{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:EXZQRPHZ7E2VXRDQMD5JKEGVEO","short_pith_number":"pith:EXZQRPHZ","schema_version":"1.0","canonical_sha256":"25f308bcf9f9355bc47060fa9510d523bed24bd16adc29449c8c28d86ef94070","source":{"kind":"arxiv","id":"astro-ph/0002467","version":1},"attestation_state":"computed","paper":{"title":"An Australia telescope survey for CMB anisotropies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2), (2) RRI, (3) UCB), Australia, India, J. Silk (3) ((1) ATNF, M. J. Kesteven (1), M. Sinclair(1), R. D. Ekers (1), R. Subrahmanyan (1","submitted_at":"2000-02-24T22:38:04Z","abstract_excerpt":"We have surveyed six distinct `empty fields' using the Australia Telescope Compact Array in an ultra-compact configuration with the aim of imaging, with a high brightness sensitivity, any arcmin-scale brightness-temperature anisotropies in the background radio sky. The six well-separated regions were observed at a frequency of 8.7 GHz and the survey regions were limited by the ATCA primary beams which have a full width at half maximum of 6 arcmin at this frequency; all fields were observed with a resolution of 2 arcmin and an rms thermal noise of 24 microJy/beam. After subtracting foreground c"},"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":"astro-ph/0002467","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-02-24T22:38:04Z","cross_cats_sorted":[],"title_canon_sha256":"40de219d75212a062ec8cf57af76decac9349a1acf5f304fbfbaff82cb7810ea","abstract_canon_sha256":"e37087d60110790347ecd2683f1fd23e08d53d13e6aab719b60bd489a2b93ab5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:16:06.797066Z","signature_b64":"QoQ278L1cRDmh+/K7GOHd/Fuqe7ShWFoeost6P52FrErK1J47qAr6ciV1KZhsbbyhdUxI5Vua46So6JD3gjVAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"25f308bcf9f9355bc47060fa9510d523bed24bd16adc29449c8c28d86ef94070","last_reissued_at":"2026-07-04T16:16:06.796648Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:16:06.796648Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"An Australia telescope survey for CMB anisotropies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2), (2) RRI, (3) UCB), Australia, India, J. Silk (3) ((1) ATNF, M. J. Kesteven (1), M. Sinclair(1), R. D. Ekers (1), R. Subrahmanyan (1","submitted_at":"2000-02-24T22:38:04Z","abstract_excerpt":"We have surveyed six distinct `empty fields' using the Australia Telescope Compact Array in an ultra-compact configuration with the aim of imaging, with a high brightness sensitivity, any arcmin-scale brightness-temperature anisotropies in the background radio sky. The six well-separated regions were observed at a frequency of 8.7 GHz and the survey regions were limited by the ATCA primary beams which have a full width at half maximum of 6 arcmin at this frequency; all fields were observed with a resolution of 2 arcmin and an rms thermal noise of 24 microJy/beam. After subtracting foreground c"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0002467","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0002467/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":"astro-ph/0002467","created_at":"2026-07-04T16:16:06.796711+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0002467v1","created_at":"2026-07-04T16:16:06.796711+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0002467","created_at":"2026-07-04T16:16:06.796711+00:00"},{"alias_kind":"pith_short_12","alias_value":"EXZQRPHZ7E2V","created_at":"2026-07-04T16:16:06.796711+00:00"},{"alias_kind":"pith_short_16","alias_value":"EXZQRPHZ7E2VXRDQ","created_at":"2026-07-04T16:16:06.796711+00:00"},{"alias_kind":"pith_short_8","alias_value":"EXZQRPHZ","created_at":"2026-07-04T16:16:06.796711+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1907.04495","citing_title":"Direct detection of the cosmic expansion: the redshift drift and the flux drift","ref_index":16,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO","json":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO.json","graph_json":"https://pith.science/api/pith-number/EXZQRPHZ7E2VXRDQMD5JKEGVEO/graph.json","events_json":"https://pith.science/api/pith-number/EXZQRPHZ7E2VXRDQMD5JKEGVEO/events.json","paper":"https://pith.science/paper/EXZQRPHZ"},"agent_actions":{"view_html":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO","download_json":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO.json","view_paper":"https://pith.science/paper/EXZQRPHZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0002467&json=true","fetch_graph":"https://pith.science/api/pith-number/EXZQRPHZ7E2VXRDQMD5JKEGVEO/graph.json","fetch_events":"https://pith.science/api/pith-number/EXZQRPHZ7E2VXRDQMD5JKEGVEO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO/action/storage_attestation","attest_author":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO/action/author_attestation","sign_citation":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO/action/citation_signature","submit_replication":"https://pith.science/pith/EXZQRPHZ7E2VXRDQMD5JKEGVEO/action/replication_record"}},"created_at":"2026-07-04T16:16:06.796711+00:00","updated_at":"2026-07-04T16:16:06.796711+00:00"}