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4 August 2010 The Primordial Inflation Polarization Explorer (PIPER): optical design
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The balloon-borne PIPER instrument will observe the polarization in the cosmic microwave background (CMB) at 200, 270, 350, and 600 GHz. Two co-pointed telescopes are placed inside a 3000 L liquid helium dewar and cooled to 1.5 K. The telescopes are arranged so that one measures Stokes parameters Q and V while the other measures U and V . Each telescope consists of a variable-delay polarization modulator (VPM) as the primary optical element, two off-axis mirrors, a folding flat, and re-imaging optics with off-axis lenses that focus each of the orthogonal linear polarization signals through an analyzer grid and onto two bolometer arrays (one for each polarization state). A cold Lyot stop is imaged onto the VPM to define the entrance pupil of the telescope. Each telescope has a 6° × 4.7° field-of-view.
© (2010) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Joseph R. Eimer, Peter A. R. Ade, Dominic J. Benford, Charles L. Bennett, David T. Chuss, Dale J. Fixsen, Alan J. Kogut, Paul Mirel, Carole E. Tucker, George M. Voellmer, and Edward J. Wollack "The Primordial Inflation Polarization Explorer (PIPER): optical design", Proc. SPIE 7733, Ground-based and Airborne Telescopes III, 77333B (4 August 2010);


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