Cosmic microwave background (CMB) polarimetry has the potential to provide revolutionary advances in cosmology. Future experiments to detect the very weak B-mode signal in CMB polarization maps will require unprecedented sensitivity and control of systematic errors. Bolometric interferometry may provide a way to achieve these goals. In a bolometric interferometer (or other adding interferometer), phase shift sequences are applied to the inputs in order to recover the visibilities. Noise is minimized when the phase shift sequences corresponding to all visibilities are orthogonal. We present a systematic method for finding sequences that produce this orthogonality, approximately minimizing both the length of the time sequence and the number of discrete phase shift values required. When some baselines are geometrically equivalent, we can choose sequences that read out those baselines simultaneously, which has been shown to improve the signal-to-noise ratio.
Copyright © 2009 The Royal Astronomical Society. This article first appeared in Monthly Notices of the Royal Astronomical Society 393, no. 2 (January 21, 2009): 531-37. doi:10.1111/j.1365-2966.2008.14194.x.
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Hyland, Peter, Brent Follin, and Emory F. Bunn. "Phase Shift Sequences for an Sdding Interferometer." Monthly Notices of the Royal Astronomical Society 393, no. 2 (January 21, 2009): 531-37. doi:10.1111/j.1365-2966.2008.14194.x.