TY - JOUR
T1 - First-year Wilkinson Microwave Anisotropy Probe (WMAP) observations
T2 - Galactic signal contamination from sidelobe pickup
AU - Barnes, C.
AU - Hill, R. S.
AU - Hinshaw, G.
AU - Page, L.
AU - Bennett, C. L.
AU - Halpern, M.
AU - Jarosik, N.
AU - Kogut, A.
AU - Limon, M.
AU - Meyer, S. S.
AU - Tucker, G. S.
AU - Wollack, E.
AU - Wright, E. L.
PY - 2003/9
Y1 - 2003/9
N2 - Since the Galactic center is ∼1000 times brighter than fluctuations in the cosmic microwave background (CMB), CMB experiments must carefully account for stray Galactic pickup. We present the level of contamination due to sidelobes for the first-year CMB maps produced by the Wilkinson Microwave Anisotropy Probe (WMAP) observatory. For each radiometer, full 4π sr antenna gain patterns are determined from a combination of numerical prediction and ground-based and space-based measurements. These patterns are convolved with the WMAP first-year sky maps and observatory scan pattern to generate the expected sidelobe signal contamination, for both intensity and polarized microwave sky maps. When the main beams are outside of the Galactic plane, we find rms values for the expected sidelobe pickup of 15, 2.1, 2.0, 0.3, and 0.5 μK for the K, Ka, Q, V, and W bands, respectively. Except for at the K band, the rms polarized contamination is ≫ 1 μK. Angular power spectra of the Galactic pickup are presented.
AB - Since the Galactic center is ∼1000 times brighter than fluctuations in the cosmic microwave background (CMB), CMB experiments must carefully account for stray Galactic pickup. We present the level of contamination due to sidelobes for the first-year CMB maps produced by the Wilkinson Microwave Anisotropy Probe (WMAP) observatory. For each radiometer, full 4π sr antenna gain patterns are determined from a combination of numerical prediction and ground-based and space-based measurements. These patterns are convolved with the WMAP first-year sky maps and observatory scan pattern to generate the expected sidelobe signal contamination, for both intensity and polarized microwave sky maps. When the main beams are outside of the Galactic plane, we find rms values for the expected sidelobe pickup of 15, 2.1, 2.0, 0.3, and 0.5 μK for the K, Ka, Q, V, and W bands, respectively. Except for at the K band, the rms polarized contamination is ≫ 1 μK. Angular power spectra of the Galactic pickup are presented.
KW - Cosmic microwave background
KW - Cosmology: observations
KW - Galaxy: structure
KW - ISM: structure
KW - Instrumentation: miscellaneous
KW - Methods: data analysis
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U2 - 10.1086/377227
DO - 10.1086/377227
M3 - Article
AN - SCOPUS:0242473595
SN - 0067-0049
VL - 148
SP - 51
EP - 62
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 1
ER -