{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:EB46ZE3EHL2W6K4VOCYEJXKX7A","short_pith_number":"pith:EB46ZE3E","schema_version":"1.0","canonical_sha256":"2079ec93643af56f2b9570b044dd57f831129c45ec61ba1deba57fe586192f67","source":{"kind":"arxiv","id":"1211.0041","version":1},"attestation_state":"computed","paper":{"title":"The Cosmology Large Angular Scale Surveyor (CLASS): 40 GHz optical design","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.IM","authors_text":"Charles L. Bennett, David T. Chuss, Edward J. Wollack, Joseph R. Eimer, Lingzhen Zeng, Tobias A. Marriage","submitted_at":"2012-10-31T21:46:10Z","abstract_excerpt":"The Cosmology Large Angular Scale Surveyor (CLASS) instrument will measure the polarization of the cosmic microwave background at 40, 90, and 150 GHz from Cerro Toco in the Atacama desert of northern Chile. In this paper, we describe the optical design of the 40 GHz telescope system. The telescope is a diffraction limited catadioptric design consisting of a front-end Variable-delay Polarization Modulator (VPM), two ambient temperature mirrors, two cryogenic dielectric lenses, thermal blocking filters, and an array of 36 smooth-wall scalar feedhorn antennas. The feed horns guide the signal to a"},"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":"1211.0041","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2012-10-31T21:46:10Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"d35b49ef324377bbde29f15922cd8c6cbe996aaa51ce54f45d07d55d5d3a6b85","abstract_canon_sha256":"d6ad6bea0ba859015c9ea4da13ba3521ff5104c20215432e41299ff68b6487bc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:41:43.307780Z","signature_b64":"AwIEGRsJS4rW/DjlNiaixhZX/cLqWi39nGhMT3QBh1G1mbpCtpiJtn19d1HZzLrwPwltuqPhsNfCnFdPrUyHBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2079ec93643af56f2b9570b044dd57f831129c45ec61ba1deba57fe586192f67","last_reissued_at":"2026-05-18T03:41:43.306937Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:41:43.306937Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Cosmology Large Angular Scale Surveyor (CLASS): 40 GHz optical design","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.IM","authors_text":"Charles L. Bennett, David T. Chuss, Edward J. Wollack, Joseph R. Eimer, Lingzhen Zeng, Tobias A. Marriage","submitted_at":"2012-10-31T21:46:10Z","abstract_excerpt":"The Cosmology Large Angular Scale Surveyor (CLASS) instrument will measure the polarization of the cosmic microwave background at 40, 90, and 150 GHz from Cerro Toco in the Atacama desert of northern Chile. In this paper, we describe the optical design of the 40 GHz telescope system. The telescope is a diffraction limited catadioptric design consisting of a front-end Variable-delay Polarization Modulator (VPM), two ambient temperature mirrors, two cryogenic dielectric lenses, thermal blocking filters, and an array of 36 smooth-wall scalar feedhorn antennas. The feed horns guide the signal to a"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1211.0041","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":"1211.0041","created_at":"2026-05-18T03:41:43.307080+00:00"},{"alias_kind":"arxiv_version","alias_value":"1211.0041v1","created_at":"2026-05-18T03:41:43.307080+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1211.0041","created_at":"2026-05-18T03:41:43.307080+00:00"},{"alias_kind":"pith_short_12","alias_value":"EB46ZE3EHL2W","created_at":"2026-05-18T12:27:04.183437+00:00"},{"alias_kind":"pith_short_16","alias_value":"EB46ZE3EHL2W6K4V","created_at":"2026-05-18T12:27:04.183437+00:00"},{"alias_kind":"pith_short_8","alias_value":"EB46ZE3E","created_at":"2026-05-18T12:27:04.183437+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.23489","citing_title":"A comparison between Galactic magnetic field models and polarized synchrotron emission with C-BASS at 4.76 GHz and S-PASS at 2.3 GHz","ref_index":142,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A","json":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A.json","graph_json":"https://pith.science/api/pith-number/EB46ZE3EHL2W6K4VOCYEJXKX7A/graph.json","events_json":"https://pith.science/api/pith-number/EB46ZE3EHL2W6K4VOCYEJXKX7A/events.json","paper":"https://pith.science/paper/EB46ZE3E"},"agent_actions":{"view_html":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A","download_json":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A.json","view_paper":"https://pith.science/paper/EB46ZE3E","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1211.0041&json=true","fetch_graph":"https://pith.science/api/pith-number/EB46ZE3EHL2W6K4VOCYEJXKX7A/graph.json","fetch_events":"https://pith.science/api/pith-number/EB46ZE3EHL2W6K4VOCYEJXKX7A/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A/action/storage_attestation","attest_author":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A/action/author_attestation","sign_citation":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A/action/citation_signature","submit_replication":"https://pith.science/pith/EB46ZE3EHL2W6K4VOCYEJXKX7A/action/replication_record"}},"created_at":"2026-05-18T03:41:43.307080+00:00","updated_at":"2026-05-18T03:41:43.307080+00:00"}