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1. Simultaneous Millimeter-wave, Gamma-Ray, and Optical Monitoring of the Blazar PKS 2326-502 during a Flaring State

Author

Hood, JC, Simpson, A, McDaniel, A, Foster, A, Ade, PAR, Ajello, M, Anderson, AJ, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chaubal, P, Chiang, HC, Chou, T-L, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gupta, N, Halverson, NW, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Madejski, G, Malkan, M, McMahon, JJ, Meyer, SS, Montgomery, J, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Omori, Y, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Tucker, C, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, Yefremenko, V, Zebrowski, JA, and Zhang, L

Subjects
Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

Abstract Including millimeter-wave data in multiwavelength studies of the variability of active galactic nuclei (AGN) can provide insights into AGN physics that are not easily accessible at other wavelengths. We demonstrate in this work the potential of cosmic microwave background (CMB) telescopes to provide long-term, high-cadence millimeter-wave AGN monitoring over large fractions of sky. We report on a pilot study using data from the SPTpol instrument on the South Pole Telescope (SPT), which was designed to observe the CMB at arcminute and larger angular scales. Between 2013 and 2016, SPTpol was used primarily to observe a single 500 deg2 field, covering the entire field several times per day with detectors sensitive to radiation in bands centered at 95 and 150 GHz. We use SPT 150 GHz observations to create AGN light curves, and we compare these millimeter-wave light curves to those at other wavelengths, in particular γ-ray and optical. In this Letter, we focus on a single source, PKS 2326-502, which has extensive, day-timescale monitoring data in gamma-ray, optical, and now millimeter-wave between 2013 and 2016. We find PKS 2326-502 to be in a flaring state in the first 2 yr of this monitoring, and we present a search for evidence of correlated variability between millimeter-wave, optical R-band, and γ-ray observations. This pilot study is paving the way for AGN monitoring with current and upcoming CMB experiments such as SPT-3G, Simons Observatory, and CMB-S4, including multiwavelength studies with facilities such as Vera C. Rubin Observatories Large Synoptic Survey Telescope.

Published
2023

2. Optimal Cosmic Microwave Background Lensing Reconstruction and Parameter Estimation with SPTpol Data

Author

Millea, M, Daley, CM, Chou, T-L, Anderes, E, Ade, PAR, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chaubal, P, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Goeckner-Wald, N, Guns, S, Gupta, N, Halverson, NW, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, McMahon, JJ, Meyer, SS, Mocanu, LM, Montgomery, J, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Omori, Y, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Thorne, B, Tucker, C, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, and Yefremenko, V

Subjects
Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We perform the first simultaneous Bayesian parameter inference and optimal reconstruction of the gravitational lensing of the cosmic microwave background (CMB), using 100 deg2 of polarization observations from the SPTpol receiver on the South Pole Telescope. These data reach noise levels as low as 5.8 µK arcmin in polarization, which are low enough that the typically used quadratic estimator (QE) technique for analyzing CMB lensing is significantly suboptimal. Conversely, the Bayesian procedure extracts all lensing information from the data and is optimal at any noise level. We infer the amplitude of the gravitational lensing potential to be A f =0.949\,\pm \,0.122 using the Bayesian pipeline, consistent with our QE pipeline result, but with 17% smaller error bars. The Bayesian analysis also provides a simple way to account for systematic uncertainties, performing a similar job as frequentist "bias hardening"or linear bias correction, and reducing the systematic uncertainty on A f due to polarization calibration from almost half of the statistical error to effectively zero. Finally, we jointly constrain A f along with A L, the amplitude of lensing-like effects on the CMB power spectra, demonstrating that the Bayesian method can be used to easily infer parameters both from an optimal lensing reconstruction and from the delensed CMB, while exactly accounting for the correlation between the two. These results demonstrate the feasibility of the Bayesian approach on real data, and pave the way for future analysis of deep CMB polarization measurements with SPT-3G, Simons Observatory, and CMB-S4, where improvements relative to the QE can reach 1.5 times tighter constraints on A f and seven times lower effective lensing reconstruction noise.

