The 10 Meter South Pole Telescope

Carlstrom, J. E.; Ade, Peter A. R.; Aird, K. A.; Benson, B. A.; Bleem, L. E.; Busetti, S.; Chang, C. L.; Chauvin, Eric; Cho, H.-M.; Crawford, T. M.; Crites, A. T.; Dobbs, M.; Halverson, N. W.; Heimsath, S.; Holzapfel, W. L.; Hrubes, J. D.; Joy, M.; Keisler, R.; Lanting, T.; Lee, A. T.; Leitch, E. M.; Leong, J.; Lü, Wei; Lueker, M.; Luong-Van, D.; McMahon, Jeff; Mehl, J.; Meyer, S. S.; Mohr, J. J.; Montroy, T. E.; Padin, S.; Plagge, T.; Pryke, C.; Ruhl, J. E.; Schaffer, K. K.; Schwan, D.; Shirokoff, E.; Spieler, H.; Staniszewski, Z.; Stark, A. A.; Tucker, C.; Vanderlinde, K.; Vieira, J. D.; Williamson, A. R.

doi:10.1086/659879

Cited by 572 publications

(384 citation statements)

References 39 publications

Supporting

Mentioning

383

Contrasting

Order By: Relevance

“…The SPTpol instrument replaced the SPT-SZ instrument on the SPT, and the outer shell of the receiver cryostat is an exact duplicate of the SPT-SZ instrument. As such, the same secondary mirror and optics cryostat 6 was reused for SPTpol. The thermal filters near prime focus in are tilted and AR coated for SPTpol to prevent polarized reflections from reaching the focal plane.…”

Section: Cold Stop and Radiation Shieldsmentioning

confidence: 99%

Performance and on-sky optical characterization of the SPTpol instrument

George

Aird

Austermann³

et al. 2012

SPIE Proceedings

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Cold Stop and Radiation Shieldsmentioning

confidence: 99%

Performance and on-sky optical characterization of the SPTpol instrument

George

Aird

Austermann³

et al. 2012

SPIE Proceedings

Self Cite

View full text Add to dashboard Cite

show abstract

“…CMB Data: The South Pole Telescope (SPT) [14] is a 10-meter telescope located at the geographic South Pole. Here we use data from SPTpol, a polarizationsensitive receiver installed on the telescope in January 2012.…”

mentioning

confidence: 99%

Detection ofB-Mode Polarization in the Cosmic Microwave Background with Data from the South Pole Telescope

Hanson¹,

Hoover²,

Crites³

et al. 2013

Phys. Rev. Lett.

Self Cite

310

165

View full text Add to dashboard Cite

Gravitational lensing of the cosmic microwave background generates a curl pattern in the observed polarization. This "B-mode" signal provides a measure of the projected mass distribution over the entire observable Universe and also acts as a contaminant for the measurement of primordial gravitywave signals. In this Letter we present the first detection of gravitational lensing B modes, using first-season data from the polarization-sensitive receiver on the South Pole Telescope (SPTpol). We construct a template for the lensing B-mode signal by combining E-mode polarization measured by SPTpol with estimates of the lensing potential from a Herschel -SPIRE map of the cosmic infrared background. We compare this template to the B modes measured directly by SPTpol, finding a non-zero correlation at 7.7σ significance. The correlation has an amplitude and scale-dependence consistent with theoretical expectations, is robust with respect to analysis choices, and constitutes the first measurement of a powerful cosmological observable. [2,3]. B modes are not generated at linear order in perturbation theory by the scalar perturbations which are the dominant source of CMB temperature and E-mode anisotropies. Because of this, B modes are of great interest as a clean probe of two more subtle signals: (1) primordial tensor perturbations in the early Universe [4,5], the measurement of which would provide a unique probe of the energy scale of inflation; and (2) gravitational lensing, which generates a distinctive nonGaussian B-mode signal [6] that can be used to measure the projected mass distribution and constrain cosmological parameters such as the sum of neutrino masses (for a review, see [7]).Previous experiments have placed upper limits on the B-mode polarization anisotropy [8][9][10][11]. In this Letter we present the first detection of B modes sourced by gravitational lensing, using first-season data from SPTpol, the polarization-sensitive receiver on the South Pole Telescope.Gravitational lensing remaps the observed position of CMB anisotropies asn →n+∇φ(n), where φ is the CMB lensing potential [12]. This remapping mixes some of the (relatively) large E-mode signal into B. The induced B mode at Fourier wavevector l B is given to first order in φ as [13]

show abstract

“…It works at high frequencies (up to 500 GHz), which cannot be observed from the ground, and with angular resolution higher than the recent Planck survey (Planck Collaboration, 2011a). At ∼ 450 GHz (near the positive maximum of the SZ spectral brightness), the angular resolution of OLIMPO is comparable to the resolution of the 10 m class mm-wave telescopes operating at ∼ 140 GHz in Antarctica (see Carlstrom et al 2011) and in Atacama (see Swetz et al 2011 andSchwan et al 2011). The OLIMPO payload has been recently upgraded with a lossless, differential, low-resolution (6 GHz), Fourier transform spectrometer (DFTS), which was placed as a plug-in between the rear part of the primary mirror and the window of the cryostat (see Fig.…”

Section: Olimpomentioning

confidence: 86%