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thumbnail Fig. 9

Univariate posterior distributions of power spectrum amplitudes for a test without (left panel) and with (right panel) foreground corrections over the full range of Fourier modes considered in this work. Red lines correspond to the true underlying cosmological power spectrum from which mock data sets were generated. The left panel clearly shows that uncorrected foreground effects yield excessive power for large-scale modes and also introduce an overall biased result. In contrast, the right panel shows results obtained from our test with foreground corrections. Clearly, a detailed treatment of all foreground effects permits us to obtain an unbiased measurement of power spectrum amplitudes over the full range of Fourier modes.

Open with DEXTER
TIME Instrument Parameters
Dish size 12 m
Instantaneous FOV $14^{prime} times 0buildrel{,prime}over{.} 43$
Survey area $1buildrel{circ}over{.} 3times 0buildrel{,prime}over{.} 43$ (1  #x00d7; 180 beams)
Number of spectrometers 32 (total), 16 per polarization
Spectral range 183–326 GHz
Spectral resolution 90–120
Survey volume 194 Mpc  #x00d7; 1.1 Mpc  #x00d7; 1240 Mpc
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