All Figures

$\begin{figure} \par\includegraphics[height=5cm,width=9cm,clip]{5258f1.ps}\end{figure}$ Figure 1: Spectral transmission of the various types of photometric pixels, obtained by combining different measurements at the component level.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{5258f2.eps}\end{figure}$ Figure 2: Schematic of the Archeops gondola.
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In the text

$\begin{figure} \par\includegraphics[angle=90,height=8cm]{5258f3.eps} \par\end{figure}$ Figure 3: Optical layout of the Archeops focal plane.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,height=10cm]{5258f4.ps} \end{figure}$ Figure 4: From top to bottom, evolution of the temperature of the focal plane and of the 1.6 K and 10 K cryogenic stages during the KS3 flight.
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In the text

$\begin{figure} \par\includegraphics[angle=90, width=17cm,height=15cm]{5258f5.ps}\end{figure}$ Figure 5: From top to bottom and from left to right: the power spectra (in $10^{-17}~{\rm W.Hz^{-\frac{1}{2}}}$ ) of the Archeops 143K03, 217K06, 353K01, and 545K01 bolometers, respectively, as a function of frequency (in Hz). For comparison, we overplot (smooth curve) the detector noise contribution for each bolometer as given by the model presented in the text.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,height=4.5cm]{5258f6.ps}\\ [1mm] \includegraphics[width=7.8cm,height=4.5cm]{5258f7.ps}\end{figure}$ Figure 6: Top: Kernel of the digital filter used for demodulation (see text for details). Bottom: Fourier power spectrum of the digital filter compared to a square filter, to the beam pattern and to the bolometer time constant.
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In the text

$\begin{figure} \par\includegraphics[scale=0.38,angle=90]{5258f8.ps} \end{figure}$ Figure 7: Top: Fourier power spectrum of KS3 143K01 bolometer data showing the frequency peaks produced by the readout electronic noise. Bottom: Same after preprocessing. The amplitude of the peaks is significantly reduced.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=8.5cm,clip]{5258f9.eps} \end{figure}$ Figure 8: Rotation period evolution during the KS3 flight.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,keepaspectratio=true]{5258f10.eps}\end{figure}$ Figure 9: Evolution of the distribution of phase differences between signals and bright stars for the KS3 flight.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,keepaspectratio=true]{5258f11.eps}\end{figure}$ Figure 10: Distribution of the axial distance of bright stars versus the diode number of the corresponding intense signals. Notice the strange behavior of the diode 26. This diode is excluded from analysis.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,keepaspectratio=true]{5258f12.eps}\end{figure}$ Figure 11: Scatter plot of the phase differences in degrees between signals and associated stars for each FSS diode.
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In the text

$\begin{figure} \par\includegraphics[height=5cm,width=5cm]{5258f13.eps} \includegraphics[height=5cm,width=5cm]{5258f14.ps}\end{figure}$ Figure 12: From top to bottom, distribution of errors in axial distance - phase plane with 95% and 68% confidence levels (in white) before and after each scan path fit, respectively.
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In the text

$\begin{figure} \par\includegraphics[height=5cm,width=5cm]{5258f15.ps} \end{figure}$ Figure 13: KS3 flight 95% end 68% confidence levels for error distribution in equatorial coordinates after the scan-path fit.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,height=6cm]{5258f16.ps} \end{figure}$ Figure 14: Top: map of Jupiter for the 143K03 bolometer in $\mu$ V before time constant deconvolution. The map is represented in the par and cross scan direction in arcmin. Bottom: As above, but after deconvolution from the time constant.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5258f17.ps} \end{figure}$ Figure 15: 217K04 Beam profile on Jupiter before (in red) and after (in black) deconvolution of the two time constants ( $\tau _1 = 5.57_{-1.08}^{+1.01}$ ms, $\alpha = 0.48_{-0.04}^{+0.04}$ and $\tau _2 = 38.38_{-4.20}^{+3.80}$ ms).
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{5258f18.ps} \end{figure}$ Figure 16: Glitch template for the bolometer 217K01. A single time constant model has been fitted to the data. For the best fit, traced in red, the time constant is $7.8\pm 0.11$ ms.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,height=5cm]{5258f19.ps} \end{figure}$ Figure 17: Comparison between glitch and Jupiter short time constant estimates.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5258f20.ps} \end{figure}$ Figure 18: From top to bottom and from left to right, for the photometric pixel 143K03, the beam pattern map in $\mu$ V from Jupiter observations, its multi-Gaussian decomposition using seven 2D Gaussians, the residuals and their distribution, which is compatible with Gaussian distributed noise (red line).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{5258f21.ps} \end{figure}$ Figure 19: Focal plane of Archeops reconstructed using Jupiter observations.
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In the text

