{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:QVZ2PMBBY42SR2RD2OZBGRJDJQ","short_pith_number":"pith:QVZ2PMBB","schema_version":"1.0","canonical_sha256":"8573a7b021c73528ea23d3b21345234c0ea10ca47b4adfc50111079076021f7c","source":{"kind":"arxiv","id":"1602.05249","version":1},"attestation_state":"computed","paper":{"title":"Beamforming Errors in Murchison Widefield Array Phased Array Antennas and their effects on Epoch of Reionization Science","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.IM","authors_text":"A. A. Deshpande, A. R. Neben, A. Williams, B. E. Corey, B. J. Hazelton, C. J. Lonsdale, C. L. Williams, D. A. Mitchell, D. L. Kaplan, D. Oberoi, E. Morgan, F. Briggs, G. Bernardi, J. D. Bowman, J. N. Hewitt, J. S. Dillon, K. S. Srivani, L. J. Greenhill, M. F. Morales, M. Johnston-Hollitt, N. Udaya Shankar, R. B. Wayth, R. F. Bradley, R. Goeke, R. J. Cappallo, R. L. Webster, R. Subrahmanyan, S. J. Tingay, S. M. Ord, S. R. McWhirter, T. Prabu","submitted_at":"2016-02-17T00:13:27Z","abstract_excerpt":"Accurate antenna beam models are critical for radio observations aiming to isolate the redshifted 21cm spectral line emission from the Dark Ages and the Epoch of Reionization and unlock the scientific potential of 21cm cosmology. Past work has focused on characterizing mean antenna beam models using either satellite signals or astronomical sources as calibrators, but antenna-to-antenna variation due to imperfect instrumentation has remained unexplored. We characterize this variation for the Murchison Widefield Array (MWA) through laboratory measurements and simulations, finding typical deviati"},"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":"1602.05249","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2016-02-17T00:13:27Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"277bdd3b232c80925c955bf4365f5e4e9d7de7952f48921d3781a0b300460eda","abstract_canon_sha256":"09e8447779a72259665b788ccf73c752c7d66147c8a790535c98462b41bb97d6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:18:37.313954Z","signature_b64":"hhiVpVXud7oR5qQJYw5txmHAdxmglRAyyT45ZgjICeE5Mc5B/oCCTcH4H/FeBG4YHMKnVtCe8kRhRGPKRBdcBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8573a7b021c73528ea23d3b21345234c0ea10ca47b4adfc50111079076021f7c","last_reissued_at":"2026-05-18T01:18:37.313409Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:18:37.313409Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Beamforming Errors in Murchison Widefield Array Phased Array Antennas and their effects on Epoch of Reionization Science","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.IM","authors_text":"A. A. Deshpande, A. R. Neben, A. Williams, B. E. Corey, B. J. Hazelton, C. J. Lonsdale, C. L. Williams, D. A. Mitchell, D. L. Kaplan, D. Oberoi, E. Morgan, F. Briggs, G. Bernardi, J. D. Bowman, J. N. Hewitt, J. S. Dillon, K. S. Srivani, L. J. Greenhill, M. F. Morales, M. Johnston-Hollitt, N. Udaya Shankar, R. B. Wayth, R. F. Bradley, R. Goeke, R. J. Cappallo, R. L. Webster, R. Subrahmanyan, S. J. Tingay, S. M. Ord, S. R. McWhirter, T. Prabu","submitted_at":"2016-02-17T00:13:27Z","abstract_excerpt":"Accurate antenna beam models are critical for radio observations aiming to isolate the redshifted 21cm spectral line emission from the Dark Ages and the Epoch of Reionization and unlock the scientific potential of 21cm cosmology. Past work has focused on characterizing mean antenna beam models using either satellite signals or astronomical sources as calibrators, but antenna-to-antenna variation due to imperfect instrumentation has remained unexplored. We characterize this variation for the Murchison Widefield Array (MWA) through laboratory measurements and simulations, finding typical deviati"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1602.05249","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":"1602.05249","created_at":"2026-05-18T01:18:37.313510+00:00"},{"alias_kind":"arxiv_version","alias_value":"1602.05249v1","created_at":"2026-05-18T01:18:37.313510+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1602.05249","created_at":"2026-05-18T01:18:37.313510+00:00"},{"alias_kind":"pith_short_12","alias_value":"QVZ2PMBBY42S","created_at":"2026-05-18T12:30:41.710351+00:00"},{"alias_kind":"pith_short_16","alias_value":"QVZ2PMBBY42SR2RD","created_at":"2026-05-18T12:30:41.710351+00:00"},{"alias_kind":"pith_short_8","alias_value":"QVZ2PMBB","created_at":"2026-05-18T12:30:41.710351+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"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":82,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ","json":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ.json","graph_json":"https://pith.science/api/pith-number/QVZ2PMBBY42SR2RD2OZBGRJDJQ/graph.json","events_json":"https://pith.science/api/pith-number/QVZ2PMBBY42SR2RD2OZBGRJDJQ/events.json","paper":"https://pith.science/paper/QVZ2PMBB"},"agent_actions":{"view_html":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ","download_json":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ.json","view_paper":"https://pith.science/paper/QVZ2PMBB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1602.05249&json=true","fetch_graph":"https://pith.science/api/pith-number/QVZ2PMBBY42SR2RD2OZBGRJDJQ/graph.json","fetch_events":"https://pith.science/api/pith-number/QVZ2PMBBY42SR2RD2OZBGRJDJQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ/action/storage_attestation","attest_author":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ/action/author_attestation","sign_citation":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ/action/citation_signature","submit_replication":"https://pith.science/pith/QVZ2PMBBY42SR2RD2OZBGRJDJQ/action/replication_record"}},"created_at":"2026-05-18T01:18:37.313510+00:00","updated_at":"2026-05-18T01:18:37.313510+00:00"}