All Figures

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{2512_f1.eps} \end{figure}$ Figure 1: The B2K focal plane (Masi et al. 2003). The 145 GHz PSB's are located in the lower row. The upper detector row hosts unpolarised (spider web) bolometers coupled to a polarimeter.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2512_f2.eps} \end{figure}$ Figure 2: The percentual ratio, as a function of frequency, between the noise power spectrum of a single detector estimated from the S+N data (by means of the iterative procedure described in the text) and the unbiased estimate of the same noise power spectrum obtained from the noise-only timestream. The black ( lower) curve is for a single detector case, while the blue ( upper) curve is obtained with a GLS map from all eight detectors. Note the strong suppression of residual bias in this case.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=5.5cm]{2512_f3.ps}\hspace*{2m... ...}\hspace*{2mm} \includegraphics[angle=90,width=5cm]{2512_f8.ps} \end{figure}$ Figure 3: Top row: I, Q, and U maps obtained by running ROMA on eight "signal-only'' simulated timelines (one for each B2K bolometer). The display area is restricted to the "shallow'' region. Bottom row: difference maps, computed by subtracting the above maps from the simulated sky that was input to the simulations. In doing so, the original maps have been degraded to $\rm NSIDE=1024$ . Note the change in the colour scale.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=5.5cm]{2512_f9.ps}\hspace*{2m... ...s}\hspace*{2mm} \includegraphics[angle=90,width=5cm]{2512_f11.ps} \end{figure}$ Figure 4: From left to right, I, Q and U output ROMA maps on eight "signal plus noise'' simulated timelines. Assumptions for the noise properties are explained in the text.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.5cm]{2512_f12.ps}\hspace*{2mm} \includegraphics[angle=90,width=7.5cm]{2512_f13.ps} \end{figure}$ Figure 5: Left panel: difference between the input, simulated sky, and the map output by ROMA, when processing a single-detector "signal-only'' (i.e. noiseless) timeline. Both (input and output) are intensity maps; the input map was degraded to $\rm NSIDE=1024$ before subtraction. Not surprisingly, the difference is dominated by the polarisation pattern that is present in the timeline, but it cannot be properly reduced when solving for a single detector map (i.e. no polarisation map can be found). Right panel: same as left, but here the I map is estimated jointly from all eight detectors. Q and U maps are also computed but are not shown here. This figure is de facto the one displayed in the left panel, bottom row of Fig. 3, but on a different scale.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=0]{2512_f14.eps}} \end{figure}$ Figure 6: Inverse time for a single PCG iteration as a function of the number of processor elements ( $N_{\rm pe}$ ) used by ROMA, for the full B2K dataset (eight timelines, consisting of $5\times 10^7$ samples each). The machine used is an IBM Power3 RS/6000. ROMA scales optimally until $N_{\rm pe} \sim 80$ .
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{2512_f1.eps} \end{figure}$	Figure 1: The B2K focal plane (Masi et al. 2003). The 145 GHz PSB's are located in the lower row. The upper detector row hosts unpolarised (spider web) bolometers coupled to a polarimeter.
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$\begin{figure} \par\includegraphics[angle=90,width=5.5cm]{2512_f9.ps}\hspace{2m... ...s}\hspace{2mm} \includegraphics[angle=90,width=5cm]{2512_f11.ps} \end{figure}$	Figure 4: From left to right, I, Q and U output ROMA maps on eight "signal plus noise'' simulated timelines. Assumptions for the noise properties are explained in the text.
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$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[angle=0]{2512_f14.eps}} \end{figure}$	Figure 6: Inverse time for a single PCG iteration as a function of the number of processor elements ( $N_{\rm pe}$ ) used by ROMA, for the full B2K dataset (eight timelines, consisting of $5\times 10^7$ samples each). The machine used is an IBM Power3 RS/6000. ROMA scales optimally until $N_{\rm pe} \sim 80$ .
Open with DEXTER