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Journal of Low Temperature Physics

, Volume 184, Issue 3–4, pp 534–539 | Cite as

Characterizing Atacama B-mode Search Detectors with a Half-Wave Plate

  • S. M. Simon
  • J. W. Appel
  • L. E. Campusano
  • S. K. Choi
  • K. T. Crowley
  • T. Essinger-Hileman
  • P. Gallardo
  • S. P. Ho
  • A. Kusaka
  • F. Nati
  • G. A. Palma
  • L. A. Page
  • S. Raghunathan
  • S. T. Staggs
Article

Abstract

The Atacama B-Mode Search (ABS) instrument is a cryogenic (\(\sim \)10 K) crossed-Dragone telescope located at an elevation of 5190 m in the Atacama Desert in Chile that observed for three seasons between February 2012 and October 2014. ABS observed the cosmic microwave background (CMB) at large angular scales (\(40<\ell <500\)) to limit the B-mode polarization spectrum around the primordial B-mode peak from inflationary gravity waves at \(\ell \sim 100\). The ABS focal plane consists of 480 transition-edge sensor (TES) bolometers. They are coupled to orthogonal polarizations from a planar ortho-mode transducer and observe at 145 GHz. ABS employs an ambient-temperature, rapidly rotating half-wave plate (HWP) to mitigate systematic effects and move the signal band away from atmospheric 1 / f noise, allowing for the recovery of large angular scales. We discuss how the signal at the second harmonic of the HWP rotation frequency can be used for data selection and for monitoring the detector responsivities.

Keywords

Atacama B-mode Search Cosmic microwave background  Polarization Half-wave plate 

Notes

Acknowledgments

This work is supported by a NASA Space Technology Research Fellowship. Work at NIST is supported by the NIST Innovations in Measurement Science Program. Work at Princeton University is supported by the NSF through Awards PHY-0355328 and PHY-085587, NASA through award NNX08AE03G, and Wilkinson Misrahi funds. PWV measurements were provided by APEX. SR acknowledges his CONICYT Ph.D. studentship, CONICYT Anillo Project (ACT No. 1122), and the Aspen Center for Physics, which is supported by National Science Foundation Grant PHY-1066293. A. K. was supported by a Dicke Fellowship. This work was supported in part by the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.

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Copyright information

© Springer Science+Business Media New York 2015

Authors and Affiliations

  • S. M. Simon
    • 1
  • J. W. Appel
    • 2
  • L. E. Campusano
    • 3
  • S. K. Choi
    • 1
  • K. T. Crowley
    • 1
  • T. Essinger-Hileman
    • 2
  • P. Gallardo
    • 4
  • S. P. Ho
    • 1
  • A. Kusaka
    • 1
    • 5
  • F. Nati
    • 6
  • G. A. Palma
    • 7
  • L. A. Page
    • 1
  • S. Raghunathan
    • 3
  • S. T. Staggs
    • 1
  1. 1.Department of PhysicsPrinceton UniversityPrincetonUSA
  2. 2.Department of Physics and AstronomyJohns Hopkins UniversityBaltimoreUSA
  3. 3.Departamento de AstronomiaUniversidad de ChileSantiagoChile
  4. 4.Department of PhysicsCornell UniversityIthacaUSA
  5. 5.Physics DivisionLawrence Berkeley National LabBerkeleyUSA
  6. 6.Department of Physics and AstronomyUniversity of PennsylvaniaPhiladelphiaUSA
  7. 7.Departamento de FisicaUniversidad de Chile FCFMSantiagoChile

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