Published
2021

3. Measurements of B-mode polarization of the cosmic microwave background from 500 square degrees of SPTpol data

Author

Sayre, JT, Reichardt, CL, Henning, JW, Ade, PAR, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chaubal, P, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Gupta, N, Halverson, NW, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, McMahon, JJ, Meyer, SS, Mocanu, LM, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Padin, S, Patil, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, and Yefremenko, V

Subjects
Particle and High Energy Physics, Physical Sciences, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics, Mathematical physics, Astronomical sciences, Particle and high energy physics
Abstract

We report a B-mode power spectrum measurement from the cosmic microwave background (CMB) polarization anisotropy observations made using the SPTpol instrument on the South Pole Telescope. This work uses 500 deg2 of SPTpol data, a five-fold increase over the last SPTpol B-mode release. As a result, the bandpower uncertainties have been reduced by more than a factor of two, and the measurement extends to lower multipoles: 52< 320.

Published
2020

4. Galaxy Clusters Selected via the Sunyaev–Zel’dovich Effect in the SPTpol 100-square-degree Survey

Author

Huang, N, Bleem, LE, Stalder, B, Ade, PAR, Allen, SW, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Floyd, B, Gallicchio, J, George, EM, Gilbert, A, Gladders, MD, Guns, S, Gupta, N, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Hubmayr, J, Irwin, KD, Khullar, G, Knox, L, Lee, AT, Li, D, Lowitz, A, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Sharon, K, Sievers, C, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, and Yefremenko, V

Subjects
Space Sciences, Physical Sciences, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics
Abstract

We present a catalog of galaxy cluster candidates detected in 100 square degrees surveyed with the SPTpol receiver on the South Pole Telescope. The catalog contains 89 candidates detected with a signal-to-noise ratio greater than 4.6. The candidates are selected using the Sunyaev-Zel'dovich effect at 95 and 150 GHz. Using both space- and ground-based optical and infrared telescopes, we have confirmed 81 candidates as galaxy clusters. We use these follow-up images and archival images to estimate photometric redshifts for 66 galaxy clusters and spectroscopic observations to obtain redshifts for 13 systems. An additional two galaxy clusters are confirmed using the overdensity of near-infrared galaxies only and are presented without redshifts. We find that 15 candidates (18% of the total sample) are at redshift z ≥ 1.0, with a maximum confirmed redshift of zmax = 1.38 ± 0.10. We expect this catalog to contain every galaxy cluster with M500c = 2.6 ×1014M⊙ h70-1 and z > 0.25 in the survey area. The mass threshold is approximately constant above z = 0.25, and the complete catalog has a median mass of approximately M500c = 2.7 ×1014M⊙ h70-1. Compared to previous SPT works, the increased depth of the millimeter-wave data (11.2 and 6.5 μK-arcmin at 95 and 150 GHz, respectively) makes it possible to find more galaxy clusters at high redshift and lower mass.

Published
2020

5. Constraints on Cosmological Parameters from the 500 deg2 SPTPOL Lensing Power Spectrum

Author

Bianchini, F, Wu, WLK, Ade, PAR, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chaubal, P, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Gupta, N, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, G, Novosad, V, Omori, Y, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Sievers, C, Simard, G, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, and Yefremenko, V

Subjects
Particle and High Energy Physics, Physical Sciences, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg2 SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO), as well as primary CMB spectra from Planck and SPTpol. The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analyzed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on. Jointly fitting with BAO data, we find away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. The SPTpol lensing spectrum constrains the spatial curvature to be and the sum of the neutrino masses to be eV at 95% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. With the differences in the signal-to-noise ratio of the lensing modes and the angular scales covered in the lensing spectra, this analysis represents an important independent check on the full-sky Planck lensing measurement.