$\begin{figure} \par\includegraphics[height=10cm,width=17cm]{5258f22.ps} \end{figure}$ Figure 20: Left column: from top to bottom, raw Archeops data in $\mu$ V (black curve) and reconstructed very low frequency drift (red curve) for the 143K03, 217K06, 353K01, and 545K01 bolometers, respectively. Right column: from top to bottom, Archeops data in $\mu$ V after removal of the very low frequency parasitic signals for the 143K03, 217K06, 353K01, and 545K01 bolometers, respectively.
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In the text

$\begin{figure} \par\includegraphics[height=10cm,width=17cm,clip]{5258f23.ps} \end{figure}$ Figure 21: Left column: from top to bottom, Archeops data in $\mu$ V (black curve) and reconstructed spin frequency systematics (red curve, including the CMB dipole and atmospheric emission) for the 143K03, 217K06, 353K01 and 545K01 bolometers respectively. Right column: from top to bottom, Archeops data in $\mu$ V before (black curve) and after (red curve) removal of the spin frequency systematics for the 143K03, 217K06, 353K01 and 545K01 bolometers respectively.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=17cm,clip]{5258f24.ps} \end{figure}$ Figure 22: From left to right and from top to bottom, the power spectrum in $\mu$ V $/\! \sqrt{\rm Hz}$ of the time-ordered Archeops data before (black curve) and after (red curve) subtraction of the spin-frequency systematics for the 143K03, 217K06, 353K01, and 545K01 bolometers.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=17cm,clip]{5258f25.ps} \par\end{figure}$ Figure 23: From left to right and from top to bottom, the power spectrum in $\mu$ V $/ \sqrt ({\rm Hz})$ of the low-frequency processed Archeops data before (in black) and after (in red) decorrelation from the high-frequency noise for the 143K03, 217K06, 353K01, and 545K01 bolometers, respectively.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,width=10cm,angle=90,clip]{5258f... ...\includegraphics[height=8.5cm,width=10cm,angle=90,clip]{5258f27.eps}\end{figure}$ Figure 24: Left column: from top to bottom, time-frequency representation in linear color scale of the 217T04 bolometer data and of the expected Galactic signal for it. Right column: same for the 217K04 bolometer.
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In the text

$\begin{figure} \par\includegraphics[angle=90,height=9cm,width=9cm,clip]{5258f28.ps}\end{figure}$ Figure 25: Top: Average wavelet power spectrum in $\mu$ V of the TOD of the 217K04 Archeops bolometer as a function of frequency computed from its DWPT Bottom: Time evolution of the power spectrum of the TOD of the 217K04 Archeops bolometer computed from its DWPT.
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In the text

$\begin{figure} \par\includegraphics[scale=0.25,angle=90]{5258f29.ps}\\ [1.5mm] ... ...31.ps}\\ [1.5mm] \includegraphics[scale=0.25,angle=90]{5258f32.ps} \end{figure}$ Figure 26: From top to bottom, results of the Kolmogorov-Smirnov test on the bolometers 143K03, 217K06, 353K06, and 545K01, respectively. The white polygons correspond to intervals in the time frequency plane where the test is considered to fail (see text for details).
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In the text

$\begin{figure} \par\includegraphics[scale=0.5,angle=90]{5258f33.ps} \end{figure}$ Figure 27: From left to right and up to bottom, maximum reduced $\chi 2$ (97 d.o.f) of the Gaussian fit of the histogram of the Fourier coefficients of the Archeops data for the 143K03, 217K06, 353K06, and 545K01 bolometers, respectively. In dark and light blue we overplot the $\chi ^{2}$ values for which the probability of having a higher one, considering a Gaussian distribution are 95% and 5%, respectively. (See text for details on the analysis.)
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In the text

$\begin{figure} \par\includegraphics[scale=0.3,angle=90]{5258f34.ps}\includegraphics[scale=0.3,angle=90]{5258f35.ps}\end{figure}$ Figure 28: From left to right, simulated and reconstructed CMB dipole maps in linear scale for the Archeops 143K03 bolometer centered on the Galactic anticenter. To reconstruct both dipole maps, the timelines have been band-pass filtered. This introduces discontinuities on the maps due to the scanning strategy.
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In the text

$\begin{figure} \par\includegraphics[scale=0.5]{5258f36.ps}\end{figure}$ Figure 29: FIRAS/Archeops Galactic profiles correlation on the Galactic plane (bolometer 353K01 at 353 GHz). Fitting a straight line gives the calibration factor.
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In the text

