{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:INFYZL6HVHJBH4LUGNLCDXAEKR","short_pith_number":"pith:INFYZL6H","schema_version":"1.0","canonical_sha256":"434b8cafc7a9d213f174335621dc0454689491186b5b3b48002072ef506ce923","source":{"kind":"arxiv","id":"0704.3991","version":1},"attestation_state":"computed","paper":{"title":"Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Polarization","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Kogut, B. Gold, C. L. Bennett, D. N. Spergel, E. Komatsu, E. L. Wright, E. Wollack, G. Hinshaw, G. S. Tucker, J. Dunkley, J. L. Weiland, L. Page, M. Halpern, M. R. Nolta, N. Jarosik, N. Odegard, O. Dor\\'e","submitted_at":"2007-04-30T18:38:26Z","abstract_excerpt":"We present a full-sky model of polarized Galactic microwave emission based on three years of observations by the Wilkinson Microwave Anisotropy Probe (WMAP) at frequencies from 23 to 94 GHz. The model compares maps of the Stokes Q and U components from each of the 5 WMAP frequency bands in order to separate synchrotron from dust emission, taking into account the spatial and frequency dependence of the synchrotron and dust components. This simple two-component model of the interstellar medium accounts for at least 97% of the polarized emission in the WMAP maps of the microwave sky. Synchrotron "},"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":"0704.3991","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-04-30T18:38:26Z","cross_cats_sorted":[],"title_canon_sha256":"0dba1d7252e4094bccf8c33c12d891619a12a809da8d175984997074b9e0f9f9","abstract_canon_sha256":"f7488851ed6eea651a33457adec060d4725104421f6d98b929d467fb447a7e93"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:44:18.389414Z","signature_b64":"gA/dJQS3dqrCJcpxl4sg1MtcbwWUEwXUFk9kzaHac67jYC+Bej8cE9yLH6FryoMrV0G7LHezB6L2sPl5FldeCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"434b8cafc7a9d213f174335621dc0454689491186b5b3b48002072ef506ce923","last_reissued_at":"2026-07-04T15:44:18.389002Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:44:18.389002Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Polarization","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Kogut, B. Gold, C. L. Bennett, D. N. Spergel, E. Komatsu, E. L. Wright, E. Wollack, G. Hinshaw, G. S. Tucker, J. Dunkley, J. L. Weiland, L. Page, M. Halpern, M. R. Nolta, N. Jarosik, N. Odegard, O. Dor\\'e","submitted_at":"2007-04-30T18:38:26Z","abstract_excerpt":"We present a full-sky model of polarized Galactic microwave emission based on three years of observations by the Wilkinson Microwave Anisotropy Probe (WMAP) at frequencies from 23 to 94 GHz. The model compares maps of the Stokes Q and U components from each of the 5 WMAP frequency bands in order to separate synchrotron from dust emission, taking into account the spatial and frequency dependence of the synchrotron and dust components. This simple two-component model of the interstellar medium accounts for at least 97% of the polarized emission in the WMAP maps of the microwave sky. Synchrotron "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0704.3991","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/0704.3991/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":"0704.3991","created_at":"2026-07-04T15:44:18.389065+00:00"},{"alias_kind":"arxiv_version","alias_value":"0704.3991v1","created_at":"2026-07-04T15:44:18.389065+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0704.3991","created_at":"2026-07-04T15:44:18.389065+00:00"},{"alias_kind":"pith_short_12","alias_value":"INFYZL6HVHJB","created_at":"2026-07-04T15:44:18.389065+00:00"},{"alias_kind":"pith_short_16","alias_value":"INFYZL6HVHJBH4LU","created_at":"2026-07-04T15:44:18.389065+00:00"},{"alias_kind":"pith_short_8","alias_value":"INFYZL6H","created_at":"2026-07-04T15:44:18.389065+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.26576","citing_title":"Detectors for CLASS-W2: The second 90 GHz telescope of the Cosmology Large Angular Scale Surveyor","ref_index":142,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR","json":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR.json","graph_json":"https://pith.science/api/pith-number/INFYZL6HVHJBH4LUGNLCDXAEKR/graph.json","events_json":"https://pith.science/api/pith-number/INFYZL6HVHJBH4LUGNLCDXAEKR/events.json","paper":"https://pith.science/paper/INFYZL6H"},"agent_actions":{"view_html":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR","download_json":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR.json","view_paper":"https://pith.science/paper/INFYZL6H","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0704.3991&json=true","fetch_graph":"https://pith.science/api/pith-number/INFYZL6HVHJBH4LUGNLCDXAEKR/graph.json","fetch_events":"https://pith.science/api/pith-number/INFYZL6HVHJBH4LUGNLCDXAEKR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR/action/storage_attestation","attest_author":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR/action/author_attestation","sign_citation":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR/action/citation_signature","submit_replication":"https://pith.science/pith/INFYZL6HVHJBH4LUGNLCDXAEKR/action/replication_record"}},"created_at":"2026-07-04T15:44:18.389065+00:00","updated_at":"2026-07-04T15:44:18.389065+00:00"}