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Title:
First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing Methods and Systematic Error Limits
Authors:
Hinshaw, G.; Barnes, C.; Bennett, C. L.; Greason, M. R.; Halpern, M.; Hill, R. S.; Jarosik, N.; Kogut, A.; Limon, M.; Meyer, S. S.; Odegard, N.; Page, L.; Spergel, D. N.; Tucker, G. S.; Weiland, J. L.; Wollack, E.; Wright, E. L.
Affiliation:
AA(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771; .), AB(Department of Physics, Princeton University, Jadwin Hall, P.O. Box 708, Princeton, NJ 08544.), AC(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771; .), AD(Science Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706.), AE(Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada.), AF(Science Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706.), AG(Department of Physics, Princeton University, Jadwin Hall, P.O. Box 708, Princeton, NJ 08544.), AH(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771; .), AI(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771; .; National Research Council (NRC) Fellow.), AJ(Departments of Astrophysics and Physics, EFI, and CfCP, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637.), AK(Science Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706.), AL(Department of Physics, Princeton University, Jadwin Hall, P.O. Box 708, Princeton, NJ 08544.), AM(Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544.), AN(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771; .; National Research Council (NRC) Fellow.; Department of Physics, Brown University, Providence, RI 02912.), AO(Science Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600, Lanham, MD 20706.), AP(NASA Goddard Space Flight Center, Code 685, Greenbelt, MD 20771; .), AQ(Department of Astronomy, UCLA, P.O. Box 951562, Los Angeles, CA 90095-1562.)
Publication:
The Astrophysical Journal Supplement Series, Volume 148, Issue 1, pp. 63-95. (ApJS Homepage)
Publication Date:
09/2003
Origin:
UCP
ApJ Keywords:
Cosmology: Cosmic Microwave Background, Cosmology: Observations, Instrumentation: Detectors, Methods: Data Analysis, Space Vehicles: Instruments
DOI:
10.1086/377222
Bibliographic Code:
2003ApJS..148...63H

Abstract

We describe the calibration and data processing methods used to generate full-sky maps of the cosmic microwave background (CMB) from the first year of Wilkinson Microwave Anisotropy Probe (WMAP) observations. Detailed limits on residual systematic errors are assigned based largely on analyses of the flight data supplemented, where necessary, with results from ground tests. The data are calibrated in flight using the dipole modulation of the CMB due to the observatory's motion around the Sun. This constitutes a full-beam calibration source. An iterative algorithm simultaneously fits the time-ordered data to obtain calibration parameters and pixelized sky map temperatures. The noise properties are determined by analyzing the time-ordered data with this sky signal estimate subtracted. Based on this, we apply a prewhitening filter to the time-ordered data to remove a low level of 1/f noise. We infer and correct for a small (~1%) transmission imbalance between the two sky inputs to each differential radiometer, and we subtract a small sidelobe correction from the 23 GHz (K-band) map prior to further analysis. No other systematic error corrections are applied to the data. Calibration and baseline artifacts, including the response to environmental perturbations, are negligible. Systematic uncertainties are comparable to statistical uncertainties in the characterization of the beam response. Both are accounted for in the covariance matrix of the window function and are propagated to uncertainties in the final power spectrum. We characterize the combined upper limits to residual systematic uncertainties through the pixel covariance matrix.

WMAP is the result of a partnership between Princeton University and the NASA Goddard Space Flight Center. Scientific guidance is provided by the WMAP Science Team.

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