$\begin{figure} \par\includegraphics[scale=0.5]{5258f37.ps} \end{figure}$ Figure 30: Comparison of the Galactic and Dipole calibration factors (in ${\rm mK}/\mu {\rm V}$ ). The error bars (both statistical and systematic) are about 4% and 8% for calibration on the dipole at 143 and 217 GHz, respectively and from 6% to 15% for the calibration on the Galaxy.
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In the text

$\begin{figure} \par\includegraphics[height=5cm,width=8cm]{5258f38.ps} \end{figure}$ Figure 31: Comparison of the point-source (Jupiter and Saturn) and dipole calibration factors. The error bars are about 4% and 8% for calibration on the dipole at 143 and 217 GHz respectively and about 12% for the calibration on the sources (essentially due to the uncertainty of the thermal emission model).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.3cm, height=5cm]{5258f39.ps} \includegraphics[width=4.3cm, height=5cm]{5258f40.ps} } \end{figure}$ Figure 32: From left to right, Archeops Galactic profiles in $\mu$ V at constant Galactic longitude respectively before and after the intercalibration for the 353 GHz bolometers.
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In the text

$\begin{figure} \par\includegraphics*[height=8.cm,keepaspectratio=true,angle=90]{... ...ludegraphics*[height=8.cm,keepaspectratio=true,angle=90]{5258f42.ps}\end{figure}$ Figure 33: Left: power spectrum of the time-ordered data of the bolometer 545K01 before (black) and after (red) destriping. Right: zoom-in of the left plot at first multiples of the spinning frequency.
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In the text

$\begin{figure} \par\includegraphics[scale=0.3,angle=90]{5258f43.ps}\includegraph... ...le=90]{5258f45.eps}\includegraphics[scale=0.3,angle=90]{5258f46.eps}\end{figure}$ Figure 34: From left to right and from top to bottom MDMC decomposition of the Archeops data at intermediate frequencies for the 143K03, 217K04, 353K01, and 545K01 bolometers. The black, blue and red line correspond to power spectrum in arbitrary units of the raw data, the parasitic-like and the Galactic-like contributions respectively.
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In the text

$\begin{figure} \par\includegraphics[scale=0.3,angle=90]{5258f47.eps} \end{figure}$ Figure 35: Power spectrum in arbitrary units of the parasitic-like component for the MDMC analysis of the bolometer 353K01 for different time intervals.
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In the text

$\begin{figure} \par\mbox{\includegraphics[scale=0.35,angle=90]{5258f48.ps} \incl... ...258f50.ps} \includegraphics[scale=0.35,angle=90]{5258f51.ps} } \par\end{figure}$ Figure 36: From top to bottom: Galactic maps in antenna temperature for the 143, 217, 353, and 545 GHz Archeops channels. They are displayed in Galactic coordinates with the Galactic anticenter at the center of the map.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=12cm]{5258f52.ps} \par\end{figure}$ Figure 37: From top to bottom, power spectrum of the Archeops time ordered data before (black curve) and after (red curve) foreground removal for the 143K03 and 217K04 bolometers, respectively. For comparison, the bottom plot shows the power spectrum of the 545K01 bolometer.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{5258f53.ps}\end{figure}$ Figure 38: Top: angular power spectrum of the simulated CMB signal before (black line) and after data processing (blue line) for the 143 GHz. Bottom: transfer function of the data processing pipeline for 143 GHz data.
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In the text

$\begin{figure} \par\includegraphics[scale=0.6,angle=90]{5258f54.ps} \includegraphics[scale=0.6,angle=90]{5258f55.ps} \par\end{figure}$ Figure 39: From top to bottom, combined Archeops CMB maps for the 143 and 217 GHz channels. In the Galactic plane region the residual galactic emission is still visible but clearly disappears at high galactic latitudes where the CMB studies are performed.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=4.3cm, height=5cm]{5258f56.eps} \includegraphics[width=4.3cm, height=5cm]{5258f57.eps} } \end{figure}$ Figure A.1: Simulation profiles.