Published
2020

6. Fractional Polarisation of Extragalactic Sources in the 500-square-degree SPTpol Survey

Author

Gupta, N, Reichardt, CL, Ade, PAR, Anderson, AJ, Archipley, M, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Feng, C, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, GI, Novosad, V, Padin, S, Patil, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Sievers, C, Smecher, G, Staniszewski, Z, Stark, AA, Story, KT, Switzer, ER, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Williamson, R, Wu, WLK, Yefremenko, V, and Zhang, L

Subjects
Astronomical Sciences, Physical Sciences, polarization, galaxies: active, cosmology: observations, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We study the polarization properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarized power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarized 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 polarization fraction 〈p2〉= [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 subsample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 〈p2〉95 < 16.9 × 10−3 and 〈p2〉150 < 2.6 × 10−3. We find no evidence that the polarization fraction depends on the source flux or observing frequency. The 1σ upper limit on measured mean-squared polarization fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarization power spectra out to at least ℓ ≲ 5700 (ℓ ≲ 4700) and ℓ ≲ 5300 (ℓ ≲ 3600), respectively, at 95 (150) GHz.

Published
2019

7. Fractional polarization of extragalactic sources in the 500 deg2 SPTpol survey

Author

Gupta, N, Reichardt, CL, Ade, PAR, Anderson, AJ, Archipley, M, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Corbett Moran, C, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Feng, C, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, GI, Novosad, V, Padin, S, Patil, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Sievers, C, Smecher, G, Staniszewski, Z, Stark, AA, Story, KT, Switzer, ER, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Williamson, R, Wu, WLK, Yefremenko, V, and Zhang, L

Subjects
polarization, galaxies: active, cosmology: observations, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We study the polarization properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarized power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarized 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 polarization fraction 〈p2〉= [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 subsample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 〈p2〉95 < 16.9 × 10−3 and 〈p2〉150 < 2.6 × 10−3. We find no evidence that the polarization fraction depends on the source flux or observing frequency. The 1σ upper limit on measured mean-squared polarization fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarization power spectra out to at least ℓ ≲ 5700 (ℓ ≲ 4700) and ℓ ≲ 5300 (ℓ ≲ 3600), respectively, at 95 (150) GHz.

Published
2019

8. A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg2 of SPTpol Temperature and Polarization Data

Author

Wu, WLK, Mocanu, LM, Ade, PAR, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Gupta, N, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Meyer, SS, Millea, M, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, GI, Novosad, V, Omori, Y, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Sievers, C, Simard, G, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, and Yefremenko, V

Subjects
Particle and High Energy Physics, Physical Sciences, cosmology: cosmic background radiation, large-scale structure of the universe, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present a measurement of the cosmic microwave background lensing potential using 500 deg2 of 150 GHz data from the SPTpol receiver on the South Pole Telescope. The lensing potential is reconstructed with signal-to-noise per mode greater than unity at lensing multipoles L ≲ 250, using a quadratic estimator on a combination of cosmic microwave background temperature and polarization maps. We report measurements of the lensing potential power spectrum in the multipole range of 100 < L < 2000 from sets of temperature-only (T), polarization-only (POL), and minimum-variance (MV) estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit Λ cold dark matter model to the Planck 2015 TT + low P + lensing data set. For the minimum-variance estimator, we find =0.944 0.025 (Sys.) SRC=restricting to only polarization data, we find POL=0.906\pm 0.090 0.040. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1σ) and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.

Published
2019

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

Author

Henning, JW, Sayre, JT, Reichardt, CL, Ade, PAR, Anderson, AJ, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Meyer, SS, Mocanu, L, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Sievers, C, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, and Yefremenko, V

Subjects
Astronomical Sciences, Physical Sciences, cosmic background radiation, cosmological parameters, cosmology: observations, polarization, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

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 50 < ℓ ≤ 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 , 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 mJy, we place a 95% confidence upper limit on residual polarized point-source power of at Dℓ = ℓ(ℓ+1)ℓℓ/2π < 0.107 μK2 at ℓ = 3000, suggesting that the EE damping tail dominates foregrounds to at least ℓ= 4050 with modest source masking. We find that the SPTpol data set is in mild tension with the ΛCDM model (2.1 δ), and different data splits prefer parameter values that differ at the ∼ 1 δ level. When fitting SPTpol data at ℓ < 1000, we find cosmological parameter constraints consistent with those for Planck temperature. Including SPTpol data at ℓ> 1000 results in a preference for a higher value of the expansion rate (H071.3 ± 2.1 Km s-1 Mpc-1) and a lower value for present-day density fluctuations (δ8 =0.77 ±0.02).

