An Overview of the SPTpol Experiment

Bleem, L. E.; Ade, Peter A. R.; Aird, K. A.; Austermann, J. E.; Beall, James A.; Becker, D.; Benson, B. A.; Britton, J.; Carlstrom, J. E.; Chang, C. L.; Cho, H.; Haan, T. de; Crawford, T. M.; Crites, A. T.; Datesman, A.; Dobbs, M.; Everett, W.; Ewall‐Wice, Aaron; George, E. M.; Halverson, N. W.; Harrington, N. L.; Henning, J. W.; Hilton, G. C.; Holzapfel, W. L.; Hoover, S.; Hubmayr, Johannes; Irwin, K. D.; Keisler, R.; Kennedy, James E.; Lee, A.; Leitch, E. M.; Li, D.; Lueker, M.; Marrone, Daniel P.; McMahon, Jeffrey; Mehl, J.; Meyer, S. S.; Montgomery, J.; Montroy, T. E.; 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.; Schafer, K.; Shirokoff, E.; Story, K. T.; Vanderlinde, K.; Vieira, J. D.; Wang, G.; Williamson, A. R.; Yefremenko, V.; Yoon, K. W.; Young, E.

doi:10.1007/s10909-012-0505-y

Cited by 32 publications

(25 citation statements)

References 15 publications

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“…Clearly, a larger sample of non-SZE selected clusters with accurate mass estimates and spanning a larger redshift range is needed to resolve the issues of redshift evolution of the radio galaxy LF and to improve the constraints on the LFs at 150 and 95 GHz. More precise measurements of high frequency radio galaxy LFs will also help us to accurately estimate the incompleteness in the ongoing or upcoming SZE surveys like SPTpol (Bleem et al 2012), SPT-3G (Benson et al 2014) and CMB-S4 (Abazajian et al 2015), which are all expected to be sensitive to lower mass clusters. We are exploring such samples using the Dark Energy Survey (DES Collaboration 2005) today and are looking forward to the opportunity to examine this population of galaxies in the upcoming eROSITA X-ray survey (Merloni et al 2012;Predehl et al 2014).…”

Section: Discussionmentioning

confidence: 99%

High Frequency Cluster Radio Galaxies: Luminosity Functions and Implications for SZE Selected Cluster Samples

Gupta

Saro

Mohr

et al. 2017

Mon. Not. R. Astron. Soc.

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We study the overdensity of point sources in the direction of X-ray-selected galaxy clusters from the Meta-Catalog of X-ray detected Clusters of galaxies (MCXC; z = 0.14) at South Pole Telescope (SPT) and Sydney University Molonglo Sky Survey (SUMSS) frequencies. Flux densities at 95, 150 and 220 GHz are extracted from the 2500 deg 2 SPT-SZ survey maps at the locations of SUMSS sources, producing a multi-frequency catalog of radio galaxies. In the direction of massive galaxy clusters, the radio galaxy flux densities at 95 and 150 GHz are biased low by the cluster Sunyaev-Zel'dovich Effect (SZE) signal, which is negative at these frequencies. We employ a cluster SZE model to remove the expected flux bias and then study these corrected source catalogs. We find that the high frequency radio galaxies are centrally concentrated within the clusters and that their luminosity functions (LFs) exhibit amplitudes that are characteristically an order of magnitude lower than the cluster LF at 843 MHz. We use the 150 GHz LF to estimate the impact of cluster radio galaxies on an SPT-SZ like survey. The radio galaxy flux typically produces a small bias on the SZE signal and has negligible impact on the observed scatter in the SZE mass-observable relation. If we assume there is no redshift evolution in the radio galaxy LF then 1.8 ± 0.7 percent of the clusters with detection significance ξ ≥ 4.5 would be lost from the sample. Allowing for redshift evolution of the form (1 + z) 2.5 increases the incompleteness to 5.6 ± 1.0 percent. Improved constraints on the evolution of the cluster radio galaxy LF require a larger cluster sample extending to higher redshift.

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Section: Discussionmentioning

confidence: 99%

High Frequency Cluster Radio Galaxies: Luminosity Functions and Implications for SZE Selected Cluster Samples

Gupta

Saro

Mohr

et al. 2017

Mon. Not. R. Astron. Soc.

