{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:S2ZG3REFKUV4MMQN2F5UN2YA6W","short_pith_number":"pith:S2ZG3REF","schema_version":"1.0","canonical_sha256":"96b26dc485552bc6320dd17b46eb00f5866a8b74b5563ca5ab48b510ac7d02f6","source":{"kind":"arxiv","id":"1109.5093","version":1},"attestation_state":"computed","paper":{"title":"Evidence for anomalous dust-correlated emission at 8 GHz","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Joanna Dunkley, Lyman Page, Michelle Lu","submitted_at":"2011-09-23T14:37:22Z","abstract_excerpt":"In 1969 Edward Conklin measured the anisotropy in celestial emission at 8 GHz with a resolution of 16.2 degrees and used the data to report a detection of the CMB dipole. Given the paucity of 8 GHz observations over large angular scales and the clear evidence for non-power law Galactic emission near 8 GHz, a new analysis of Conklin's data is informative. In this paper we compare Conklin's data to that from Haslam et al. (0.4 GHz), Reich and Reich (1.4 GHz), and WMAP (23-94 GHz). We show that the spectral index between Conklin's data and the 23 GHz WMAP data is beta=-1.7+-0.1, where we model th"},"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":"1109.5093","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2011-09-23T14:37:22Z","cross_cats_sorted":[],"title_canon_sha256":"729ea70acf022577c0ee7916e6444343e01e2d3f06fbde10bb4d04cf0a720db9","abstract_canon_sha256":"f2f759ea88d6b23e3bf5b806d7893df5f4350d2078c4553d1cb2d10f342d6dd6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:00:25.959093Z","signature_b64":"6KNrkKm/R2G7WEVgaoI+iGOxssBo/PnGSL+5UvcZc+x67wtV3BLt2T6xMItM7BGCWHKxrfELZvGczmW+RrL+Cg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"96b26dc485552bc6320dd17b46eb00f5866a8b74b5563ca5ab48b510ac7d02f6","last_reissued_at":"2026-05-18T02:00:25.958222Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:00:25.958222Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evidence for anomalous dust-correlated emission at 8 GHz","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Joanna Dunkley, Lyman Page, Michelle Lu","submitted_at":"2011-09-23T14:37:22Z","abstract_excerpt":"In 1969 Edward Conklin measured the anisotropy in celestial emission at 8 GHz with a resolution of 16.2 degrees and used the data to report a detection of the CMB dipole. Given the paucity of 8 GHz observations over large angular scales and the clear evidence for non-power law Galactic emission near 8 GHz, a new analysis of Conklin's data is informative. In this paper we compare Conklin's data to that from Haslam et al. (0.4 GHz), Reich and Reich (1.4 GHz), and WMAP (23-94 GHz). We show that the spectral index between Conklin's data and the 23 GHz WMAP data is beta=-1.7+-0.1, where we model th"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1109.5093","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":"1109.5093","created_at":"2026-05-18T02:00:25.958425+00:00"},{"alias_kind":"arxiv_version","alias_value":"1109.5093v1","created_at":"2026-05-18T02:00:25.958425+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1109.5093","created_at":"2026-05-18T02:00:25.958425+00:00"},{"alias_kind":"pith_short_12","alias_value":"S2ZG3REFKUV4","created_at":"2026-05-18T12:26:41.206345+00:00"},{"alias_kind":"pith_short_16","alias_value":"S2ZG3REFKUV4MMQN","created_at":"2026-05-18T12:26:41.206345+00:00"},{"alias_kind":"pith_short_8","alias_value":"S2ZG3REF","created_at":"2026-05-18T12:26:41.206345+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.23489","citing_title":"A comparison between Galactic magnetic field models and polarized synchrotron emission with C-BASS at 4.76 GHz and S-PASS at 2.3 GHz","ref_index":294,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W","json":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W.json","graph_json":"https://pith.science/api/pith-number/S2ZG3REFKUV4MMQN2F5UN2YA6W/graph.json","events_json":"https://pith.science/api/pith-number/S2ZG3REFKUV4MMQN2F5UN2YA6W/events.json","paper":"https://pith.science/paper/S2ZG3REF"},"agent_actions":{"view_html":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W","download_json":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W.json","view_paper":"https://pith.science/paper/S2ZG3REF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1109.5093&json=true","fetch_graph":"https://pith.science/api/pith-number/S2ZG3REFKUV4MMQN2F5UN2YA6W/graph.json","fetch_events":"https://pith.science/api/pith-number/S2ZG3REFKUV4MMQN2F5UN2YA6W/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W/action/timestamp_anchor","attest_storage":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W/action/storage_attestation","attest_author":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W/action/author_attestation","sign_citation":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W/action/citation_signature","submit_replication":"https://pith.science/pith/S2ZG3REFKUV4MMQN2F5UN2YA6W/action/replication_record"}},"created_at":"2026-05-18T02:00:25.958425+00:00","updated_at":"2026-05-18T02:00:25.958425+00:00"}