Published
2018

10. Optimization of Transition Edge Sensor Arrays for Cosmic Microwave Background Observations with the South Pole Telescope

Author

Ding, J, Ade, PAR, Anderson, AJ, Avva, J, Ahmed, Z, Arnold, K, Austermann, JE, Bender, AN, Benson, BA, Bleem, LE, Byrum, K, Carlstrom, JE, Carter, FW, Chang, CL, Cho, HM, Clich, JF, Cukierman, A, Czaplewski, D, Divan, R, De Haan, T, Dobbs, MA, Dutcher, D, Everett, W, Gilbert, A, Gannon, R, Guyser, R, Halverson, NW, Harrington, NL, Hattori, K, Henning, JW, Hilton, GC, Holzapfel, WL, Hubmayr, J, Huang, N, Irwin, KD, Jeong, O, Khaire, T, Kubik, D, Kuo, CL, Lee, AT, Leitch, EM, Meyer, SS, Miller, CS, Montgomery, J, Nadolski, A, Natoli, T, Nguyen, H, Novosad, V, Padin, S, Pan, Z, Pearson, J, Posada, CM, Rahlin, A, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Shariff, JA, Shirley, I, Shirokoff, E, Smecher, G, Sobrin, J, Stan, L, Stark, AA, Story, K, Suzuki, A, Tang, QY, Thakur, RB, Thompson, KL, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK, Yefremenko, V, and Yoon, KW

Subjects
Transition edge sensors, superconducting detectors, bolometers, cosmic microwave background, South Pole telescope, General Physics, Electrical and Electronic Engineering, Condensed Matter Physics, Materials Engineering
Abstract

In this paper, we describe the optimization of transition-edge-sensor (TES) detector arrays for the third-generation camera for the South Pole Telescope. The camera, which contains ~ 16 000 detectors, will make high-angular-resolution maps of the temperature and polarization of the cosmic microwave background. Our key results are scatter in the transition temperature of Ti/Au TESs is reduced by fabricating the TESs on a thin Ti(5 nm)/Au(5 nm) buffer layer and the thermal conductivity of the legs that support our detector islands is dominated by the SiOx dielectric in the microstrip transmission lines that run along the legs.

Published
2017

11. STELLAR MASSES AND STAR FORMATION RATES OF LENSED, DUSTY, STAR-FORMING GALAXIES FROM THE SPT SURVEY

Author

Ma, Jingzhe, Gonzalez, Anthony H, Spilker, JS, Strandet, M, Ashby, MLN, Aravena, M, Béthermin, M, Bothwell, MS, de Breuck, C, Brodwin, M, Chapman, SC, Fassnacht, CD, Greve, TR, Gullberg, B, Hezaveh, Y, Malkan, M, Marrone, DP, Saliwanchik, BR, Vieira, JD, Weiss, A, and Welikala, N

Subjects
galaxies: high-redshift, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

