The Q/U imaging experiment instrument

C. Bischoff; A. Brizius; I. Buder; Y. Chinone; K. Cleary; R. N. Dumoulin; A. Kusaka; R. Monsalve; S. K. Næss; L. B. Newburgh; G. Nixon; R. Reeves; K. M. Smith; K. Vanderlinde; I. K. Wehus; M. Bogdan; R. Bustos; S. E. Church; R. Davis; C. Dickinson; H. K. Eriksen; T. Gaier; J. O. Gundersen; M. Hasegawa; M. Hazumi; C. Holler; K. M. Huffenberger; W. A. Imbriale; K. Ishidoshiro; M. E. Jones; P. Kangaslahti; D. J. Kapner; C. R. Lawrence; E. M. Leitch; M. Limon; J. J. McMahon; A. D. Miller; M. Nagai; H. Nguyen; T. J. Pearson; L. Piccirillo; S. J E Radford; A. C S Readhead; J. L. Richards; D. Samtleben; M. Seiffert; M. C. Shepherd; S. T. Staggs; O. Tajima; K. L. Thompson; R. Williamson; B. Winstein; E. J. Wollack; J. T L Zwart

doi:10.1088/0004-637X/768/1/9

The Q/U imaging experiment instrument

C. Bischoff, A. Brizius, I. Buder, Y. Chinone, K. Cleary, R. N. Dumoulin, A. Kusaka, R. Monsalve, S. K. Næss, L. B. Newburgh, G. Nixon, R. Reeves, K. M. Smith, K. Vanderlinde, I. K. Wehus, M. Bogdan, R. Bustos, S. E. Church, R. Davis, C. DickinsonH. K. Eriksen, T. Gaier, J. O. Gundersen, M. Hasegawa, M. Hazumi, C. Holler, K. M. Huffenberger, W. A. Imbriale, K. Ishidoshiro, M. E. Jones, P. Kangaslahti, D. J. Kapner, C. R. Lawrence, E. M. Leitch, M. Limon, J. J. McMahon, A. D. Miller, M. Nagai, H. Nguyen, T. J. Pearson, L. Piccirillo, S. J E Radford, A. C S Readhead, J. L. Richards, D. Samtleben, M. Seiffert, M. C. Shepherd, S. T. Staggs, O. Tajima, K. L. Thompson, R. Williamson, B. Winstein, E. J. Wollack, J. T L Zwart

Research output: Contribution to journal › Article › peer-review

Abstract

The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(∼1°). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 μKs1/2) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r <0.1. The 84-element W-band polarimeter array has a sensitivity of 87 μKs1/2 at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r <0.01. The two arrays together cover multipoles in the range ℓ ∼ 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument. © 2013. The American Astronomical Society. All rights reserved.

Original language	English
Article number	9
Journal	Astrophysical Journal
Volume	768
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/768/1/9
Publication status	Published - 1 May 2013

Keywords

cosmic background radiation
cosmology: observations
instrumentation: detectors
instrumentation: polarimeters
telescopes

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10.1088/0004-637X/768/1/9

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Bischoff, C., Brizius, A., Buder, I., Chinone, Y., Cleary, K., Dumoulin, R. N., Kusaka, A., Monsalve, R., Næss, S. K., Newburgh, L. B., Nixon, G., Reeves, R., Smith, K. M., Vanderlinde, K., Wehus, I. K., Bogdan, M., Bustos, R., Church, S. E., Davis, R., ... Zwart, J. T. L. (2013). The Q/U imaging experiment instrument. Astrophysical Journal, 768(1), Article 9. https://doi.org/10.1088/0004-637X/768/1/9

@article{1127b943d0764fe7a508b505d382cadd,

title = "The Q/U imaging experiment instrument",

abstract = "The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(∼1°). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 μKs1/2) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r <0.1. The 84-element W-band polarimeter array has a sensitivity of 87 μKs1/2 at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r <0.01. The two arrays together cover multipoles in the range ℓ ∼ 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.",

keywords = "cosmic background radiation, cosmology: observations, instrumentation: detectors, instrumentation: polarimeters, telescopes",

author = "C. Bischoff and A. Brizius and I. Buder and Y. Chinone and K. Cleary and Dumoulin, {R. N.} and A. Kusaka and R. Monsalve and N{\ae}ss, {S. K.} and Newburgh, {L. B.} and G. Nixon and R. Reeves and Smith, {K. M.} and K. Vanderlinde and Wehus, {I. K.} and M. Bogdan and R. Bustos and Church, {S. E.} and R. Davis and C. Dickinson and Eriksen, {H. K.} and T. Gaier and Gundersen, {J. O.} and M. Hasegawa and M. Hazumi and C. Holler and Huffenberger, {K. M.} and Imbriale, {W. A.} and K. Ishidoshiro and Jones, {M. E.} and P. Kangaslahti and Kapner, {D. J.} and Lawrence, {C. R.} and Leitch, {E. M.} and M. Limon and McMahon, {J. J.} and Miller, {A. D.} and M. Nagai and H. Nguyen and Pearson, {T. J.} and L. Piccirillo and Radford, {S. J E} and Readhead, {A. C S} and Richards, {J. L.} and D. Samtleben and M. Seiffert and Shepherd, {M. C.} and Staggs, {S. T.} and O. Tajima and Thompson, {K. L.} and R. Williamson and B. Winstein and Wollack, {E. J.} and Zwart, {J. T L}",

