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Title:
First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Beam Profiles and Window Functions
Authors:
Page, L.; Barnes, C.; Hinshaw, G.; Spergel, D. N.; Weiland, J. L.; Wollack, E.; Bennett, C. L.; Halpern, M.; Jarosik, N.; Kogut, A.; Limon, M.; Meyer, S. S.; Tucker, G. S.; Wright, E. L.
Affiliation:
AA(Department of Physics, Jadwin Hall, Princeton, NJ 08544; .), AB(Department of Physics, Jadwin Hall, Princeton, NJ 08544; .), AC(NASA Goddard Space Flight Center, Greenbelt, Code 685, MD 20771.), AD(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544.), AE(Science Systems and Applications, Inc. (SSAI), 10210 Greenbelt Road, Suite 600 Lanham, MD 20706.), AF(NASA Goddard Space Flight Center, Greenbelt, Code 685, MD 20771.), AG(NASA Goddard Space Flight Center, Greenbelt, Code 685, MD 20771.), AH(Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada.), AI(Department of Physics, Jadwin Hall, Princeton, NJ 08544; .), AJ(Department of Physics, Jadwin Hall, Princeton, NJ 08544; .), AK(Department of Physics, Jadwin Hall, Princeton, NJ 08544; .; National Research Council (NRC) Fellow.), AL(Departments of Astrophysics and Physics, EFI, and CfCP, University of Chicago, Chicago, IL 60637.), AM(National Research Council (NRC) Fellow.; Department of Physics, Brown University, Providence, RI 02912.), AN(Department of Astronomy, UCLA, P.O. Box 951562, Los Angeles, CA 90095-1562.)
Publication:
The Astrophysical Journal Supplement Series, Volume 148, Issue 1, pp. 39-50. (ApJS Homepage)
Publication Date:
09/2003
Origin:
UCP
ApJ Keywords:
Cosmology: Cosmic Microwave Background, Cosmology: Observations, Instrumentation: Miscellaneous, Planets and Satellites: Individual: Jupiter, Telescopes
DOI:
10.1086/377223
Bibliographic Code:
2003ApJS..148...39P

Abstract

Knowledge of the beam profiles is of critical importance for interpreting data from cosmic microwave background experiments. In this paper, we present the characterization of the in-flight optical response of the WMAP satellite. The main-beam intensities have been mapped to <=-30 dB of their peak values by observing Jupiter with the satellite in the same observing mode as for CMB observations. The beam patterns closely follow the prelaunch expectations. The full width at half-maximum is a function of frequency and ranges from 0.82d at 23 GHz to 0.21d at 94 GHz; however, the beams are not Gaussian. We present (a) the beam patterns for all 10 differential radiometers, showing that the patterns are substantially independent of polarization in all but the 23 GHz channel; (b) the effective symmetrized beam patterns that result from WMAP's compound spin observing pattern; (c) the effective window functions for all radiometers and the formalism for propagating the window function uncertainty; and (d) the conversion factor from point-source flux to antenna temperature. A summary of the systematic uncertainties, which currently dominate our knowledge of the beams, is also presented. The constancy of Jupiter's temperature within a frequency band is an essential check of the optical system. The tests enable us to report a calibration of Jupiter to 1%-3% accuracy relative to the CMB dipole.

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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