To understand cosmic mass assembly in the universe at early epochs, we primarily rely on measurements of the stellar masses and star formation rates (SFRs) of distant galaxies. In this paper, we present stellar masses and SFRs of six high-redshift (2.8 ≤ z ≤ 5.7) dusty, star-forming galaxies (DSFGs) that are strongly gravitationally lensed by foreground galaxies. These sources were first discovered by the South Pole Telescope (SPT) at millimeter wavelengths and all have spectroscopic redshifts and robust lens models derived from Atacama Large Millimeter/submillimeter Array observations. We have conducted follow-up observations to obtain multi-wavelength imaging data using the Hubble Space Telescope (HST), Spitzer, Herschel, and the Atacama Pathfinder EXperiment. We use the high-resolution HST/Wide Field Camera 3 images to disentangle the background source from the foreground lens in Spitzer/IRAC data. The detections and upper limits provide important constraints on the spectral energy distributions (SEDs) for these DSFGs, yielding stellar masses, IR luminosities, and SFRs. The SED fits of six SPT sources show that the intrinsic stellar masses span a range more than one order of magnitude with a median value ∼5 ×1010 Mo. The intrinsic IR luminosities range from 4 × 1012 Lo to 4 × 1013 Lo. They all have prodigious intrinsic SFRs of 510-4800 Mo yr-1. Compared to the star-forming main sequence (MS), these six DSFGs have specific SFRs that all lie above the MS, including two galaxies that are a factor of 10 higher than the MS. Our results suggest that we are witnessing ongoing strong starburst events that may be driven by major mergers.

Published
2015

12. A demonstration of improved constraints on primordial gravitational waves with delensing

Author

Ade, PAR, Ahmed, Z, Amiri, M, Anderson, AJ, Austermann, JE, Avva, JS, Barkats, D, Thakur, RB, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bischoff, CA, Bleem, LE, Bock, JJ, Boenish, H, Bullock, E, Buza, V, Carlstrom, JE, Chang, CL, Cheshire, JR, Chiang, HC, Chou, T-L, Citron, R, Connors, J, Moran, CC, Cornelison, J, Crawford, TM, Crites, AT, Crumrine, M, Cukierman, A, de Haan, T, Dierickx, M, Dobbs, MA, Duband, L, Everett, W, Fatigoni, S, Filippini, JP, Fliescher, S, Gallicchio, J, George, EM, St Germaine, T, Goeckner-Wald, N, Goldfinger, DC, Grayson, J, Gupta, N, Hall, G, Halpern, M, Halverson, NW, Harrison, S, Henderson, S, Henning, JW, Hildebrandt, SR, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Hui, H, Irwin, KD, Kang, J, Karkare, KS, Karpel, E, Kefeli, S, Kernasovskiy, SA, Knox, L, Kovac, JM, Kuo, CL, Lau, K, Lee, AT, Leitch, EM, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Megerian, KG, Meyer, SS, Millea, M, Mocanu, LM, Moncelsi, L, Montgomery, J, Nadolski, A, Namikawa, T, Natoli, T, Netterfield, CB, Nguyen, HT, Nibarger, JP, Noble, G, Novosad, V, O'Brient, R, Ogburn, RW, Omori, Y, Padin, S, Palladino, S, Patil, S, Prouve, T, Pryke, C, Racine, B, Reichardt, CL, Reintsema, CD, Richter, S, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Schillaci, A, Schmitt, BL, Schwarz, R, Sheehy, CD, Sievers, C, Smecher, G, Soliman, A, Stark, AA, Steinbach, B, Sudiwala, R, Teply, GP, Thompson, KL, Tolan, JE, Tucker, C, Turner, AD, Umilta, C, Veach, T, Vieira, JD, Vieregg, AG, Wandui, A, Wang, G, Weber, AC, Whitehorn, N, Wiebe, D, Willmert, J, Wong, CL, Wu, WLK, Yang, H, Yefremenko, V, Yoon, KW, Young, E, Yu, C, Zeng, L, Zhang, C, Ade, PAR, Ahmed, Z, Amiri, M, Anderson, AJ, Austermann, JE, Avva, JS, Barkats, D, Thakur, RB, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bischoff, CA, Bleem, LE, Bock, JJ, Boenish, H, Bullock, E, Buza, V, Carlstrom, JE, Chang, CL, Cheshire, JR, Chiang, HC, Chou, T-L, Citron, R, Connors, J, Moran, CC, Cornelison, J, Crawford, TM, Crites, AT, Crumrine, M, Cukierman, A, de Haan, T, Dierickx, M, Dobbs, MA, Duband, L, Everett, W, Fatigoni, S, Filippini, JP, Fliescher, S, Gallicchio, J, George, EM, St Germaine, T, Goeckner-Wald, N, Goldfinger, DC, Grayson, J, Gupta, N, Hall, G, Halpern, M, Halverson, NW, Harrison, S, Henderson, S, Henning, JW, Hildebrandt, SR, Hilton, GC, Holder, GP, Holzapfel, WL, Hrubes, JD, Huang, N, Hubmayr, J, Hui, H, Irwin, KD, Kang, J, Karkare, KS, Karpel, E, Kefeli, S, Kernasovskiy, SA, Knox, L, Kovac, JM, Kuo, CL, Lau, K, Lee, AT, Leitch, EM, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Megerian, KG, Meyer, SS, Millea, M, Mocanu, LM, Moncelsi, L, Montgomery, J, Nadolski, A, Namikawa, T, Natoli, T, Netterfield, CB, Nguyen, HT, Nibarger, JP, Noble, G, Novosad, V, O'Brient, R, Ogburn, RW, Omori, Y, Padin, S, Palladino, S, Patil, S, Prouve, T, Pryke, C, Racine, B, Reichardt, CL, Reintsema, CD, Richter, S, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Schillaci, A, Schmitt, BL, Schwarz, R, Sheehy, CD, Sievers, C, Smecher, G, Soliman, A, Stark, AA, Steinbach, B, Sudiwala, R, Teply, GP, Thompson, KL, Tolan, JE, Tucker, C, Turner, AD, Umilta, C, Veach, T, Vieira, JD, Vieregg, AG, Wandui, A, Wang, G, Weber, AC, Whitehorn, N, Wiebe, D, Willmert, J, Wong, CL, Wu, WLK, Yang, H, Yefremenko, V, Yoon, KW, Young, E, Yu, C, Zeng, L, and Zhang, C

