population of Galactic supernova remnants in the TeV range","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Constantin Steppa, Dominique Meyer, Kathrin Egberts, Pierre Cristofari, Rowan Batzofin","submitted_at":"2024-04-29T11:11:00Z","abstract_excerpt":"Supernova remnants (SNRs) are likely to be significant sources of cosmic rays up to the knee of the local cosmic-ray (CR) spectrum. They produce gamma-rays in the very-high-energy (VHE) ($E>0.1$ TeV) range via: hadronic interactions with the interstellar medium and leptonic interactions with soft photons. Current observations have lead to the detection of about a dozen of VHE SNRs and future instruments should increase this number. The details of particle acceleration at SNRs, and of the mechanisms producing VHE gamma-rays at SNRs are poorly understood. We aim to study the population of SNRs d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2404.18595","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/2404.18595/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":"2404.18595","created_at":"2026-07-05T08:47:19.412026+00:00"},{"alias_kind":"arxiv_version","alias_value":"2404.18595v1","created_at":"2026-07-05T08:47:19.412026+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2404.18595","created_at":"2026-07-05T08:47:19.412026+00:00"},{"alias_kind":"pith_short_12","alias_value":"ECUOPQNWHIOO","created_at":"2026-07-05T08:47:19.412026+00:00"},{"alias_kind":"pith_short_16","alias_value":"ECUOPQNWHIOODHIA","created_at":"2026-07-05T08:47:19.412026+00:00"},{"alias_kind":"pith_short_8","alias_value":"ECUOPQNW","created_at":"2026-07-05T08:47:19.412026+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.11485","citing_title":"Superdiffusion of cosmic rays in the vicinity of their accelerators and the resulting $\\gamma$-ray emission","ref_index":57,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A","json":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A.json","graph_json":"https://pith.science/api/pith-number/ECUOPQNWHIOODHIAYWVCR45D6A/graph.json","events_json":"https://pith.science/api/pith-number/ECUOPQNWHIOODHIAYWVCR45D6A/events.json","paper":"https://pith.science/paper/ECUOPQNW"},"agent_actions":{"view_html":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A","download_json":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A.json","view_paper":"https://pith.science/paper/ECUOPQNW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2404.18595&json=true","fetch_graph":"https://pith.science/api/pith-number/ECUOPQNWHIOODHIAYWVCR45D6A/graph.json","fetch_events":"https://pith.science/api/pith-number/ECUOPQNWHIOODHIAYWVCR45D6A/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A/action/storage_attestation","attest_author":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A/action/author_attestation","sign_citation":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A/action/citation_signature","submit_replication":"https://pith.science/pith/ECUOPQNWHIOODHIAYWVCR45D6A/action/replication_record"}},"created_at":"2026-07-05T08:47:19.412026+00:00","updated_at":"2026-07-05T08:47:19.412026+00:00"}