Figure 1: Approximate formula (red line) from Eq. (30) and actual values (black dots) for the number of equivalent baselines as a function of for 256 entry horns on a square compact grid. | |
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Figure 2: Power spectrum error bar ratio between an imager and a bolometric interferometer (red solid) and between an imager and a heterodyne interferometer (blue dashed). The thick lines only include the noise contribution while the thin lines also include sample variance (with a tensor to scalar ratio of 0.1). In each case we have assumed 256 horns, a sky fraction defined by the 20 degrees FWHM primary beam of the interferometers. The left panel corresponds to a 10 arcmin resolution imager and the right one to a one degree imager. The points are obtained with a precise measurement of the number of equivalent baselines and the lines are from the approximate expression given above. The green dotted line shows the region where the relative sample variance is greater than one. The ratio of the heterodyne interferometer to the imager depends on the square of the NET ratio; we have assumed 250 and 150 taken from (Samtleben et al. 2007) and Clover (North et al. 2007) at 90 GHz for Chile. It is straightforward to scale the curves for different values of the NET. | |
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