In the text

$\begin{figure} \par\includegraphics[height=5cm,width=9cm,clip]{5258f1.ps}\end{figure}$	Figure 1: Spectral transmission of the various types of photometric pixels, obtained by combining different measurements at the component level.
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{5258f2.eps}\end{figure}$	Figure 2: Schematic of the Archeops gondola.
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$\begin{figure} \par\includegraphics[angle=90,height=8cm]{5258f3.eps} \par\end{figure}$	Figure 3: Optical layout of the Archeops focal plane.
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$\begin{figure} \par\includegraphics[width=8.5cm,height=10cm]{5258f4.ps} \end{figure}$	Figure 4: From top to bottom, evolution of the temperature of the focal plane and of the 1.6 K and 10 K cryogenic stages during the KS3 flight.
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$\begin{figure} \par\includegraphics[angle=90, width=17cm,height=15cm]{5258f5.ps}\end{figure}$	Figure 5: From top to bottom and from left to right: the power spectra (in $10^{-17}~{\rm W.Hz^{-\frac{1}{2}}}$ ) of the Archeops 143K03, 217K06, 353K01, and 545K01 bolometers, respectively, as a function of frequency (in Hz). For comparison, we overplot (smooth curve) the detector noise contribution for each bolometer as given by the model presented in the text.
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$\begin{figure} \par\includegraphics[width=7.8cm,height=4.5cm]{5258f6.ps}\\ [1mm] \includegraphics[width=7.8cm,height=4.5cm]{5258f7.ps}\end{figure}$	Figure 6: Top: Kernel of the digital filter used for demodulation (see text for details). Bottom: Fourier power spectrum of the digital filter compared to a square filter, to the beam pattern and to the bolometer time constant.
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$\begin{figure} \par\includegraphics[scale=0.38,angle=90]{5258f8.ps} \end{figure}$	Figure 7: Top: Fourier power spectrum of KS3 143K01 bolometer data showing the frequency peaks produced by the readout electronic noise. Bottom: Same after preprocessing. The amplitude of the peaks is significantly reduced.
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$\begin{figure} \par\includegraphics[height=8cm,width=8.5cm,clip]{5258f9.eps} \end{figure}$	Figure 8: Rotation period evolution during the KS3 flight.
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$\begin{figure} \par\includegraphics[height=8cm,keepaspectratio=true]{5258f10.eps}\end{figure}$	Figure 9: Evolution of the distribution of phase differences between signals and bright stars for the KS3 flight.
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$\begin{figure} \par\includegraphics[height=8cm,keepaspectratio=true]{5258f11.eps}\end{figure}$	Figure 10: Distribution of the axial distance of bright stars versus the diode number of the corresponding intense signals. Notice the strange behavior of the diode 26. This diode is excluded from analysis.
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$\begin{figure} \par\includegraphics[height=8cm,keepaspectratio=true]{5258f12.eps}\end{figure}$	Figure 11: Scatter plot of the phase differences in degrees between signals and associated stars for each FSS diode.
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$\begin{figure} \par\includegraphics[height=5cm,width=5cm]{5258f13.eps} \includegraphics[height=5cm,width=5cm]{5258f14.ps}\end{figure}$	Figure 12: From top to bottom, distribution of errors in axial distance - phase plane with 95% and 68% confidence levels (in white) before and after each scan path fit, respectively.
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$\begin{figure} \par\includegraphics[height=5cm,width=5cm]{5258f15.ps} \end{figure}$	Figure 13: KS3 flight 95% end 68% confidence levels for error distribution in equatorial coordinates after the scan-path fit.
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$\begin{figure} \par\includegraphics[width=9cm,height=6cm]{5258f16.ps} \end{figure}$	Figure 14: Top: map of Jupiter for the 143K03 bolometer in $\mu$ V before time constant deconvolution. The map is represented in the par and cross scan direction in arcmin. Bottom: As above, but after deconvolution from the time constant.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5258f17.ps} \end{figure}$	Figure 15: 217K04 Beam profile on Jupiter before (in red) and after (in black) deconvolution of the two time constants ( $\tau _1 = 5.57_{-1.08}^{+1.01}$ ms, $\alpha = 0.48_{-0.04}^{+0.04}$ and $\tau _2 = 38.38_{-4.20}^{+3.80}$ ms).
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{5258f18.ps} \end{figure}$	Figure 16: Glitch template for the bolometer 217K01. A single time constant model has been fitted to the data. For the best fit, traced in red, the time constant is $7.8\pm 0.11$ ms.
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$\begin{figure} \par\includegraphics[width=12cm,height=5cm]{5258f19.ps} \end{figure}$	Figure 17: Comparison between glitch and Jupiter short time constant estimates.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5258f20.ps} \end{figure}$	Figure 18: From top to bottom and from left to right, for the photometric pixel 143K03, the beam pattern map in $\mu$ V from Jupiter observations, its multi-Gaussian decomposition using seven 2D Gaussians, the residuals and their distribution, which is compatible with Gaussian distributed noise (red line).
