{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:M757Y63NH7QSGJJIDL2FQPQXUO","short_pith_number":"pith:M757Y63N","schema_version":"1.0","canonical_sha256":"67fbfc7b6d3fe12325281af4583e17a3a5ff80bb159d8f1ae65d72f2cee711c1","source":{"kind":"arxiv","id":"1301.5644","version":3},"attestation_state":"computed","paper":{"title":"Giant radio relics in galaxy clusters: reacceleration of fossil relativistic electrons?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"Anders Pinzke, Christoph Pfrommer, S. Peng Oh","submitted_at":"2013-01-23T21:01:11Z","abstract_excerpt":"Many bright radio relics in the outskirts of galaxy clusters have low inferred Mach numbers, defying expectations from shock acceleration theory and heliospheric observations that the injection efficiency of relativistic particles plummets at low Mach numbers. With a suite of cosmological simulations, we follow the diffusive shock acceleration as well as radiative and Coulomb cooling of cosmic ray electrons during the assembly of a cluster. We find a substantial population of fossil electrons. When reaccelerated at a shock (through diffusive shock acceleration), they are competitive with direc"},"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":"1301.5644","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-01-23T21:01:11Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"f3afdcfa62ab46c157fe4f1e981755d1f04d682dc4b854fc6524cc6f7260238a","abstract_canon_sha256":"12d80e9e10ba8e4f1ee76296e08ec1b367ca453a10b4fe93ca86c02436bb18bf"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:14:27.997481Z","signature_b64":"Vu6JNycRVM24Uv9ZnHXTFv5BijpWApu2zvWQaK2xipzUSA/8tC+2zYY43P6ZMBTiGAkAs2ICMYXVp/aeDNWICg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"67fbfc7b6d3fe12325281af4583e17a3a5ff80bb159d8f1ae65d72f2cee711c1","last_reissued_at":"2026-05-18T03:14:27.996900Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:14:27.996900Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Giant radio relics in galaxy clusters: reacceleration of fossil relativistic electrons?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"Anders Pinzke, Christoph Pfrommer, S. Peng Oh","submitted_at":"2013-01-23T21:01:11Z","abstract_excerpt":"Many bright radio relics in the outskirts of galaxy clusters have low inferred Mach numbers, defying expectations from shock acceleration theory and heliospheric observations that the injection efficiency of relativistic particles plummets at low Mach numbers. With a suite of cosmological simulations, we follow the diffusive shock acceleration as well as radiative and Coulomb cooling of cosmic ray electrons during the assembly of a cluster. We find a substantial population of fossil electrons. When reaccelerated at a shock (through diffusive shock acceleration), they are competitive with direc"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1301.5644","kind":"arxiv","version":3},"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":"1301.5644","created_at":"2026-05-18T03:14:27.996997+00:00"},{"alias_kind":"arxiv_version","alias_value":"1301.5644v3","created_at":"2026-05-18T03:14:27.996997+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1301.5644","created_at":"2026-05-18T03:14:27.996997+00:00"},{"alias_kind":"pith_short_12","alias_value":"M757Y63NH7QS","created_at":"2026-05-18T12:27:51.066281+00:00"},{"alias_kind":"pith_short_16","alias_value":"M757Y63NH7QSGJJI","created_at":"2026-05-18T12:27:51.066281+00:00"},{"alias_kind":"pith_short_8","alias_value":"M757Y63N","created_at":"2026-05-18T12:27:51.066281+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2607.07750","citing_title":"Multi-Wavelength Signatures of a Giant Cometary Radio Halo in MACSJ0417-1154","ref_index":289,"is_internal_anchor":true},{"citing_arxiv_id":"2606.04084","citing_title":"Simulating realistic radio morphologies of Fanaroff-Riley I jets in a self-regulating cool-core cluster","ref_index":254,"is_internal_anchor":true},{"citing_arxiv_id":"2606.24738","citing_title":"Probing Merger Shocks in Galaxy Clusters in the SKA Era","ref_index":62,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15264","citing_title":"Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization","ref_index":254,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO","json":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO.json","graph_json":"https://pith.science/api/pith-number/M757Y63NH7QSGJJIDL2FQPQXUO/graph.json","events_json":"https://pith.science/api/pith-number/M757Y63NH7QSGJJIDL2FQPQXUO/events.json","paper":"https://pith.science/paper/M757Y63N"},"agent_actions":{"view_html":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO","download_json":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO.json","view_paper":"https://pith.science/paper/M757Y63N","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1301.5644&json=true","fetch_graph":"https://pith.science/api/pith-number/M757Y63NH7QSGJJIDL2FQPQXUO/graph.json","fetch_events":"https://pith.science/api/pith-number/M757Y63NH7QSGJJIDL2FQPQXUO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO/action/storage_attestation","attest_author":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO/action/author_attestation","sign_citation":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO/action/citation_signature","submit_replication":"https://pith.science/pith/M757Y63NH7QSGJJIDL2FQPQXUO/action/replication_record"}},"created_at":"2026-05-18T03:14:27.996997+00:00","updated_at":"2026-05-18T03:14:27.996997+00:00"}