South Pole Telescope optics

Padin, S.; Staniszewski, Z.; Keisler, R.; Joy, M.; Stark, A. A.; Ade, Peter A. R.; Aird, K. A.; Benson, B. A.; Bleem, Lindsey; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Dobbs, M.; Halverson, N. W.; Heimsath, S.; Hills, R. E.; Holzapfel, W. L.; Lawrie, Craig; Lee, A. T.; Leitch, E. M.; Leong, J.; Lü, Wei; Lueker, M.; McMahon, Jeff; Meyer, S. S.; Mohr, J. J.; Montroy, T. E.; Plagge, T.; Pryke, C.; Ruhl, J. E.; Schaffer, K. K.; Shirokoff, E.; Spieler, H.; Vieira, J. D.

doi:10.1364/ao.47.004418

Cited by 77 publications

(64 citation statements)

References 11 publications

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“…The SPT is a 10 m off-axis Gregorian telescope located at the Amundsen-Scott South Pole station that we designed for dedicated measurements of the CMB (Padin et al 2008;Carlstrom et al 2011). To complement the polarizationsensitive receiver, we modified the telescope to reduce ground pickup by installing a 1 m guard ring around the 10 m primary and a small "snout" near prime focus at the top of the receiver cabin in 2012.…”

Section: The Sptpol Instrumentmentioning

confidence: 99%

Measurements of the Temperature and E-mode Polarization of the CMB from 500 Square Degrees of SPTpol Data

Henning

Sayre

Reichardt

et al. 2018

ApJ

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209

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We present measurements of the E-mode polarization angular auto-power spectrum (EE) and temperature-E-mode cross-power spectrum (TE) of the cosmic microwave background (CMB) using 150 GHz data from three seasons of SPTpol observations. We report the power spectra over the spherical harmonic multipole range ℓ 50 8000  < and detect nine acoustic peaks in the EE spectrum with high signal-to-noise ratio. These measurements are the most sensitive to date of the EE and TE power spectra at ℓ 1050 > and ℓ 1475 > , respectively. The observations cover 500 deg 2 , a fivefold increase in area compared to previous SPTpol analyses, which increases our sensitivity to the photon diffusion damping tail of the CMB power spectra enabling tighter constraints on ΛCDM model extensions. After masking all sources with unpolarized flux 50 > mJy, we place a 95% confidence upper limit on residual polarized point-source power of D ℓ ℓ C 1 2 0.107 K ℓ ℓ 2 p m = + < ( ) at ℓ 3000 = , suggesting that the EE damping

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Section: The Sptpol Instrumentmentioning

confidence: 99%

Measurements of the Temperature and E-mode Polarization of the CMB from 500 Square Degrees of SPTpol Data

Henning

Sayre

Reichardt

et al. 2018

ApJ

Self Cite

209

264

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“…The South Pole Telescope (SPT) is a 10 m diameter telescope located at the Amundsen-Scott South Pole Station in Antarctica (Padin et al 2008;Carlstrom et al 2011). During the austral summer of 2011-2012, the polarization-sensitive SPTpol receiver was installed on the SPT.…”

Section: Cmb Data: the Sptpol Instrument And Observationsmentioning

confidence: 99%

CMB Polarization B-mode Delensing with SPTpol and Herschel

Manzotti

Story

et al. 2017

ApJ

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We present a demonstration of delensing the observed cosmic microwave background (CMB) B-mode polarization anisotropy. This process of reducing the gravitational-lensing-generated B-mode component will become increasingly important for improving searches for the B modes produced by primordial gravitational waves. In this work, we delens B-mode maps constructed from multi-frequency SPTpol observations of a 90 deg 2 patch of sky by subtracting a B-mode template constructed from two inputs: SPTpol E-mode maps and a lensing potential map estimated from the Herschel 500 μm map of the cosmic infrared background. We find that our delensing procedure reduces the measured B-mode power spectrum by 28% in the multipole range < < ℓ 300 2300; this is shown to be consistent with expectations from simulations and to be robust against systematics. The null hypothesis of no delensing is rejected at s 6.9 . Furthermore, we build and use a suite of realistic simulations to study the general properties of the delensing process and find that the delensing efficiency achieved in this work is limited primarily by the noise in the lensing potential map. We demonstrate the importance of including realistic experimental nonidealities in the delensing forecasts used to inform instrument and survey-strategy planning of upcoming lowernoise experiments, such as CMB-S4.

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“…The SPT-SZ survey (Schaffer et al 2011) used the 10 m SPT at the National Science Foundationʼs (NSF) Amundsen-Scott South Pole Station to survey a large area of the sky at millimeter and sub-millimeter wavelengths with arcminute angular resolution and low noise (Ruhl et al 2004;Padin et al 2008;Carlstrom et al 2011). The survey observed 2500 deg 2 of the southern sky during the austral winter seasons of 2008 through 2011.…”

Section: The South Pole Telescope Sz Surveymentioning

confidence: 99%

Constraining Agn Feedback in Massive Ellipticals With South Pole Telescope Measurements of the Thermal Sunyaev–zel’dovich Effect

Spacek

Scannapieco

Cohen

et al. 2016

ApJ

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Energetic feedback due to active galactic nuclei (AGNs) is likely to play an important role in the observed antihierarchical trend in the evolution of galaxies, and yet the energy injected into the circumgalactic medium by this process is largely unknown. One promising approach to constrain this feedback is through measurements of spectral distortions in the cosmic microwave background due to the thermal Sunyaev-Zeldovich (tSZ) effect, whose magnitude is directly proportional to the energy input by AGNs. With current instruments, making such measurements requires stacking large numbers of objects to increase signal-to-noise. While one possible target for such stacks is AGNs themselves, these are relatively scarce sources that contain contaminating emission that complicates tSZ measurements. Here we adopt an alternative approach and co-add South Pole Telescope SZ (SPT-SZ) survey data around a large set of massive quiescent elliptical galaxies at  z 0.5, which are much more numerous and less contaminated than active AGNs, yet are subject to the same feedback processes from the AGNs they hosted in the past. We use data from the Blanco Cosmology Survey and VISTA Hemisphere Survey to create a large catalog of galaxies split up into two redshift bins: one with 3394 galaxies at   z 0.5 1.0 and one with 924 galaxies at   z 1.0 1.5, with typical stellar masses of´ M 1.5 10 . 11We then co-add the emission around these galaxies, resulting in a measured tSZ signal at s 2.2 significance for the lower redshift bin and a contaminating signal at s 1.1 for the higher redshift bin. To remove contamination due to dust emission, we use SPT-SZ source counts to model a contaminant source population in both the SPT-SZ bands and Planck highfrequency bands for a subset of 937 galaxies in the low-redshift bin and 240 galaxies in the high-redshift bin. This increases our detection to s 3.6 for low redshifts and s 0.9 for high redshifts. We find the mean angularly integrated Compton-y values to be- 60 erg, respectively. These numbers are higher than expected from simple theoretical models that do not include AGN feedback, and serve as constraints that can be applied to current simulations of massive galaxy formation.

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South Pole Telescope optics

Cited by 77 publications

References 11 publications

Measurements of the Temperature and E-mode Polarization of the CMB from 500 Square Degrees of SPTpol Data

Measurements of the Temperature and E-mode Polarization of the CMB from 500 Square Degrees of SPTpol Data

CMB Polarization B-mode Delensing with SPTpol and Herschel

Constraining Agn Feedback in Massive Ellipticals With South Pole Telescope Measurements of the Thermal Sunyaev–zel’dovich Effect

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