{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:VNT3ACMB5GFYSOYMLBL4KUOJJ4","short_pith_number":"pith:VNT3ACMB","schema_version":"1.0","canonical_sha256":"ab67b00981e98b893b0c5857c551c94f12afd2c5c6256af0ef23a35920e6f094","source":{"kind":"arxiv","id":"2004.06041","version":2},"attestation_state":"computed","paper":{"title":"Foreground modelling via Gaussian process regression: an application to HERA data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Aaron Ewall-Wice, Aaron R. Parsons, Abhik Ghosh, Abraham R. Neben, Adam P. Beardsley, Adrian Liu, Alec Josaitis, Amy S. Igarashi, Andrei Mesinger, Angelo Syce, Anita Loots, Austin F. Fortino, Austin Julius, Bharat K. Gehlot, Bojan Nikolic, Bradley Greig, Brian Glendenning, Bryna J. Hazelton, Carina Cheng, Christopher L. Carilli, Chuneeta D. Nunhokee, Craig Smith, Cresshim Malgas, Daniel C. Jacobs, David MacMahon, David R. DeBoer, Deepthi Gorthi, Eloy de Lera Acedo, Eunice Matsetela, Florent Mertens, Gcobisa Fadana, Gianni Bernardi, Haoxuan Zheng, Jack Hickish, James E. Aguirre, James Robnett, Jasper Grobbelaar, Jon Ringuette, Joshua S. Dillon, Judd D. Bowman, Kathryn Rosie, L\\'eon V. E. Koopmans, Lourence Malan, MacCalvin Kariseb, M\\'ario G. Santos, Matthew Kolopanis, Matthys Maree, Max Tegmark, Miguel F. Morales, Nathan Mathison, Nicholas S. Kern, Nicolas Fagnoni, Nima Razavi-Ghods, Nipanjana Patra, Nithyanandan Thyagarajan, Oleg M. Smirnov, Paul Alexander, Paul M. Chichura, Peter K. G. Williams, Raddwine Sell, Randall Fritz, Richard F. Bradley, Roshan K. Benefo, Samantha Pieterse, Samavarti Gallardo, Saul A. Kohn, Siyanda Matika, Steve R. Furlanetto, Tashalee S. Billings, Telalo Lekalake, Trienko L. Grobler, Zachary E. Martinot, Zaki S. Ali","submitted_at":"2020-04-13T16:17:16Z","abstract_excerpt":"The key challenge in the observation of the redshifted 21-cm signal from cosmic reionization is its separation from the much brighter foreground emission. Such separation relies on the different spectral properties of the two components, although, in real life, the foreground intrinsic spectrum is often corrupted by the instrumental response, inducing systematic effects that can further jeopardize the measurement of the 21-cm signal. In this paper, we use Gaussian Process Regression to model both foreground emission and instrumental systematics in $\\sim 2$ hours of data from the Hydrogen Epoch"},"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":"2004.06041","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2020-04-13T16:17:16Z","cross_cats_sorted":[],"title_canon_sha256":"bf1c7ea9899088295e4c881ddf7d7d377cc6e68f6ac4db42e195343886490f95","abstract_canon_sha256":"005d9dc06de7ae02181556350ad09e238b4b85932a78529d6aaeccf8f497db56"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:04:22.630794Z","signature_b64":"6dPy+1dQxqscnx+JmahMNCOIXExGChh96idM76Hhg2O1I7eFe5wUuZfSimr+AEczKvtgi2gv/FYcFx+ZrMYUDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ab67b00981e98b893b0c5857c551c94f12afd2c5c6256af0ef23a35920e6f094","last_reissued_at":"2026-07-05T01:04:22.630241Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:04:22.630241Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Foreground modelling via Gaussian process regression: an application to HERA data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Aaron Ewall-Wice, Aaron R. Parsons, Abhik Ghosh, Abraham R. Neben, Adam P. Beardsley, Adrian Liu, Alec Josaitis, Amy S. Igarashi, Andrei Mesinger, Angelo Syce, Anita Loots, Austin F. Fortino, Austin Julius, Bharat K. Gehlot, Bojan Nikolic, Bradley Greig, Brian Glendenning, Bryna J. Hazelton, Carina Cheng, Christopher L. Carilli, Chuneeta D. Nunhokee, Craig Smith, Cresshim Malgas, Daniel C. Jacobs, David MacMahon, David R. DeBoer, Deepthi Gorthi, Eloy de Lera Acedo, Eunice Matsetela, Florent Mertens, Gcobisa