{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:T65GJ4VUCIIHUK4UTMEKV7MYXE","short_pith_number":"pith:T65GJ4VU","schema_version":"1.0","canonical_sha256":"9fba64f2b412107a2b949b08aafd98b91ee4708070f6fbbd018cfac1c9e1f4ce","source":{"kind":"arxiv","id":"1911.03547","version":1},"attestation_state":"computed","paper":{"title":"Deprojecting beam systematics for next-generation CMB B-mode searches","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"Christopher Sheehy","submitted_at":"2019-11-08T21:21:41Z","abstract_excerpt":"Measurements of the cosmic microwave background polarization are vulnerable to systematic contamination from beam imperfections. Because the unpolarized CMB T is orders of magnitude larger than the polarized E and B signals, even a tiny difference in instrument response between two orthogonally polarized measurements of the CMB will result in a large non-zero differential signal, even if the CMB is unpolarized. Two strategies to mitigate this temperature-to-polarization leakage are the use of a rotating half-wave-plate and the fitting and removal of leakage templates from the polarized signal."},"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":"1911.03547","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2019-11-08T21:21:41Z","cross_cats_sorted":[],"title_canon_sha256":"f9cf98190b32c72436934d5fce3e7003753de202c7e01d00c20fffe5aa2fcb6a","abstract_canon_sha256":"583340a7defd251c3a4f711ad8bd98d6163845912a9a5415f03fbf0c6caad6a4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:18:13.496842Z","signature_b64":"SYnTcHDeeWKbnBi6Jhg0qoSXzDHkv6If7wm5D88f9Kdq3wlKs0xD+x3q7qXP/0ZRFIuaOutSb+jZFbiVLgyMBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9fba64f2b412107a2b949b08aafd98b91ee4708070f6fbbd018cfac1c9e1f4ce","last_reissued_at":"2026-07-05T00:18:13.496333Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:18:13.496333Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Deprojecting beam systematics for next-generation CMB B-mode searches","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"Christopher Sheehy","submitted_at":"2019-11-08T21:21:41Z","abstract_excerpt":"Measurements of the cosmic microwave background polarization are vulnerable to systematic contamination from beam imperfections. Because the unpolarized CMB T is orders of magnitude larger than the polarized E and B signals, even a tiny difference in instrument response between two orthogonally polarized measurements of the CMB will result in a large non-zero differential signal, even if the CMB is unpolarized. Two strategies to mitigate this temperature-to-polarization leakage are the use of a rotating half-wave-plate and the fitting and removal of leakage templates from the polarized signal."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1911.03547","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/1911.03547/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":"1911.03547","created_at":"2026-07-05T00:18:13.496391+00:00"},{"alias_kind":"arxiv_version","alias_value":"1911.03547v1","created_at":"2026-07-05T00:18:13.496391+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1911.03547","created_at":"2026-07-05T00:18:13.496391+00:00"},{"alias_kind":"pith_short_12","alias_value":"T65GJ4VUCIIH","created_at":"2026-07-05T00:18:13.496391+00:00"},{"alias_kind":"pith_short_16","alias_value":"T65GJ4VUCIIHUK4U","created_at":"2026-07-05T00:18:13.496391+00:00"},{"alias_kind":"pith_short_8","alias_value":"T65GJ4VU","created_at":"2026-07-05T00:18:13.496391+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.20415","citing_title":"Forecasts of effects of beam systematics and deprojection on the third-generation ground-based cosmic microwave background experiment","ref_index":54,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE","json":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE.json","graph_json":"https://pith.science/api/pith-number/T65GJ4VUCIIHUK4UTMEKV7MYXE/graph.json","events_json":"https://pith.science/api/pith-number/T65GJ4VUCIIHUK4UTMEKV7MYXE/events.json","paper":"https://pith.science/paper/T65GJ4VU"},"agent_actions":{"view_html":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE","download_json":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE.json","view_paper":"https://pith.science/paper/T65GJ4VU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1911.03547&json=true","fetch_graph":"https://pith.science/api/pith-number/T65GJ4VUCIIHUK4UTMEKV7MYXE/graph.json","fetch_events":"https://pith.science/api/pith-number/T65GJ4VUCIIHUK4UTMEKV7MYXE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE/action/storage_attestation","attest_author":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE/action/author_attestation","sign_citation":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE/action/citation_signature","submit_replication":"https://pith.science/pith/T65GJ4VUCIIHUK4UTMEKV7MYXE/action/replication_record"}},"created_at":"2026-07-05T00:18:13.496391+00:00","updated_at":"2026-07-05T00:18:13.496391+00:00"}