year = "2013",

month = may,

day = "1",

doi = "10.1088/0004-637X/768/1/9",

language = "English",

volume = "768",

journal = "Astrophysical Journal",

issn = "1538-4357",

publisher = "American Astronomical Society",

number = "1",

}

Bischoff, C, Brizius, A, Buder, I, Chinone, Y, Cleary, K, Dumoulin, RN, Kusaka, A, Monsalve, R, Næss, SK, Newburgh, LB, Nixon, G, Reeves, R, Smith, KM, Vanderlinde, K, Wehus, IK, Bogdan, M, Bustos, R, Church, SE, Davis, R, Dickinson, C, Eriksen, HK, Gaier, T, Gundersen, JO, Hasegawa, M, Hazumi, M, Holler, C, Huffenberger, KM, Imbriale, WA, Ishidoshiro, K, Jones, ME, Kangaslahti, P, Kapner, DJ, Lawrence, CR, Leitch, EM, Limon, M, McMahon, JJ, Miller, AD, Nagai, M, Nguyen, H, Pearson, TJ, Piccirillo, L, Radford, SJE, Readhead, ACS, Richards, JL, Samtleben, D, Seiffert, M, Shepherd, MC, Staggs, ST, Tajima, O, Thompson, KL, Williamson, R, Winstein, B, Wollack, EJ & Zwart, JTL 2013, 'The Q/U imaging experiment instrument', Astrophysical Journal, vol. 768, no. 1, 9. https://doi.org/10.1088/0004-637X/768/1/9

TY - JOUR

T1 - The Q/U imaging experiment instrument

AU - Bischoff, C.

AU - Brizius, A.

AU - Buder, I.

AU - Chinone, Y.

AU - Cleary, K.

AU - Dumoulin, R. N.

AU - Kusaka, A.

AU - Monsalve, R.

AU - Næss, S. K.

AU - Newburgh, L. B.

AU - Nixon, G.

AU - Reeves, R.

AU - Smith, K. M.

AU - Vanderlinde, K.

AU - Wehus, I. K.

AU - Bogdan, M.

AU - Bustos, R.

AU - Church, S. E.

AU - Davis, R.

AU - Dickinson, C.

AU - Eriksen, H. K.

AU - Gaier, T.

AU - Gundersen, J. O.

AU - Hasegawa, M.

AU - Hazumi, M.

AU - Holler, C.

AU - Huffenberger, K. M.

AU - Imbriale, W. A.

AU - Ishidoshiro, K.

AU - Jones, M. E.

AU - Kangaslahti, P.

AU - Kapner, D. J.

AU - Lawrence, C. R.

AU - Leitch, E. M.

AU - Limon, M.

AU - McMahon, J. J.

AU - Miller, A. D.

AU - Nagai, M.

AU - Nguyen, H.

AU - Pearson, T. J.

AU - Piccirillo, L.

AU - Radford, S. J E

AU - Readhead, A. C S

AU - Richards, J. L.

AU - Samtleben, D.

AU - Seiffert, M.

AU - Shepherd, M. C.

AU - Staggs, S. T.

AU - Tajima, O.

AU - Thompson, K. L.

AU - Williamson, R.

AU - Winstein, B.

AU - Wollack, E. J.

AU - Zwart, J. T L

PY - 2013/5/1

Y1 - 2013/5/1

N2 - The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(∼1°). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 μKs1/2) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r <0.1. The 84-element W-band polarimeter array has a sensitivity of 87 μKs1/2 at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r <0.01. The two arrays together cover multipoles in the range ℓ ∼ 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument. © 2013. The American Astronomical Society. All rights reserved.

AB - The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(∼1°). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 μKs1/2) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r <0.1. The 84-element W-band polarimeter array has a sensitivity of 87 μKs1/2 at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r <0.01. The two arrays together cover multipoles in the range ℓ ∼ 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument. © 2013. The American Astronomical Society. All rights reserved.

KW - cosmic background radiation

KW - cosmology: observations

KW - instrumentation: detectors

KW - instrumentation: polarimeters

KW - telescopes

U2 - 10.1088/0004-637X/768/1/9

DO - 10.1088/0004-637X/768/1/9

M3 - Article

SN - 1538-4357

VL - 768

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 9

ER -

The Q/U imaging experiment instrument

Abstract

Keywords

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