An Overview of the SPTpol Experiment

作者：Bleem L^*; Ade P; Aird K; Austermann J; Beall J; Becker D; Benson B; Britton J; Carlstrom J; Chang C L; Cho H; de Haan T; Crawford T; Crites A; Datesman A; Dobbs M; Everett W; Ewall Wice A; George E; Halverson N; Harrington N; Henning J; Hilton G; Holzapfel W; Hoover S; Hubmayr J; Irwin K; Keisler R; Kennedy J; Lee A; Leitch E; Li D; Lueker M; Marrone D P; McMahon J; Mehl J; Meyer S; Montgomery J; Montroy T

来源：Journal of Low Temperature Physics, 2012, 167(5-6): 859-864.

DOI：10.1007/s10909-012-0505-y

• Polarimetry
• Transition-edge sensors
• Bolometers
• Cosmic microwave background
• Cosmology

In 2012 the South Pole Telescope (SPT) will begin a 625 deg(2) survey to measure the polarization anisotropy of the cosmic microwave background (CMB). Observations of the CMB B-mode angular power spectrum will be used to search for the large angular scale signal induced by inflationary gravitational waves. Additionally, the B-mode spectrum will enable a measurement of the neutrino mass through the gravitational lensing of the CMB. The new 780 pixel polarization-sensitive camera is composed of two different detector architectures and will map the sky at two frequencies. At 150 GHz, the camera consists of arrays of corrugated feedhorn-coupled TES polarimeters fabricated at the National Institute of Standards and Technology (NIST). At 90 GHz, we use individually packaged dual-polarization absorber-coupled polarimeters developed at Argonne National Laboratory. Each 90 GHz pixel couples to the telescope through machined contoured feedhorns. The entire focal plane is read out using a digital frequency-domain multiplexer system. We discuss the design and goals of this experiment and provide a description of the detectors.

• 出版日期2012-6
• 单位McGill