{"paper":{"title":"First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Angular Power Spectrum","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) Princeton, (3) SSAI, (4) U. Chicago, (5) UBC, (6) Brown, (7) UCLA), A. Kogut (1), C. Barnes (1), C. L. Bennett (2), D. N. Spergel (2), E. Komatsu (2), E. L. Wright (7) ((1) NASA's GSFC, E. Wollack (1), G. Hinshaw (1), G. S. Tucker (6), J. Weiland (3), L. Page (2), L. Verde (2), M. Halpern (5), M. Limon (1), N. Jarosik (2), R. S. Hill (3), S. S. Meyer (4)","submitted_at":"2003-02-11T21:41:09Z","abstract_excerpt":"We present the angular power spectrum derived from the first-year Wilkinson Microwave Anisotropy Probe (WMAP) sky maps. We study a variety of power spectrum estimation methods and data combinations and demonstrate that the results are robust. The data are modestly contaminated by diffuse Galactic foreground emission, but we show that a simple Galactic template model is sufficient to remove the signal. Point sources produce a modest contamination in the low frequency data. After masking ~700 known bright sources from the maps, we estimate residual sources contribute ~3500 uK^2 at 41 GHz, and ~1"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0302217","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"}