{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:OWVTBAM5KXA7ADXY4JWFXB54ZH","short_pith_number":"pith:OWVTBAM5","schema_version":"1.0","canonical_sha256":"75ab30819d55c1f00ef8e26c5b87bcc9fa935ba63daa415e38e7efd65683687a","source":{"kind":"arxiv","id":"1603.05137","version":1},"attestation_state":"computed","paper":{"title":"The environment of the gamma-ray emitting SNR G338.3-0.0: a hadronic interpretation for HESS J1640-465","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A. D. Supanitsky, G. Castelletti, L. Supan","submitted_at":"2016-03-16T15:06:51Z","abstract_excerpt":"The supernova remnant (SNR) G338.3-0.0 spatially correlates with HESS J1640-465, which is considered the most luminous gamma-ray source associated with a SNR in our Galaxy. The X-ray pulsar PSR J1640-4631 has been recently discovered within the SNR shell, which could favor a leptonic origin for the detected very-high energy (VHE) emission. In spite of this, the origin of the VHE radiation from HESS J1640-465 has not been unambiguously clarified so far. Indeed, a hadronic explanation cannot be ruled out by current observations. On the basis of atomic (HI) and molecular (12^CO) archival data, we"},"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":"1603.05137","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2016-03-16T15:06:51Z","cross_cats_sorted":[],"title_canon_sha256":"a1f7a53f8dd7ffeebe285ff4e8d273db0a6a6792f3f4a845ad6dd2484c69f2ea","abstract_canon_sha256":"934789d8c5f395a22d01ffbad0b65a2f2043069ceed53616ac0a7a79a8dfffe4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:17:16.879752Z","signature_b64":"fXjsROMdV05f/Bcw1gBY0jqOb7nzu3OYoxXVXVQqsE6165xvu579b4M8leUj5Vf0bj2jf/eXDE8K+6jLf5c/Ag==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"75ab30819d55c1f00ef8e26c5b87bcc9fa935ba63daa415e38e7efd65683687a","last_reissued_at":"2026-05-18T01:17:16.879193Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:17:16.879193Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The environment of the gamma-ray emitting SNR G338.3-0.0: a hadronic interpretation for HESS J1640-465","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A. D. Supanitsky, G. Castelletti, L. Supan","submitted_at":"2016-03-16T15:06:51Z","abstract_excerpt":"The supernova remnant (SNR) G338.3-0.0 spatially correlates with HESS J1640-465, which is considered the most luminous gamma-ray source associated with a SNR in our Galaxy. The X-ray pulsar PSR J1640-4631 has been recently discovered within the SNR shell, which could favor a leptonic origin for the detected very-high energy (VHE) emission. In spite of this, the origin of the VHE radiation from HESS J1640-465 has not been unambiguously clarified so far. Indeed, a hadronic explanation cannot be ruled out by current observations. On the basis of atomic (HI) and molecular (12^CO) archival data, we"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1603.05137","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":""},"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":"1603.05137","created_at":"2026-05-18T01:17:16.879278+00:00"},{"alias_kind":"arxiv_version","alias_value":"1603.05137v1","created_at":"2026-05-18T01:17:16.879278+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1603.05137","created_at":"2026-05-18T01:17:16.879278+00:00"},{"alias_kind":"pith_short_12","alias_value":"OWVTBAM5KXA7","created_at":"2026-05-18T12:30:36.002864+00:00"},{"alias_kind":"pith_short_16","alias_value":"OWVTBAM5KXA7ADXY","created_at":"2026-05-18T12:30:36.002864+00:00"},{"alias_kind":"pith_short_8","alias_value":"OWVTBAM5","created_at":"2026-05-18T12:30:36.002864+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2601.00692","citing_title":"Hadronic Origin of Sub-PeV Gamma-Ray Emission from LHAASO J0621+3755","ref_index":10,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH","json":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH.json","graph_json":"https://pith.science/api/pith-number/OWVTBAM5KXA7ADXY4JWFXB54ZH/graph.json","events_json":"https://pith.science/api/pith-number/OWVTBAM5KXA7ADXY4JWFXB54ZH/events.json","paper":"https://pith.science/paper/OWVTBAM5"},"agent_actions":{"view_html":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH","download_json":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH.json","view_paper":"https://pith.science/paper/OWVTBAM5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1603.05137&json=true","fetch_graph":"https://pith.science/api/pith-number/OWVTBAM5KXA7ADXY4JWFXB54ZH/graph.json","fetch_events":"https://pith.science/api/pith-number/OWVTBAM5KXA7ADXY4JWFXB54ZH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH/action/storage_attestation","attest_author":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH/action/author_attestation","sign_citation":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH/action/citation_signature","submit_replication":"https://pith.science/pith/OWVTBAM5KXA7ADXY4JWFXB54ZH/action/replication_record"}},"created_at":"2026-05-18T01:17:16.879278+00:00","updated_at":"2026-05-18T01:17:16.879278+00:00"}