Published
2021

13. CMB Polarization B-mode Delensing with SPTpol and Herschel

Author

Manzotti, A, Story, KT, Wu, WLK, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Bock, JJ, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Conley, A, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dodelson, S, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, McMahon, JJ, Meyer, SS, Mocanu, LM, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Vanderlinde, K, Vieira, JD, Viero, MP, Wang, G, Whitehorn, N, Yefremenko, V, Zemcov, M, Manzotti, A, Story, KT, Wu, WLK, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Bock, JJ, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Conley, A, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Dodelson, S, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, McMahon, JJ, Meyer, SS, Mocanu, LM, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Vanderlinde, K, Vieira, JD, Viero, MP, Wang, G, Whitehorn, N, Yefremenko, V, and Zemcov, M

Published
2017

14. COSMOLOGICAL CONSTRAINTS FROM GALAXY CLUSTERS IN THE 2500 SQUARE-DEGREE SPT-SZ SURVEY

Author

de Haan, T, Benson, BA, Bleem, LE, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Bayliss, M, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, Dobbs, MA, Doucouliagos, AN, Foley, RJ, Forman, WR, Garmire, GP, George, EM, Gladders, MD, Gonzalez, AH, Gupta, N, Halverson, NW, Hlavacek-Larrondo, J, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, von der Linden, A, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Rapetti, D, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zenteno, A, de Haan, T, Benson, BA, Bleem, LE, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Bayliss, M, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, Dobbs, MA, Doucouliagos, AN, Foley, RJ, Forman, WR, Garmire, GP, George, EM, Gladders, MD, Gonzalez, AH, Gupta, N, Halverson, NW, Hlavacek-Larrondo, J, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, von der Linden, A, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Rapetti, D, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, and Zenteno, A

Published
2016

15. STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 < z < 1.25: A TRANSITIONING FUEL SUPPLY

Author

McDonald, M, Stalder, B, Bayliss, M, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chiu, I, Desai, S, Gonzalez, AH, Hlavacek-Larrondo, J, Holzapfel, WL, Marrone, DP, Miller, ED, Reichardt, CL, Saliwanchik, BR, Saro, A, Schrabback, T, Stanford, SA, Stark, AA, Vieira, JD, Zenteno, A, McDonald, M, Stalder, B, Bayliss, M, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Brodwin, M, Carlstrom, JE, Chiu, I, Desai, S, Gonzalez, AH, Hlavacek-Larrondo, J, Holzapfel, WL, Marrone, DP, Miller, ED, Reichardt, CL, Saliwanchik, BR, Saro, A, Schrabback, T, Stanford, SA, Stark, AA, Vieira, JD, and Zenteno, A

