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Fig. 5


Comparison of BB angular power spectrum error bars (in μK2) for the HWP setups under consideration. The spectra have been estimated by an implementation of the MASTER pseudo-Cl method from 50 N, S and S+N Monte Carlo maps. The error bars correspond to the standard deviation of the realizations (i.e. the dispersion of the simulations). The spectra have been produced assuming a couple of detectors for one day of operation. We note that the noise-only maps have been rescaled by a factor ~28.7, as (optimistically) expected by extending the observation to 110 detectors and 15 days. First column: HWP stepped every 1 s (solid black line), 60 s (dotted red line) and 3600 s (dashed blue line), for a telescope scanning at 12 deg/s (top) and 0.7 deg/s (bottom). Second column: HWP spinning at 5 Hz (in solid black line), 2 Hz (dotted red line) and 0.5 Hz (dashed blue line), for a telescope scanning at 12 deg/s (top) and 0.7 deg/s (bottom).

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