{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:S3WFBQMYT7VPTHZF6CW45H3TAA","short_pith_number":"pith:S3WFBQMY","schema_version":"1.0","canonical_sha256":"96ec50c1989feaf99f25f0adce9f730006461d57f1d895dab93ef0cc308537a0","source":{"kind":"arxiv","id":"2502.18459","version":1},"attestation_state":"computed","paper":{"title":"Spectral modelling of Cygnus A between 110 and 250 MHz. Impact on the LOFAR 21-cm signal power spectrum","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"A. Acharya, A. R. Offringa, B. Ciardi, B. K. Gehlot, C. H\\\"ofer, E. Ceccotti, F. G. Mertens, I. Hothi, I. T. Iliev, J. K. Chege, J. P. McKean, L. V. E. Koopmans, M. Mevius, R. Ghara, S. A. Brackenhoff, S. Ghosh, S. Munshi, S. Zaroubi","submitted_at":"2025-02-25T18:58:49Z","abstract_excerpt":"Studying the redshifted 21-cm signal from the the neutral hydrogen during the Epoch of Reionization and Cosmic Dawn is fundamental for understanding the physics of the early universe. One of the challenges that 21-cm experiments face is the contamination by bright foreground sources, such as Cygnus A, for which accurate spatial and spectral models are needed to minimise the residual contamination after their removal. In this work, we develop a new, high-resolution model of Cygnus A using Low Frequency Array (LOFAR) observations in the $110{-}250$ MHz range, improving upon previous models by in"},"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":"2502.18459","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-02-25T18:58:49Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"81c29dee9f1fa3406d247a43e71f9a2d4d7fac6ce8a4dbcd4c6080c39f3467b3","abstract_canon_sha256":"f8abf8b381dd30e1643a3e6544e0ea347d57f90ed232e53fdfa5a40d8553220a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:46:00.963034Z","signature_b64":"lohcDj6o+oRJUNOTdx0TDUOObftExGPK0PCx65PCQrdwNhCsCvLA+TJZKtyD7380zn2WixXcw1t/Q9H7MvnaAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"96ec50c1989feaf99f25f0adce9f730006461d57f1d895dab93ef0cc308537a0","last_reissued_at":"2026-07-05T10:46:00.962571Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:46:00.962571Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Spectral modelling of Cygnus A between 110 and 250 MHz. Impact on the LOFAR 21-cm signal power spectrum","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"A. Acharya, A. R. Offringa, B. Ciardi, B. K. Gehlot, C. H\\\"ofer, E. Ceccotti, F. G. Mertens, I. Hothi, I. T. Iliev, J. K. Chege, J. P. McKean, L. V. E. Koopmans, M. Mevius, R. Ghara, S. A. Brackenhoff, S. Ghosh, S. Munshi, S. Zaroubi","submitted_at":"2025-02-25T18:58:49Z","abstract_excerpt":"Studying the redshifted 21-cm signal from the the neutral hydrogen during the Epoch of Reionization and Cosmic Dawn is fundamental for understanding the physics of the early universe. One of the challenges that 21-cm experiments face is the contamination by bright foreground sources, such as Cygnus A, for which accurate spatial and spectral models are needed to minimise the residual contamination after their removal. In this work, we develop a new, high-resolution model of Cygnus A using Low Frequency Array (LOFAR) observations in the $110{-}250$ MHz range, improving upon previous models by in"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2502.18459","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/2502.18459/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":"2502.18459","created_at":"2026-07-05T10:46:00.962632+00:00"},{"alias_kind":"arxiv_version","alias_value":"2502.18459v1","created_at":"2026-07-05T10:46:00.962632+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2502.18459","created_at":"2026-07-05T10:46:00.962632+00:00"},{"alias_kind":"pith_short_12","alias_value":"S3WFBQMYT7VP","created_at":"2026-07-05T10:46:00.962632+00:00"},{"alias_kind":"pith_short_16","alias_value":"S3WFBQMYT7VPTHZF","created_at":"2026-07-05T10:46:00.962632+00:00"},{"alias_kind":"pith_short_8","alias_value":"S3WFBQMY","created_at":"2026-07-05T10:46:00.962632+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.10533","citing_title":"Improved upper limits on the 21-cm signal power spectrum at $z=17.0$ and $z=20.3$ from an optimal field observed with NenuFAR","ref_index":16,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA","json":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA.json","graph_json":"https://pith.science/api/pith-number/S3WFBQMYT7VPTHZF6CW45H3TAA/graph.json","events_json":"https://pith.science/api/pith-number/S3WFBQMYT7VPTHZF6CW45H3TAA/events.json","paper":"https://pith.science/paper/S3WFBQMY"},"agent_actions":{"view_html":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA","download_json":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA.json","view_paper":"https://pith.science/paper/S3WFBQMY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2502.18459&json=true","fetch_graph":"https://pith.science/api/pith-number/S3WFBQMYT7VPTHZF6CW45H3TAA/graph.json","fetch_events":"https://pith.science/api/pith-number/S3WFBQMYT7VPTHZF6CW45H3TAA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA/action/storage_attestation","attest_author":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA/action/author_attestation","sign_citation":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA/action/citation_signature","submit_replication":"https://pith.science/pith/S3WFBQMYT7VPTHZF6CW45H3TAA/action/replication_record"}},"created_at":"2026-07-05T10:46:00.962632+00:00","updated_at":"2026-07-05T10:46:00.962632+00:00"}