{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:7DBDXVPXW6T7YWWSQQQCN3KI7U","short_pith_number":"pith:7DBDXVPX","schema_version":"1.0","canonical_sha256":"f8c23bd5f7b7a7fc5ad2842026ed48fd22d908400368952565f8eced53feece7","source":{"kind":"arxiv","id":"2504.13070","version":2},"attestation_state":"computed","paper":{"title":"A quadratic estimator view of the transfer function correction in intensity mapping surveys","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Zhaoting Chen","submitted_at":"2025-04-17T16:31:14Z","abstract_excerpt":"In single dish neutral hydrogen (HI) intensity mapping, signal separation methods such as principal component analysis (PCA) are used to clean the astrophysical foregrounds. PCA induces a signal loss in the estimated power spectrum, which can be corrected by a transfer function (TF). By injecting mock signals of HI into the data and performing the PCA cleaning, we can use the cleaned mock HI signal to cross-correlate with the original mock, and estimate the signal loss as a TF, ${T}(\\vec{k})$. As expected, a correction of ${T} (\\vec{k})^{-1}$ restores the cross-power between the HI and optical"},"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":"2504.13070","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-04-17T16:31:14Z","cross_cats_sorted":[],"title_canon_sha256":"dfda841b53e6128cf9de1e934438710c96d51eb209a4399652120e916e135350","abstract_canon_sha256":"3dec1508baeb015a9592a2caf99f8854f0dcf0bb1762f1dbe29088dd64ada641"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:47:21.961127Z","signature_b64":"XPZE9Pm6t98NsislFHZlNLzcMoGzLf70SIv0jDAqlNgQ+YmKEEa4zQ1QMpJL0xaxgDnjgIYCPSsR3SeVcHjpAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f8c23bd5f7b7a7fc5ad2842026ed48fd22d908400368952565f8eced53feece7","last_reissued_at":"2026-07-05T11:47:21.960604Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:47:21.960604Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A quadratic estimator view of the transfer function correction in intensity mapping surveys","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Zhaoting Chen","submitted_at":"2025-04-17T16:31:14Z","abstract_excerpt":"In single dish neutral hydrogen (HI) intensity mapping, signal separation methods such as principal component analysis (PCA) are used to clean the astrophysical foregrounds. PCA induces a signal loss in the estimated power spectrum, which can be corrected by a transfer function (TF). By injecting mock signals of HI into the data and performing the PCA cleaning, we can use the cleaned mock HI signal to cross-correlate with the original mock, and estimate the signal loss as a TF, ${T}(\\vec{k})$. As expected, a correction of ${T} (\\vec{k})^{-1}$ restores the cross-power between the HI and optical"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2504.13070","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/2504.13070/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":"2504.13070","created_at":"2026-07-05T11:47:21.960657+00:00"},{"alias_kind":"arxiv_version","alias_value":"2504.13070v2","created_at":"2026-07-05T11:47:21.960657+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2504.13070","created_at":"2026-07-05T11:47:21.960657+00:00"},{"alias_kind":"pith_short_12","alias_value":"7DBDXVPXW6T7","created_at":"2026-07-05T11:47:21.960657+00:00"},{"alias_kind":"pith_short_16","alias_value":"7DBDXVPXW6T7YWWS","created_at":"2026-07-05T11:47:21.960657+00:00"},{"alias_kind":"pith_short_8","alias_value":"7DBDXVPX","created_at":"2026-07-05T11:47:21.960657+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.08593","citing_title":"Beyond {\\Lambda}CDM with the SKA Observatory -- II: Unveiling the Secrets of the Early Universe","ref_index":17,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U","json":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U.json","graph_json":"https://pith.science/api/pith-number/7DBDXVPXW6T7YWWSQQQCN3KI7U/graph.json","events_json":"https://pith.science/api/pith-number/7DBDXVPXW6T7YWWSQQQCN3KI7U/events.json","paper":"https://pith.science/paper/7DBDXVPX"},"agent_actions":{"view_html":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U","download_json":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U.json","view_paper":"https://pith.science/paper/7DBDXVPX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2504.13070&json=true","fetch_graph":"https://pith.science/api/pith-number/7DBDXVPXW6T7YWWSQQQCN3KI7U/graph.json","fetch_events":"https://pith.science/api/pith-number/7DBDXVPXW6T7YWWSQQQCN3KI7U/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U/action/storage_attestation","attest_author":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U/action/author_attestation","sign_citation":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U/action/citation_signature","submit_replication":"https://pith.science/pith/7DBDXVPXW6T7YWWSQQQCN3KI7U/action/replication_record"}},"created_at":"2026-07-05T11:47:21.960657+00:00","updated_at":"2026-07-05T11:47:21.960657+00:00"}