Fadana, Gianni Bernardi, Haoxuan Zheng, Jack Hickish, James E. Aguirre, James Robnett, Jasper Grobbelaar, Jon Ringuette, Joshua S. Dillon, Judd D. Bowman, Kathryn Rosie, L\\'eon V. E. Koopmans, Lourence Malan, MacCalvin Kariseb, M\\'ario G. Santos, Matthew Kolopanis, Matthys Maree, Max Tegmark, Miguel F. Morales, Nathan Mathison, Nicholas S. Kern, Nicolas Fagnoni, Nima Razavi-Ghods, Nipanjana Patra, Nithyanandan Thyagarajan, Oleg M. Smirnov, Paul Alexander, Paul M. Chichura, Peter K. G. Williams, Raddwine Sell, Randall Fritz, Richard F. Bradley, Roshan K. Benefo, Samantha Pieterse, Samavarti Gallardo, Saul A. Kohn, Siyanda Matika, Steve R. Furlanetto, Tashalee S. Billings, Telalo Lekalake, Trienko L. Grobler, Zachary E. Martinot, Zaki S. Ali","submitted_at":"2020-04-13T16:17:16Z","abstract_excerpt":"The key challenge in the observation of the redshifted 21-cm signal from cosmic reionization is its separation from the much brighter foreground emission. Such separation relies on the different spectral properties of the two components, although, in real life, the foreground intrinsic spectrum is often corrupted by the instrumental response, inducing systematic effects that can further jeopardize the measurement of the 21-cm signal. In this paper, we use Gaussian Process Regression to model both foreground emission and instrumental systematics in $\\sim 2$ hours of data from the Hydrogen Epoch"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2004.06041","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/2004.06041/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":"2004.06041","created_at":"2026-07-05T01:04:22.630303+00:00"},{"alias_kind":"arxiv_version","alias_value":"2004.06041v2","created_at":"2026-07-05T01:04:22.630303+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2004.06041","created_at":"2026-07-05T01:04:22.630303+00:00"},{"alias_kind":"pith_short_12","alias_value":"VNT3ACMB5GFY","created_at":"2026-07-05T01:04:22.630303+00:00"},{"alias_kind":"pith_short_16","alias_value":"VNT3ACMB5GFYSOYM","created_at":"2026-07-05T01:04:22.630303+00:00"},{"alias_kind":"pith_short_8","alias_value":"VNT3ACMB","created_at":"2026-07-05T01:04:22.630303+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07814","citing_title":"Intensity fluctuations of radio halo in galaxy cluster: Insights from power spectrum estimation","ref_index":134,"is_internal_anchor":true},{"citing_arxiv_id":"2510.25886","citing_title":"Mitigating gain calibration errors from EoR observations with SKA1-Low AA*","ref_index":79,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4","json":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4.json","graph_json":"https://pith.science/api/pith-number/VNT3ACMB5GFYSOYMLBL4KUOJJ4/graph.json","events_json":"https://pith.science/api/pith-number/VNT3ACMB5GFYSOYMLBL4KUOJJ4/events.json","paper":"https://pith.science/paper/VNT3ACMB"},"agent_actions":{"view_html":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4","download_json":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4.json","view_paper":"https://pith.science/paper/VNT3ACMB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2004.06041&json=true","fetch_graph":"https://pith.science/api/pith-number/VNT3ACMB5GFYSOYMLBL4KUOJJ4/graph.json","fetch_events":"https://pith.science/api/pith-number/VNT3ACMB5GFYSOYMLBL4KUOJJ4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4/action/storage_attestation","attest_author":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4/action/author_attestation","sign_citation":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4/action/citation_signature","submit_replication":"https://pith.science/pith/VNT3ACMB5GFYSOYMLBL4KUOJJ4/action/replication_record"}},"created_at":"2026-07-05T01:04:22.630303+00:00","updated_at":"2026-07-05T01:04:22.630303+00:00"}