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“…Operating experiments from the ground and monitoring percent sky fractions have already reported the existence of acoustic oscillations for T down to the arcminute scale, namely the South Pole Telescope [SPT, see 6,7] and the Atacama Cosmology Telescope [APT, see 8,9]. Sub-orbital probes such as the E and B experiment 1 [EBEX, see 10] and POLARBEAR 2 [11], Spider [12], SPTpol [13], ACTpol [14], the Large Scale Polarisation Experiment [LSPE, see 15], QUbic [16] are designed to probe CMB polarisation looking in particular for the B modes from primordial GWs on percent sky fractions with angular resolution similar to Planck; moreover, proposals for a future post-Planck CMB satellite, aiming at an all sky study of CMB polarisation, are in preparation: see e.g. the Cosmic ORigin Explorer 3 (CORE), CMBpol 4 , the Primordial Inflation Explorer [17], and the Light (Lite) satellite for the studies of B-mode polarisation and Inflation from cosmic background Radiation Detection (LiteBIRD 5 ).…”

Section: Introductionmentioning

confidence: 99%

Maps of CMB lensing deflection from N-body simulations in Coupled Dark Energy Cosmologies

Carbone

Baldi

Pettorino

et al. 2013

J. Cosmol. Astropart. Phys.

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Abstract. We produce lensing potential and deflection-angle maps in order to simulate the weak gravitational lensing of the Cosmic Microwave Background (CMB) via ray-tracing through the COupled Dark Energy Cosmological Simulations (CoDECS), the largest suite of N-body simulations to date for interacting Dark Energy cosmologies. The constructed maps faithfully reflect the Nbody cosmic structures on a range of scales going from the arcminute to the degree scale, limited only by the resolution and extension of the simulations. We investigate the variation of the lensing pattern due to the underlying Dark Energy (DE) dynamics, characterised by different background and perturbation behaviours as a consequence of the interaction between the DE field and Cold Dark Matter (CDM). In particular, we study in detail the results from three cosmological models differing in the background and perturbations evolution at the epoch in which the lensing cross section is most effective, corresponding to a redshift of ∼ 1, with the purpose to isolate their imprints in the lensing observables, regardless of the compatibility of these models with present constraints. The scenarios investigated here include a reference ΛCDM cosmology, a standard coupled DE (cDE) scenario, and a "bouncing" cDE scenario. For the standard cDE scenario, we find that typical differences in the lensing potential result from two effects: the enhanced growth of linear CDM density fluctuations with respect to the ΛCDM case, and the modified nonlinear dynamics of collapsed structures induced by the DE-CDM interaction. As a consequence, CMB lensing highlights the DE impact in the cosmological expansion, even in the degenerate case where the amplitude of the linear matter density perturbations, parametrised through σ 8 , is the same in both the standard cDE and ΛCDM cosmologies. For the "bouncing" scenario, we find that the two opposite behaviours of the lens density contrast and of the matter abundance lead to a counterintuitive effect, making the power of the lensing signal in this model lower by 10% than in the ΛCDM scenario. Moreover, we compare the behaviour of CDM and baryons in CoDECS separately, in order to isolate effects coming from the coupling with the DE component. We find that, in the bouncing scenario, baryons show an opposite trend with respect to CDM, due to the coupling of the latter with the DE component. These results confirm the relevance of CMB lensing as a probe for DE at the early stages of cosmic acceleration, and demonstrate the reliability of N-body based large scale CMB lensing simulations in the context of DE studies.

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“…At small angular scales observations produce maps of weak lensing that constrain the sum of the neutrino masses. SPTpol is among the most sensitive CMB polarization instruments now in operation, 1 and, including Planck priors, is expected to have a 1-σ uncertainty on the sum of the neutrino masses of σ(Σm ν ) = 0.096 eV and place a constraint of σ(r) = 0.028 on the tensor-to-scalar ratio.…”

Section: Introductionmentioning

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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An Overview of the SPTpol Experiment

Cited by 32 publications

References 15 publications

High Frequency Cluster Radio Galaxies: Luminosity Functions and Implications for SZE Selected Cluster Samples

High Frequency Cluster Radio Galaxies: Luminosity Functions and Implications for SZE Selected Cluster Samples

Maps of CMB lensing deflection from N-body simulations in Coupled Dark Energy Cosmologies

Performance and on-sky optical characterization of the SPTpol instrument

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