2001/04/30 by Yongzhong Xu, Max Tegmark, A. de Oliveira‐Costa +1 · 2 citations
Mathematics · Physics and Astronomy · #Algorithm #Astrophysics #Astrophysics and Cosmic Phenomena #Computer science #Cosmic microwave background #Cosmology and Gravitation Theories #Mathematics #Optics #Physics #Radio Astronomy Observations and Technology #Scale (ratio) #Spectral density #Statistics #astro-ph
paper · pdf · doi:10.1103/physrevd.65.083002
published as Phys.Rev.D65:083002,2002 · Revised to match accepted PRD version. Substantially expanded. Window functions, map and covariance matrix at http://www.hep.upenn.edu/~xuyz/qmask.html
arxiv created 2002/01/18 · openalex publication_date 2002/03/21 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We measure the cosmic microwave background power spectrum on angular scales l\ensuremath∼30--200 (1\ifmmode^∘\else\textdegree\fi--6\ifmmode^∘\else\textdegree\fi) from the QMASK map, which combines the data from the QMAP and Saskatoon experiments. Since the accuracy of recent measurements leftward of the first acoustic peak is limited by sample variance, the large area of the QMASK map (648 square degrees) allows us to place among the sharpest constraints to date in this range, in good agreement with BOOMERanG and (on the largest scales) COBE-DMR. By band-pass filtering the QMAP and Saskatoon maps, we are able to spatially compare them scale by scale to check for beam- and pointing-related systematic errors.