Feedhorn-coupled TES polarimeter camera modules at 150 GHz for CMB polarization measurements with SPTpol

Henning, J. W.; Aird, K. A.; Austermann, J. E.; Beall, James A.; Becker, Daniel; Benson, B. A.; Bleem, L. E.; Britton, J.; Carlstrom, J. E.; Chang, C. L.; Cho, H. M.; Crawford, T. M.; Crites, A. T.; Datesman, A.; Haan, T. de; Dobbs, M.; Everett, W.; Ewall‐Wice, Aaron; George, E. M.; Halverson, N. W.; Harrington, N. L.; Hilton, G. C.; Holzapfel, W. L.; Hubmayr, J.; Irwin, K. D.; Karfunkle, M.; Keisler, R.; Kennedy, James E.; Lee, A. T.; Leitch, E. M.; Li, D.; Lueker, M.; Marrone, Dan; McMahon, Jeff; Mehl, J.; Meyer, S. S.; Montgomery, J.; Montroy, T. E.; Nagy, Johanna; Natoli, T.; Nibarger, J. P.; Niemack, Michael D.; Novosad, V.; Padin, S.; Pryke, C.; Reichardt, Christian; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Schaffer, K. K.; Shirokoff, E.; Story, K. T.; Tucker, C.; Vanderlinde, K.; Vieira, J. D.; Wang, G.; Williamson, A. R.; Yefremenko, V.; Yoon, K. W.; Young, E.

doi:10.1117/12.927172

Cited by 24 publications

(24 citation statements)

References 28 publications

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“…In CMB experiments in which TES bolometers are readout with frequency division SQUID multiplexing electronics, such as SPTpol [10], [11], R T ES ≈ 0.8 ∼ 0.9 Ω, T T ES ≈ 0.5 K, P ≈ 15 pW, and L ≈ 24 μH. Therefore, the upper limit of the thermal loop gain L can be around 30 for a natural time constant of C 0 /G ≈ 10 ms.…”

mentioning

confidence: 98%

Mo/Au Bilayer TES Resistive Transition Engineering

Wang

Chang

Yefremenko

et al. 2015

IEEE Trans. Appl. Supercond.

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We have investigated two types of superconducting transition edge sensor (TES) modified with structures on the surface. One is a Mo/Au TES modified with Nb stripes, which increase the transition temperature and broaden the transition width. Another is a Mo/Au TES modified with Au stripes, which decrease the transition temperature and broaden the transition width. It is experimentally demonstrated that the resistive transition profile of a TES can be desirably engineered with a superconductor and/or a normal metal by properly choosing the width and spacing of the modification stripes on the surface.Index Terms-Bolometer, proximity effect, superconductivity, transition edge sensor.

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mentioning

confidence: 98%

Mo/Au Bilayer TES Resistive Transition Engineering

Wang

Chang

Yefremenko

et al. 2015

IEEE Trans. Appl. Supercond.

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“…A full description of the design of the 150 GHz modules and detector architecture can be found elsewhere in these proceedings. 3 The modules are arranged in a hexagonal close-packed arrangement in the center of the focal plane.…”

Section: Focal Planementioning

confidence: 99%

“…The full complement of 150 GHz detectors consists of 7 arrays of 84 ortho-mode transducers (OMTs) stripline coupled to two TES detectors each. 3 Each of the 180 pixels at 90 GHz consists of two antenna-coupled absorbers coupled to two TES detectors. 4 Both types of detectors are feedhorn coupled to the telescope.…”

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confidence: 99%

Performance and on-sky optical characterization of the SPTpol instrument

George

Aird

Austermann³

et al. 2012

SPIE Proceedings

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In January 2012, the 10m South Pole Telescope (SPT) was equipped with a polarization-sensitive camera, SPTpol, in order to measure the polarization anisotropy of the cosmic microwave background (CMB). Measurements of the polarization of the CMB at small angular scales (∼several arcminutes) can detect the gravitational lensing of the CMB by large scale structure and constrain the sum of the neutrino masses. At large angular scales (∼few degrees) CMB measurements can constrain the energy scale of Inflation. SPTpol is a two-color mm-wave camera that consists of 180 polarimeters at 90 GHz and 588 polarimeters at 150 GHz, with each polarimeter consisting of a dual transition edge sensor (TES) bolometers. The full complement of 150 GHz detectors consists of 7 arrays of 84 ortho-mode transducers (OMTs) that are stripline coupled to two TES detectors per OMT, developed by the TRUCE collaboration and fabricated at NIST. Each 90 GHz pixel consists of two antenna-coupled absorbers coupled to two TES detectors, developed with Argonne National Labs. The 1536 total detectors are read out with digital frequency-domain multiplexing (DfMUX). The SPTpol deployment represents the first on-sky tests of both of these detector technologies, and is one of the first deployed instruments using DfMUX readout technology. We present the details of the design, commissioning, deployment, on-sky optical characterization and detector performance of the complete SPTpol focal plane.

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“…The polarisation-sensitive SPTpol receiver was installed on the South Pole Telescope in the austral summer of 2011-2012. The receiver has 180 and 588 polarisation-sensitive pixels at 95 and 150 GHz respectively (Sayre et al 2012;Henning et al 2012). The angular resolution at these frequencies is approximately 1.…”

Section: The 500 Deg 2 Sptpol Surveymentioning

confidence: 99%

Fractional polarization of extragalactic sources in the 500 deg2 SPTpol survey

Gupta

Reichardt

Ade

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the polarisation properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg 2 survey. We estimate the polarised power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarised power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarisation fraction p 2 = [8.9 ± 1.1] × 10 −4 at 95 GHz and [6.9 ± 1.1] × 10 −4 at 150 GHz for the full sample. This is consistent with the values obtained for a sub-sample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of p 2 95 < 16.9 × 10 −3 and p 2 150 < 2.6 × 10 −3 . We find no evidence that the polarisation fraction depends on the source flux or observing frequency. The 1-σ upper limit on measured mean squared polarisation fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarisation power spectra out to at least 5700 ( 4700) and 5300 ( 3600), respectively at 95 (150) GHz.

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Feedhorn-coupled TES polarimeter camera modules at 150 GHz for CMB polarization measurements with SPTpol

Cited by 24 publications

References 28 publications

Mo/Au Bilayer TES Resistive Transition Engineering

Mo/Au Bilayer TES Resistive Transition Engineering

Performance and on-sky optical characterization of the SPTpol instrument

Fractional polarization of extragalactic sources in the 500 deg2 SPTpol survey

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