{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:OFY6VKNQMUS2YQHQWSJYLI7J3O","short_pith_number":"pith:OFY6VKNQ","schema_version":"1.0","canonical_sha256":"7171eaa9b06525ac40f0b49385a3e9dbaccf141ecb20172cf9b4ebe5f8b1058c","source":{"kind":"arxiv","id":"2112.01458","version":1},"attestation_state":"computed","paper":{"title":"The 90 and 150 GHz universal focal-plane modules for the Simons Observatory","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"Bradley R. Johnson, Cody J. Duell, Daniel Dutcher, Erin Healy, Eve M. Vavagiakis, Heather McCarrick, Jason Austermann, Johannes Hubmayr, Joseph Seibert, Kaiwen Zheng, Kam Arnold, Maximiliano Silva-Feaver, Michael D. Niemack, Nicholas Galitzk, Ningfeng Zhu, Rita F. Sonka, Shannon M. Duff, Steve K. Choi, Suzanne T. Staggs, Tanay Bhandarkar, Yuhan Wang, Zachary Atkins, Zachary B. Huber, Zhilei Xu","submitted_at":"2021-12-02T17:57:00Z","abstract_excerpt":"The Simons Observatory (SO) is a suite of telescopes located in the Atacama Desert in Chile that will make sensitive measurements of the cosmic microwave background. There are a host of cosmological and astrophysical questions that SO is forecasted to address. The universal focal-plane modules (UFMs) populate the four SO telescope receiver focal planes. There are three varieties of UFMs, each of which contains transition-edge-sensor bolometers observing in two spectral bands between 30 and 290~GHz. We describe the novel mid-frequency UFMs, which target two of the six spectral bands at 90 and 1"},"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":"2112.01458","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2021-12-02T17:57:00Z","cross_cats_sorted":[],"title_canon_sha256":"44856d9fa5349fb38eaca427fd2011c143e7a1001d9db35e03bc9b8b7be9b3c3","abstract_canon_sha256":"2bf01e28374f97bc74a74d9fdecd08182edcb4414b7c0f9063c5558df2f864d7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:37:09.776798Z","signature_b64":"3U7ZOLgCHeFX/qkSvTAxgWBRjEKChz/Jsm6kSRiHMaOUkj+MsN7JENKIc2F4FLmKSUTgt12oHqVS2tef/i70AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7171eaa9b06525ac40f0b49385a3e9dbaccf141ecb20172cf9b4ebe5f8b1058c","last_reissued_at":"2026-07-05T03:37:09.776397Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:37:09.776397Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The 90 and 150 GHz universal focal-plane modules for the Simons Observatory","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"Bradley R. Johnson, Cody J. Duell, Daniel Dutcher, Erin Healy, Eve M. Vavagiakis, Heather McCarrick, Jason Austermann, Johannes Hubmayr, Joseph Seibert, Kaiwen Zheng, Kam Arnold, Maximiliano Silva-Feaver, Michael D. Niemack, Nicholas Galitzk, Ningfeng Zhu, Rita F. Sonka, Shannon M. Duff, Steve K. Choi, Suzanne T. Staggs, Tanay Bhandarkar, Yuhan Wang, Zachary Atkins, Zachary B. Huber, Zhilei Xu","submitted_at":"2021-12-02T17:57:00Z","abstract_excerpt":"The Simons Observatory (SO) is a suite of telescopes located in the Atacama Desert in Chile that will make sensitive measurements of the cosmic microwave background. There are a host of cosmological and astrophysical questions that SO is forecasted to address. The universal focal-plane modules (UFMs) populate the four SO telescope receiver focal planes. There are three varieties of UFMs, each of which contains transition-edge-sensor bolometers observing in two spectral bands between 30 and 290~GHz. We describe the novel mid-frequency UFMs, which target two of the six spectral bands at 90 and 1"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2112.01458","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/2112.01458/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":"2112.01458","created_at":"2026-07-05T03:37:09.776455+00:00"},{"alias_kind":"arxiv_version","alias_value":"2112.01458v1","created_at":"2026-07-05T03:37:09.776455+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2112.01458","created_at":"2026-07-05T03:37:09.776455+00:00"},{"alias_kind":"pith_short_12","alias_value":"OFY6VKNQMUS2","created_at":"2026-07-05T03:37:09.776455+00:00"},{"alias_kind":"pith_short_16","alias_value":"OFY6VKNQMUS2YQHQ","created_at":"2026-07-05T03:37:09.776455+00:00"},{"alias_kind":"pith_short_8","alias_value":"OFY6VKNQ","created_at":"2026-07-05T03:37:09.776455+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.01204","citing_title":"The Simons Observatory: Design, Optimization, and Performance of Low Frequency Detectors","ref_index":12,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O","json":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O.json","graph_json":"https://pith.science/api/pith-number/OFY6VKNQMUS2YQHQWSJYLI7J3O/graph.json","events_json":"https://pith.science/api/pith-number/OFY6VKNQMUS2YQHQWSJYLI7J3O/events.json","paper":"https://pith.science/paper/OFY6VKNQ"},"agent_actions":{"view_html":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O","download_json":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O.json","view_paper":"https://pith.science/paper/OFY6VKNQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2112.01458&json=true","fetch_graph":"https://pith.science/api/pith-number/OFY6VKNQMUS2YQHQWSJYLI7J3O/graph.json","fetch_events":"https://pith.science/api/pith-number/OFY6VKNQMUS2YQHQWSJYLI7J3O/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O/action/storage_attestation","attest_author":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O/action/author_attestation","sign_citation":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O/action/citation_signature","submit_replication":"https://pith.science/pith/OFY6VKNQMUS2YQHQWSJYLI7J3O/action/replication_record"}},"created_at":"2026-07-05T03:37:09.776455+00:00","updated_at":"2026-07-05T03:37:09.776455+00:00"}