{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:2NJKHIJFTD2PP5ODNXJYJBA3XB","short_pith_number":"pith:2NJKHIJF","schema_version":"1.0","canonical_sha256":"d352a3a12598f4f7f5c36dd384841bb86290282e52f940795cef64f1ee30f17b","source":{"kind":"arxiv","id":"1502.07596","version":2},"attestation_state":"computed","paper":{"title":"Foregrounds in Wide-Field Redshifted 21 cm Power Spectra","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.IM","authors_text":"A. de Oliveira-Costa, A. E. E. Rogers, A. Ewall-Wice, A. Loeb, A. P. Beardsley, A. R. Neben, A. R. Offringa, A. Roshi, A. R. Whitney, A. Williams, B. E. Corey, B. J. Hazelton, B. McKinley, B. Pindor, C. J. Lonsdale, C. L. Williams, C. M. Trott, C. Wu, D. A. Mitchell, Daniel C. Jacobs, D. Emrich, D. L. Kaplan, D. Oberoi, E. Kratzenberg, E. Lenc, E. Morgan, F. Briggs, G. Bernardi, Han-Seek Kim, I. S. Sullivan, J. C. Kasper, J. C. Pober, J. Line, J. N. Hewitt, Joshua S. Dillon, J. Riding, J. S. B. Wyithe, Judd D. Bowman, K. S. Srivani, L. Feng, L. J. Greenhill, M. F. Morales, M. J. Lynch, M. Johnston-Hollitt, M. Tegmark, M. Waterson, N. Barry, N. Hurley-Walker, Nithyanandan Thyagarajan, N. Udaya Shankar, P. Carroll, P. Kittiwisit, P. Procopio, R. B. Wayth, R. Goeke, R. J. Cappallo, R. L. Webster, R. Subrahmanyan, Shiv K. Sethi, S. J. Tingay, S. M. Ord, Sourabh Paul, S. R. McWhirter, T. Prabu","submitted_at":"2015-02-24T21:00:16Z","abstract_excerpt":"Detection of 21~cm emission of HI from the epoch of reionization, at redshifts z>6, is limited primarily by foreground emission. We investigate the signatures of wide-field measurements and an all-sky foreground model using the delay spectrum technique that maps the measurements to foreground object locations through signal delays between antenna pairs. We demonstrate interferometric measurements are inherently sensitive to all scales, including the largest angular scales, owing to the nature of wide-field measurements. These wide-field effects are generic to all observations but antenna shape"},"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":"1502.07596","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2015-02-24T21:00:16Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"3e739460c5d6a4b07399d949b92154066b520485a277f60521518bcd6029406e","abstract_canon_sha256":"0dfa84d8d0e3057c7aac8a2b4dd70465db86802d64dc109219dac6940e260b9f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:18:04.660152Z","signature_b64":"H2iuAl7KgwpljCxGe8RXHXa8/lDvgqBvE53G4OZ79F2sS5U4lUve/eubWqfj16ik6IDj/BqkDMB74qU/VHSYAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d352a3a12598f4f7f5c36dd384841bb86290282e52f940795cef64f1ee30f17b","last_reissued_at":"2026-05-18T01:18:04.659236Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:18:04.659236Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Foregrounds in Wide-Field Redshifted 21 cm Power Spectra","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.IM","authors_text":"A. de Oliveira-Costa, A. E. E. Rogers, A. Ewall-Wice, A. Loeb, A. P. Beardsley, A. R. Neben, A. R. Offringa, A. Roshi, A. R. Whitney, A. Williams, B. E. Corey, B. J. Hazelton, B. McKinley, B. Pindor, C. J. Lonsdale, C. L. Williams, C. M. Trott, C. Wu, D. A. Mitchell, Daniel C. Jacobs, D. Emrich, D. L. Kaplan, D. Oberoi, E. Kratzenberg, E. Lenc, E. Morgan, F. Briggs, G. Bernardi, Han-Seek Kim, I. S. Sullivan, J. C. Kasper, J. C. Pober, J. Line, J. N. Hewitt, Joshua S. Dillon, J. Riding, J. S. B. Wyithe, Judd D. Bowman, K. S. Srivani, L. Feng, L. J. Greenhill, M. F. Morales, M. J. Lynch, M. Johnston-Hollitt, M. Tegmark, M. Waterson, N. Barry, N. Hurley-Walker, Nithyanandan Thyagarajan, N. Udaya Shankar, P. Carroll, P. Kittiwisit, P. Procopio, R. B. Wayth, R. Goeke, R. J. Cappallo, R. L. Webster, R. Subrahmanyan, Shiv K. Sethi, S. J. Tingay, S. M. Ord, Sourabh Paul, S. R. McWhirter, T. Prabu","submitted_at":"2015-02-24T21:00:16Z","abstract_excerpt":"Detection of 21~cm emission of HI from the epoch of reionization, at redshifts z>6, is limited primarily by foreground emission. We investigate the signatures of wide-field measurements and an all-sky foreground model using the delay spectrum technique that maps the measurements to foreground object locations through signal delays between antenna pairs. We demonstrate interferometric measurements are inherently sensitive to all scales, including the largest angular scales, owing to the nature of wide-field measurements. These wide-field effects are generic to all observations but antenna shape"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1502.07596","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":"1502.07596","created_at":"2026-05-18T01:18:04.659369+00:00"},{"alias_kind":"arxiv_version","alias_value":"1502.07596v2","created_at":"2026-05-18T01:18:04.659369+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1502.07596","created_at":"2026-05-18T01:18:04.659369+00:00"},{"alias_kind":"pith_short_12","alias_value":"2NJKHIJFTD2P","created_at":"2026-05-18T12:29:02.477457+00:00"},{"alias_kind":"pith_short_16","alias_value":"2NJKHIJFTD2PP5OD","created_at":"2026-05-18T12:29:02.477457+00:00"},{"alias_kind":"pith_short_8","alias_value":"2NJKHIJF","created_at":"2026-05-18T12:29:02.477457+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.20518","citing_title":"Mapping Cosmological Signal Scales to Beam Calibration Requirements in 21cm Experiments and Implications for Near-Field Measurement","ref_index":91,"is_internal_anchor":true},{"citing_arxiv_id":"2605.10928","citing_title":"Mitigating residual foregrounds and systematic errors in SKA1-Low AA* EoR observations via Bayesian Gaussian Process Regression","ref_index":18,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB","json":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB.json","graph_json":"https://pith.science/api/pith-number/2NJKHIJFTD2PP5ODNXJYJBA3XB/graph.json","events_json":"https://pith.science/api/pith-number/2NJKHIJFTD2PP5ODNXJYJBA3XB/events.json","paper":"https://pith.science/paper/2NJKHIJF"},"agent_actions":{"view_html":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB","download_json":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB.json","view_paper":"https://pith.science/paper/2NJKHIJF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1502.07596&json=true","fetch_graph":"https://pith.science/api/pith-number/2NJKHIJFTD2PP5ODNXJYJBA3XB/graph.json","fetch_events":"https://pith.science/api/pith-number/2NJKHIJFTD2PP5ODNXJYJBA3XB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB/action/storage_attestation","attest_author":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB/action/author_attestation","sign_citation":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB/action/citation_signature","submit_replication":"https://pith.science/pith/2NJKHIJFTD2PP5ODNXJYJBA3XB/action/replication_record"}},"created_at":"2026-05-18T01:18:04.659369+00:00","updated_at":"2026-05-18T01:18:04.659369+00:00"}