Published
2016

16. CMB lensing tomography with the DES Science Verification galaxies

Author

Giannantonio, T, Fosalba, P, Cawthon, R, Omori, Y, Crocce, M, Elsner, F, Leistedt, B, Dodelson, S, Benoit-Levy, A, Gaztanaga, E, Holder, G, Peiris, HV, Percival, WJ, Kirk, D, Bauer, AH, Benson, BA, Bernstein, GM, Carretero, J, Crawford, TM, Crittenden, R, Huterer, D, Jain, B, Krause, E, Reichardt, CL, Ross, AJ, Simard, G, Soergel, B, Stark, A, Story, KT, Vieira, JD, Weller, J, Abbott, T, Abdalla, FB, Allam, S, Armstrong, R, Banerji, M, Bernstein, RA, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Capozzi, D, Carlstrom, JE, Rosell, AC, Kind, MC, Castander, FJ, Chang, CL, Cunha, CE, da Costa, LN, D'Andrea, CB, DePoy, DL, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Eifler, TF, Evrard, AE, Fausti Neto, A, Fernandez, E, Finley, DA, Flaugher, B, Frieman, J, Gerdes, D, Gruen, D, Gruendl, RA, Gutierrez, G, Holzapfel, WL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, March, M, Marshall, JL, Martini, P, Melchior, P, Miquel, R, Mohr, JJ, Nichol, RC, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Roodman, A, Rykoff, ES, Sako, M, Saliwanchik, BR, Sanchez, E, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Thomas, D, Vikram, V, Walker, AR, Wechsler, RH, Zuntz, J, Giannantonio, T, Fosalba, P, Cawthon, R, Omori, Y, Crocce, M, Elsner, F, Leistedt, B, Dodelson, S, Benoit-Levy, A, Gaztanaga, E, Holder, G, Peiris, HV, Percival, WJ, Kirk, D, Bauer, AH, Benson, BA, Bernstein, GM, Carretero, J, Crawford, TM, Crittenden, R, Huterer, D, Jain, B, Krause, E, Reichardt, CL, Ross, AJ, Simard, G, Soergel, B, Stark, A, Story, KT, Vieira, JD, Weller, J, Abbott, T, Abdalla, FB, Allam, S, Armstrong, R, Banerji, M, Bernstein, RA, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Capozzi, D, Carlstrom, JE, Rosell, AC, Kind, MC, Castander, FJ, Chang, CL, Cunha, CE, da Costa, LN, D'Andrea, CB, DePoy, DL, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Eifler, TF, Evrard, AE, Fausti Neto, A, Fernandez, E, Finley, DA, Flaugher, B, Frieman, J, Gerdes, D, Gruen, D, Gruendl, RA, Gutierrez, G, Holzapfel, WL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, March, M, Marshall, JL, Martini, P, Melchior, P, Miquel, R, Mohr, JJ, Nichol, RC, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Roodman, A, Rykoff, ES, Sako, M, Saliwanchik, BR, Sanchez, E, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Thomas, D, Vikram, V, Walker, AR, Wechsler, RH, and Zuntz, J