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{5258f21.ps} \end{figure}$	Figure 19: Focal plane of Archeops reconstructed using Jupiter observations.
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$\begin{figure} \par\includegraphics[height=8cm,width=17cm,clip]{5258f24.ps} \end{figure}$	Figure 22: From left to right and from top to bottom, the power spectrum in $\mu$ V $/\! \sqrt{\rm Hz}$ of the time-ordered Archeops data before (black curve) and after (red curve) subtraction of the spin-frequency systematics for the 143K03, 217K06, 353K01, and 545K01 bolometers.
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$\begin{figure} \par\includegraphics[height=8cm,width=17cm,clip]{5258f25.ps} \par\end{figure}$	Figure 23: From left to right and from top to bottom, the power spectrum in $\mu$ V $/ \sqrt ({\rm Hz})$ of the low-frequency processed Archeops data before (in black) and after (in red) decorrelation from the high-frequency noise for the 143K03, 217K06, 353K01, and 545K01 bolometers, respectively.
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$\begin{figure} \par\includegraphics[height=8.5cm,width=10cm,angle=90,clip]{5258f... ...\includegraphics[height=8.5cm,width=10cm,angle=90,clip]{5258f27.eps}\end{figure}$	Figure 24: Left column: from top to bottom, time-frequency representation in linear color scale of the 217T04 bolometer data and of the expected Galactic signal for it. Right column: same for the 217K04 bolometer.
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$\begin{figure} \par\includegraphics[angle=90,height=9cm,width=9cm,clip]{5258f28.ps}\end{figure}$	Figure 25: Top: Average wavelet power spectrum in $\mu$ V of the TOD of the 217K04 Archeops bolometer as a function of frequency computed from its DWPT Bottom: Time evolution of the power spectrum of the TOD of the 217K04 Archeops bolometer computed from its DWPT.
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$\begin{figure} \par\includegraphics[scale=0.25,angle=90]{5258f29.ps}\\ [1.5mm] ... ...31.ps}\\ [1.5mm] \includegraphics[scale=0.25,angle=90]{5258f32.ps} \end{figure}$	Figure 26: From top to bottom, results of the Kolmogorov-Smirnov test on the bolometers 143K03, 217K06, 353K06, and 545K01, respectively. The white polygons correspond to intervals in the time frequency plane where the test is considered to fail (see text for details).
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$\begin{figure} \par\includegraphics[scale=0.3,angle=90]{5258f34.ps}\includegraphics[scale=0.3,angle=90]{5258f35.ps}\end{figure}$	Figure 28: From left to right, simulated and reconstructed CMB dipole maps in linear scale for the Archeops 143K03 bolometer centered on the Galactic anticenter. To reconstruct both dipole maps, the timelines have been band-pass filtered. This introduces discontinuities on the maps due to the scanning strategy.
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$\begin{figure} \par\includegraphics[scale=0.5]{5258f36.ps}\end{figure}$	Figure 29: FIRAS/Archeops Galactic profiles correlation on the Galactic plane (bolometer 353K01 at 353 GHz). Fitting a straight line gives the calibration factor.
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$\begin{figure} \par\includegraphics[scale=0.5]{5258f37.ps} \end{figure}$	Figure 30: Comparison of the Galactic and Dipole calibration factors (in ${\rm mK}/\mu {\rm V}$ ). The error bars (both statistical and systematic) are about 4% and 8% for calibration on the dipole at 143 and 217 GHz, respectively and from 6% to 15% for the calibration on the Galaxy.
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$\begin{figure} \par\includegraphics[height=5cm,width=8cm]{5258f38.ps} \end{figure}$	Figure 31: Comparison of the point-source (Jupiter and Saturn) and dipole calibration factors. The error bars are about 4% and 8% for calibration on the dipole at 143 and 217 GHz respectively and about 12% for the calibration on the sources (essentially due to the uncertainty of the thermal emission model).
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$\begin{figure} \par\mbox{\includegraphics[width=4.3cm, height=5cm]{5258f39.ps} \includegraphics[width=4.3cm, height=5cm]{5258f40.ps} } \end{figure}$	Figure 32: From left to right, Archeops Galactic profiles in $\mu$ V at constant Galactic longitude respectively before and after the intercalibration for the 353 GHz bolometers.
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$\begin{figure} \par\includegraphics[height=8.cm,keepaspectratio=true,angle=90]{... ...ludegraphics[height=8.cm,keepaspectratio=true,angle=90]{5258f42.ps}\end{figure}$	Figure 33: Left: power spectrum of the time-ordered data of the bolometer 545K01 before (black) and after (red) destriping. Right: zoom-in of the left plot at first multiples of the spinning frequency.
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