{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:QXUNHPF4GPMJMLDPCQRSKPPPI2","short_pith_number":"pith:QXUNHPF4","schema_version":"1.0","canonical_sha256":"85e8d3bcbc33d8962c6f1423253def46ade30416a1b9ceff20f4e19ef4f73e18","source":{"kind":"arxiv","id":"1906.02725","version":1},"attestation_state":"computed","paper":{"title":"Non-thermal emission from the reverse shock of the youngest galactic Supernova remnant G1.9+0.3","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"I. Sushch, K. J. Luken, M. D. Filipovic, M. Pohl, R. Brose, R. Lin","submitted_at":"2019-06-06T17:48:38Z","abstract_excerpt":"Context. The youngest Galactic supernova remnant G1.9+0.3 is an interesting target for next generation gamma-ray observatories. So far, the remnant is only detected in the radio and the X-ray bands, but its young age of ~100 yrs and inferred shock speed of ~14,000 km/s could make it an efficient particle accelerator. Aims. We aim to model the observed radio and X-ray spectra together with the morphology of the remnant. At the same time, we aim to estimate the gamma-ray flux from the source and evaluated the prospects of its detection with future gamma-ray experiments. Methods. We performed sph"},"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":"1906.02725","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2019-06-06T17:48:38Z","cross_cats_sorted":[],"title_canon_sha256":"f5586f9379d0065b382f7416c1781650e493c4990cf43815559c36c60896f212","abstract_canon_sha256":"98353f6cb15b0be12457f674783e8330d966003b0d5ab17926882c4c284640a4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:39:43.247367Z","signature_b64":"3LeMajT/SIO8IhIEVZEQ7ktqjjC3xxZFFMe3q3BLr6rNmJXlYJ3S7tN05SojR+sH2R08WYGbfP+wZwIz7/PmBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"85e8d3bcbc33d8962c6f1423253def46ade30416a1b9ceff20f4e19ef4f73e18","last_reissued_at":"2026-05-17T23:39:43.246698Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:39:43.246698Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Non-thermal emission from the reverse shock of the youngest galactic Supernova remnant G1.9+0.3","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"I. Sushch, K. J. Luken, M. D. Filipovic, M. Pohl, R. Brose, R. Lin","submitted_at":"2019-06-06T17:48:38Z","abstract_excerpt":"Context. The youngest Galactic supernova remnant G1.9+0.3 is an interesting target for next generation gamma-ray observatories. So far, the remnant is only detected in the radio and the X-ray bands, but its young age of ~100 yrs and inferred shock speed of ~14,000 km/s could make it an efficient particle accelerator. Aims. We aim to model the observed radio and X-ray spectra together with the morphology of the remnant. At the same time, we aim to estimate the gamma-ray flux from the source and evaluated the prospects of its detection with future gamma-ray experiments. Methods. We performed sph"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1906.02725","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":"1906.02725","created_at":"2026-05-17T23:39:43.246801+00:00"},{"alias_kind":"arxiv_version","alias_value":"1906.02725v1","created_at":"2026-05-17T23:39:43.246801+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1906.02725","created_at":"2026-05-17T23:39:43.246801+00:00"},{"alias_kind":"pith_short_12","alias_value":"QXUNHPF4GPMJ","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_16","alias_value":"QXUNHPF4GPMJMLDP","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_8","alias_value":"QXUNHPF4","created_at":"2026-05-18T12:33:27.125529+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.18703","citing_title":"SAETASS: Solver for Astroparticle Equation of Transport Analysis in Spherical Symmetry","ref_index":17,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2","json":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2.json","graph_json":"https://pith.science/api/pith-number/QXUNHPF4GPMJMLDPCQRSKPPPI2/graph.json","events_json":"https://pith.science/api/pith-number/QXUNHPF4GPMJMLDPCQRSKPPPI2/events.json","paper":"https://pith.science/paper/QXUNHPF4"},"agent_actions":{"view_html":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2","download_json":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2.json","view_paper":"https://pith.science/paper/QXUNHPF4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1906.02725&json=true","fetch_graph":"https://pith.science/api/pith-number/QXUNHPF4GPMJMLDPCQRSKPPPI2/graph.json","fetch_events":"https://pith.science/api/pith-number/QXUNHPF4GPMJMLDPCQRSKPPPI2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2/action/storage_attestation","attest_author":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2/action/author_attestation","sign_citation":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2/action/citation_signature","submit_replication":"https://pith.science/pith/QXUNHPF4GPMJMLDPCQRSKPPPI2/action/replication_record"}},"created_at":"2026-05-17T23:39:43.246801+00:00","updated_at":"2026-05-17T23:39:43.246801+00:00"}