{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:Q4CRDFDCMOJVGQZSOQYJPF6O4I","short_pith_number":"pith:Q4CRDFDC","schema_version":"1.0","canonical_sha256":"8705119462639353433274309797cee23e5f8cea85673d7684b30ce98abe7fae","source":{"kind":"arxiv","id":"1909.12369","version":1},"attestation_state":"computed","paper":{"title":"Foregrounds and their mitigation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"Emma Chapman, Vibor Jeli\\'c","submitted_at":"2019-09-26T20:11:19Z","abstract_excerpt":"The low-frequency radio sky is dominated by the diffuse synchrotron emission of our Galaxy and extragalactic radio sources related to Active Galactic Nuclei and star-forming galaxies. This foreground emission is much brighter than the cosmological 21 cm emission from the Cosmic Dawn and Epoch of Reionization. Studying the physical properties of the foregrounds is therefore of fundamental importance for their mitigation in the cosmological 21 cm experiments. This chapter gives a comprehensive overview of the foregrounds and our current state-of-the-art knowledge about their mitigation."},"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":"1909.12369","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2019-09-26T20:11:19Z","cross_cats_sorted":["astro-ph.GA","astro-ph.IM"],"title_canon_sha256":"83831355ca26a5377fc9a6bcadc1fd715fb9ade36ecb3a396c5a2891b588ede2","abstract_canon_sha256":"4e4d7b2ca0b873d04f95e9f8447cd179ac3c55edb495fe4a484d701b8e515cdb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:07:38.780415Z","signature_b64":"hWMp1eo0LC54Dfh0cJPh7LuyMrKHDQrEWl4h7CPJh7eoHgRjJDLKZEd6waIGDfb4lkyyeCarVadF+q2WBWBJCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8705119462639353433274309797cee23e5f8cea85673d7684b30ce98abe7fae","last_reissued_at":"2026-07-05T00:07:38.779940Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:07:38.779940Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Foregrounds and their mitigation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"Emma Chapman, Vibor Jeli\\'c","submitted_at":"2019-09-26T20:11:19Z","abstract_excerpt":"The low-frequency radio sky is dominated by the diffuse synchrotron emission of our Galaxy and extragalactic radio sources related to Active Galactic Nuclei and star-forming galaxies. This foreground emission is much brighter than the cosmological 21 cm emission from the Cosmic Dawn and Epoch of Reionization. Studying the physical properties of the foregrounds is therefore of fundamental importance for their mitigation in the cosmological 21 cm experiments. This chapter gives a comprehensive overview of the foregrounds and our current state-of-the-art knowledge about their mitigation."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1909.12369","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/1909.12369/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":"1909.12369","created_at":"2026-07-05T00:07:38.780000+00:00"},{"alias_kind":"arxiv_version","alias_value":"1909.12369v1","created_at":"2026-07-05T00:07:38.780000+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1909.12369","created_at":"2026-07-05T00:07:38.780000+00:00"},{"alias_kind":"pith_short_12","alias_value":"Q4CRDFDCMOJV","created_at":"2026-07-05T00:07:38.780000+00:00"},{"alias_kind":"pith_short_16","alias_value":"Q4CRDFDCMOJVGQZS","created_at":"2026-07-05T00:07:38.780000+00:00"},{"alias_kind":"pith_short_8","alias_value":"Q4CRDFDC","created_at":"2026-07-05T00:07:38.780000+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.10105","citing_title":"Application of Machine Learning to 21 cm Cosmology","ref_index":18,"is_internal_anchor":false},{"citing_arxiv_id":"2510.25886","citing_title":"Mitigating gain calibration errors from EoR observations with SKA1-Low AA*","ref_index":27,"is_internal_anchor":false},{"citing_arxiv_id":"2605.10105","citing_title":"Application of Machine Learning to 21 cm Cosmology","ref_index":18,"is_internal_anchor":false},{"citing_arxiv_id":"2605.10105","citing_title":"Application of Machine Learning to 21 cm Cosmology","ref_index":11,"is_internal_anchor":false},{"citing_arxiv_id":"2604.27465","citing_title":"Foreground Mitigation and Power Spectrum Analysis for Tianlai Full-Sky 21 cm Survey Observation","ref_index":8,"is_internal_anchor":false},{"citing_arxiv_id":"2605.10105","citing_title":"Application of Machine Learning to 21 cm Cosmology","ref_index":11,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I","json":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I.json","graph_json":"https://pith.science/api/pith-number/Q4CRDFDCMOJVGQZSOQYJPF6O4I/graph.json","events_json":"https://pith.science/api/pith-number/Q4CRDFDCMOJVGQZSOQYJPF6O4I/events.json","paper":"https://pith.science/paper/Q4CRDFDC"},"agent_actions":{"view_html":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I","download_json":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I.json","view_paper":"https://pith.science/paper/Q4CRDFDC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1909.12369&json=true","fetch_graph":"https://pith.science/api/pith-number/Q4CRDFDCMOJVGQZSOQYJPF6O4I/graph.json","fetch_events":"https://pith.science/api/pith-number/Q4CRDFDCMOJVGQZSOQYJPF6O4I/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I/action/storage_attestation","attest_author":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I/action/author_attestation","sign_citation":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I/action/citation_signature","submit_replication":"https://pith.science/pith/Q4CRDFDCMOJVGQZSOQYJPF6O4I/action/replication_record"}},"created_at":"2026-07-05T00:07:38.780000+00:00","updated_at":"2026-07-05T00:07:38.780000+00:00"}