Published
2016

17. Detection of the kinematic Sunyaev-Zel'dovich effect with DES Year 1 and SPT

Author

Soergel, B, Flender, S, Story, KT, Bleem, L, Giannantonio, T, Efstathiou, G, Rykoff, E, Benson, BA, Crawford, T, Dodelson, S, Habib, S, Heitmann, K, Holder, G, Jain, B, Rozo, E, Saro, A, Weller, J, Abdalla, FB, Allam, S, Annis, J, Armstrong, R, Benoit-Levy, A, Bernstein, GM, Carlstrom, JE, Carnero Rosell, A, Kind, MC, Castander, FJ, Chiu, I, Chown, R, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, de Haan, T, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Estrada, J, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gruen, D, Gruendl, RA, Holzapfel, WL, Honscheid, K, James, DJ, Keisler, R, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Marshall, JL, McDonald, M, Melchior, P, Miller, CJ, Miquel, R, Nord, B, Ogando, R, Omori, Y, Plazas, AA, Rapetti, D, Reichardt, CL, Romer, AK, Roodman, A, Saliwanchik, BR, Sanchez, E, Schubnell, M, Sevilla-Noarbe, I, Sheldon, E, Smith, RC, Soares-Santos, M, Sobreira, F, Stark, A, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Vieira, JD, Walker, AR, Whitehorn, N, Soergel, B, Flender, S, Story, KT, Bleem, L, Giannantonio, T, Efstathiou, G, Rykoff, E, Benson, BA, Crawford, T, Dodelson, S, Habib, S, Heitmann, K, Holder, G, Jain, B, Rozo, E, Saro, A, Weller, J, Abdalla, FB, Allam, S, Annis, J, Armstrong, R, Benoit-Levy, A, Bernstein, GM, Carlstrom, JE, Carnero Rosell, A, Kind, MC, Castander, FJ, Chiu, I, Chown, R, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, de Haan, T, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Estrada, J, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gruen, D, Gruendl, RA, Holzapfel, WL, Honscheid, K, James, DJ, Keisler, R, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Marshall, JL, McDonald, M, Melchior, P, Miller, CJ, Miquel, R, Nord, B, Ogando, R, Omori, Y, Plazas, AA, Rapetti, D, Reichardt, CL, Romer, AK, Roodman, A, Saliwanchik, BR, Sanchez, E, Schubnell, M, Sevilla-Noarbe, I, Sheldon, E, Smith, RC, Soares-Santos, M, Sobreira, F, Stark, A, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Vieira, JD, Walker, AR, and Whitehorn, N

Published
2016

18. MILLIMETER TRANSIENT POINT SOURCES IN THE SPTpol 100 SQUARE DEGREE SURVEY

Author

Whitehorn, N, Natoli, T, Ade, PAR, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, McMahon, JJ, Meyer, SS, Mocanu, L, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Yefremenko, V, Whitehorn, N, Natoli, T, Ade, PAR, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, McMahon, JJ, Meyer, SS, Mocanu, L, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, and Yefremenko, V

Abstract

The millimeter transient sky is largely unexplored, with measurements limited to follow-up of objects detected at other wavelengths. High-angular-resolution telescopes, designed for measurement of the cosmic microwave background (CMB), offer the possibility to discover new, unknown transient sources in this band—particularly the afterglows of unobserved gamma-ray bursts (GRBs). Here, we use the 10 m millimeter-wave South Pole Telescope, designed for the primary purpose of observing the CMB at arcminute and larger angular scales, to conduct a search for such objects. During the 2012–2013 season, the telescope was used to continuously observe a 100 deg2 patch of sky centered at R.A. 23h30m and decl. −55° using the polarization-sensitive SPTpol camera in two bands centered at 95 and 150 GHz. These 6000 hr of observations provided continuous monitoring for day- to month-scale millimeter-wave transient sources at the 10 mJy level. One candidate object was observed with properties broadly consistent with a GRB afterglow, but at a statistical significance too low (p = 0.01) to confirm detection.

Published
2016

19. SPT-GMOS: A GEMINI/GMOS-SOUTH SPECTROSCOPIC SURVEY OF GALAXY CLUSTERS IN THE SPT-SZ SURVEY

Author

Bayliss, MB, Ruel, J, Stubbs, CW, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Capasso, R, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Doucouliagos, AN, Foley, RJ, Forman, WR, Garmire, GP, George, EM, Gladders, MD, Gonzalez, AH, Gupta, N, Halverson, NW, