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Fig.1 Frequency response of the WMAP data collection system and some representative input spectra. The curve labeled ‘‘AEU filter’’ (dot-dashed line) is the amplitude response of the two-pole Bessel filter (ƒ_{3dB} = 100 Hz) before the voltage-to-frequency converter in the Analog Electronics Unit. The four solid lines labeled ‘‘Integrator’’ are the absolute values of the sinc functions corresponding to the 128, 102.4, 76.8, and 51.2 ms integration periods used for the
different radiometer frequency bands. (See Fig. 8 of Bennett et al. 2003b.) The dashed lines labeled ‘‘Window’’ are the frequency spectra that would result
from WMAP’s scan pattern and beams if it were observing a scale invariant angular power spectrum (C_{l} = const.) sky based on the window functions in Page
et al. (2003a). The dotted line labeled ‘‘CMB’’ is the input signal to the data collection system that would occur for a typical CMB sky sampled by an ideal
pencil beam. The two squares on this last curve show the approximate locations of the first two peaks in the CMB power spectrum. The response of the AEU
filter is down from unity by 0.1% at l = 1000, indicating that it has a negligible effect on the shape of the observed power spectra.
Fig.2 Noise power spectral density of the V12 radiometer obtained from 3 days of on-orbit data. Sky signals arising from the dipole, CMB, Galaxy, and point sources have been removed. The inset contains an
expanded view of the low-frequency region of the same data. The flat
spectrum down to very low frequencies ( ƒ_{knee} = 1.41 mHz) indicates
proper radiometer performance.
Fig.3 Dependence of ƒ_{knee} on T_{off} for the 20 radiometers comprising WMAP. The solid line is a power-law fit to the data of the form ƒ_{knee} ∝ [(|T_{off}|Δν_{eff}^{½})/T_{sys}]^{2/α} with α = 1.70. The scaling of ƒ_{knee} with T_{off}
indicates that ƒ_{knee} is largely determined by radiometer gain fluctuations
modulating the signal from the radiometer offsets, as expected.
Fig.4 Predicted differential (thin line) and common-mode (thick line)
CMB dipole signal for a typical 2 hr period of WMAP observations. The
rapid period (≈2 minute) corresponds to WMAP’s spin rate and the slower
period (1 hr) to the precession rate. Measurement of the common-mode
signal component in a radiometer’s output allows characterization of the
nonideal (common-mode) radiometric response.
Fig.5 On-orbit measurements of the radiometer offset temperatures, T_{off} (stars), and predicted contributions to the offset temperature, ΔT_{off} (diamonds),
for all 20 WMAP radiometers. Values of ΔT_{off} are obtained from measurements of the radiometer common-mode responses to the CMB dipole signal.
Significant correlation between the measured offset and the predicted values of ΔT_{off} are expected and observed. The lines are drawn to aid in seeing the correlation.
Fig.6 Distribution of the prewhitened V12 radiometer noise obtained from 10 days of observations. Sky signals arising from the dipole, CMB, and Galaxy have been removed. Data points were cut when either radiometer
beam encountered a planet or a region of high Galactic emission. The line corresponds to a unit variance Gaussian distribution normalized to the observed frequency at s = 0. The two symbols denote the values obtained from the two sides of the distribution. The highly Gaussian distribution indicates that the noise variance for each pixel of the resulting sky maps should scale inversely with the number of observations of that pixel.
Fig.7 Measured sample variance, s^{2}, dependence on normalized
number of observations, N_{obs}, for the V1 sky map. The diamonds are the
sample variances measured from each subset of map elements for which
N - 0.5 < N_{obs} < N + 0.5. The solid line is a linear fit to the data. As
expected, the noise variance scales as N
obs, confirming that it is a good
predictor of the pixel noise.
Fig.8 Comparison of the V11 radiometer gains measured from the
CMB dipole (diamonds) and the gain model (solid line). The CMB derived
gains are 24 hr averages. The high-frequency noise in the gain model arises
from the quantization of the RF bias housekeeping data. The rapid gain
change ≈245 days after launch is the result of a small (0.5 K) change of the
RXB temperature as a consequence of an adjustment of the spacecraft’s
main bus voltage. Note the entire vertical scale spans a ≈4% range. The
model clearly tracks the measured gain values well and is therefore useful in
smoothing and interpolating the hourly gain measurements.