{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:YLWSUSUBYK2IOQDVJVRKVIBNA5","short_pith_number":"pith:YLWSUSUB","schema_version":"1.0","canonical_sha256":"c2ed2a4a81c2b48740754d62aaa02d07405445fc2ee2ee4ca5a2a6ea5438de80","source":{"kind":"arxiv","id":"2111.06940","version":2},"attestation_state":"computed","paper":{"title":"MeerKAT view of the diffuse radio sources in Abell 3667 and their interactions with the thermal plasma","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Finoguenov, D. Wittor, F. De Gasperin, H. Akamatsu, J. O. Chibueze, K. Knowles, L. Rudnick, L. Sebokolodi, M. Bruggen, P. Dominguez-Fernandez, S. P. O'Sullivan, T. E. Clarke, V. Cuciti, W. Cotton","submitted_at":"2021-11-12T20:53:48Z","abstract_excerpt":"During their lifetime, galaxy clusters grow through the accretion of matter from the filaments of the large scale structure and from mergers with other clusters. These mergers release a large amount of energy into the intracluster medium (ICM) through merger shocks and turbulence. These phenomena are associated with the formation of radio sources known as radio relics and radio halos, respectively. Radio relics and halos are unique proxies to study the complex properties of these dynamically active regions of clusters and in general the micro physics of the ICM. Abell 3667 is a spectacular exa"},"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":"2111.06940","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2021-11-12T20:53:48Z","cross_cats_sorted":[],"title_canon_sha256":"c6ccccfdd9b937cdcddb37870fad73b9678ec31db998665366d68c31e7f68ec6","abstract_canon_sha256":"58a2510f179ce3023ecf358b7819f1cd002741be77f371948fab5f48ee73f9b7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:07:27.663370Z","signature_b64":"zpRLmwYJ8hJBi6YWAHjm/1Z2pB/9yrBzllGkuElECR9N5cki6Xz4dB4CLR1ffD0rYkG76hPQfU1wR9+MfS9KAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c2ed2a4a81c2b48740754d62aaa02d07405445fc2ee2ee4ca5a2a6ea5438de80","last_reissued_at":"2026-07-05T04:07:27.662882Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:07:27.662882Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"MeerKAT view of the diffuse radio sources in Abell 3667 and their interactions with the thermal plasma","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Finoguenov, D. Wittor, F. De Gasperin, H. Akamatsu, J. O. Chibueze, K. Knowles, L. Rudnick, L. Sebokolodi, M. Bruggen, P. Dominguez-Fernandez, S. P. O'Sullivan, T. E. Clarke, V. Cuciti, W. Cotton","submitted_at":"2021-11-12T20:53:48Z","abstract_excerpt":"During their lifetime, galaxy clusters grow through the accretion of matter from the filaments of the large scale structure and from mergers with other clusters. These mergers release a large amount of energy into the intracluster medium (ICM) through merger shocks and turbulence. These phenomena are associated with the formation of radio sources known as radio relics and radio halos, respectively. Radio relics and halos are unique proxies to study the complex properties of these dynamically active regions of clusters and in general the micro physics of the ICM. Abell 3667 is a spectacular exa"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2111.06940","kind":"arxiv","version":2},"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/2111.06940/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":"2111.06940","created_at":"2026-07-05T04:07:27.662944+00:00"},{"alias_kind":"arxiv_version","alias_value":"2111.06940v2","created_at":"2026-07-05T04:07:27.662944+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2111.06940","created_at":"2026-07-05T04:07:27.662944+00:00"},{"alias_kind":"pith_short_12","alias_value":"YLWSUSUBYK2I","created_at":"2026-07-05T04:07:27.662944+00:00"},{"alias_kind":"pith_short_16","alias_value":"YLWSUSUBYK2IOQDV","created_at":"2026-07-05T04:07:27.662944+00:00"},{"alias_kind":"pith_short_8","alias_value":"YLWSUSUB","created_at":"2026-07-05T04:07:27.662944+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.07750","citing_title":"Multi-Wavelength Signatures of a Giant Cometary Radio Halo in MACSJ0417-1154","ref_index":280,"is_internal_anchor":true},{"citing_arxiv_id":"2607.06346","citing_title":"Unravelling Turbulence and Magnetic Fields in Galaxy Clusters with SKA and XRISM","ref_index":34,"is_internal_anchor":true},{"citing_arxiv_id":"2605.20779","citing_title":"A MINOT-based Study of Gamma-ray emission from SPT-CL J2012-5649/Abell 3667","ref_index":61,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5","json":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5.json","graph_json":"https://pith.science/api/pith-number/YLWSUSUBYK2IOQDVJVRKVIBNA5/graph.json","events_json":"https://pith.science/api/pith-number/YLWSUSUBYK2IOQDVJVRKVIBNA5/events.json","paper":"https://pith.science/paper/YLWSUSUB"},"agent_actions":{"view_html":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5","download_json":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5.json","view_paper":"https://pith.science/paper/YLWSUSUB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2111.06940&json=true","fetch_graph":"https://pith.science/api/pith-number/YLWSUSUBYK2IOQDVJVRKVIBNA5/graph.json","fetch_events":"https://pith.science/api/pith-number/YLWSUSUBYK2IOQDVJVRKVIBNA5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5/action/storage_attestation","attest_author":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5/action/author_attestation","sign_citation":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5/action/citation_signature","submit_replication":"https://pith.science/pith/YLWSUSUBYK2IOQDVJVRKVIBNA5/action/replication_record"}},"created_at":"2026-07-05T04:07:27.662944+00:00","updated_at":"2026-07-05T04:07:27.662944+00:00"}