{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:NOTRNUBMM5CXC5D2NOHRNSAZWB","short_pith_number":"pith:NOTRNUBM","schema_version":"1.0","canonical_sha256":"6ba716d02c674571747a6b8f16c819b05a73c9c9bb0959e861f5bcc509a70b72","source":{"kind":"arxiv","id":"1402.0376","version":2},"attestation_state":"computed","paper":{"title":"Impact of local structure on the cosmic radio dipole","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"David Bacon, Dominik J. Schwarz, Matthias Rubart","submitted_at":"2014-02-03T13:13:22Z","abstract_excerpt":"We investigate the contribution that a local over- or under-density can have on linear cosmic dipole estimations. We focus here on radio surveys, such as the NRAO VLA Sky Survey (NVSS), and forthcoming surveys such as those with the LOw Frequency ARray (LOFAR), the Australian Square Kilometre Array Pathfinder (ASKAP) and the Square Kilometre Array (SKA). The NVSS has already been used to estimate the cosmic radio dipole; it was shown recently that this radio dipole amplitude is larger than expected from a purely kinematic effect, assuming the velocity inferred from the dipole of the cosmic mic"},"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":"1402.0376","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2014-02-03T13:13:22Z","cross_cats_sorted":[],"title_canon_sha256":"31ee096cf2a2fc43f7aae088f3e6e0f60c076d0c9ace65d3229df9c32d3aabfd","abstract_canon_sha256":"1d074383bfac35366cb74b09e836bb18798b61f91d0f7b2dcb21552f31f5878d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:51:14.858440Z","signature_b64":"Uo+62V6CxLMWHNIT4pn9+BtGbM9GAT13x26sw/GT0imlslS5iLzKhnGT13U/S087HhV5MJHswOh2y7koH1CXCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6ba716d02c674571747a6b8f16c819b05a73c9c9bb0959e861f5bcc509a70b72","last_reissued_at":"2026-05-18T02:51:14.857982Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:51:14.857982Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Impact of local structure on the cosmic radio dipole","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"David Bacon, Dominik J. Schwarz, Matthias Rubart","submitted_at":"2014-02-03T13:13:22Z","abstract_excerpt":"We investigate the contribution that a local over- or under-density can have on linear cosmic dipole estimations. We focus here on radio surveys, such as the NRAO VLA Sky Survey (NVSS), and forthcoming surveys such as those with the LOw Frequency ARray (LOFAR), the Australian Square Kilometre Array Pathfinder (ASKAP) and the Square Kilometre Array (SKA). The NVSS has already been used to estimate the cosmic radio dipole; it was shown recently that this radio dipole amplitude is larger than expected from a purely kinematic effect, assuming the velocity inferred from the dipole of the cosmic mic"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1402.0376","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":""},"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":"1402.0376","created_at":"2026-05-18T02:51:14.858052+00:00"},{"alias_kind":"arxiv_version","alias_value":"1402.0376v2","created_at":"2026-05-18T02:51:14.858052+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1402.0376","created_at":"2026-05-18T02:51:14.858052+00:00"},{"alias_kind":"pith_short_12","alias_value":"NOTRNUBMM5CX","created_at":"2026-05-18T12:28:41.024544+00:00"},{"alias_kind":"pith_short_16","alias_value":"NOTRNUBMM5CXC5D2","created_at":"2026-05-18T12:28:41.024544+00:00"},{"alias_kind":"pith_short_8","alias_value":"NOTRNUBM","created_at":"2026-05-18T12:28:41.024544+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.19476","citing_title":"Prospect of Measuring the Cosmic Dipole by Strongly Lensed Gravitational Waves Associated with Galaxy Surveys","ref_index":18,"is_internal_anchor":true},{"citing_arxiv_id":"2602.11093","citing_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","ref_index":66,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB","json":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB.json","graph_json":"https://pith.science/api/pith-number/NOTRNUBMM5CXC5D2NOHRNSAZWB/graph.json","events_json":"https://pith.science/api/pith-number/NOTRNUBMM5CXC5D2NOHRNSAZWB/events.json","paper":"https://pith.science/paper/NOTRNUBM"},"agent_actions":{"view_html":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB","download_json":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB.json","view_paper":"https://pith.science/paper/NOTRNUBM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1402.0376&json=true","fetch_graph":"https://pith.science/api/pith-number/NOTRNUBMM5CXC5D2NOHRNSAZWB/graph.json","fetch_events":"https://pith.science/api/pith-number/NOTRNUBMM5CXC5D2NOHRNSAZWB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB/action/storage_attestation","attest_author":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB/action/author_attestation","sign_citation":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB/action/citation_signature","submit_replication":"https://pith.science/pith/NOTRNUBMM5CXC5D2NOHRNSAZWB/action/replication_record"}},"created_at":"2026-05-18T02:51:14.858052+00:00","updated_at":"2026-05-18T02:51:14.858052+00:00"}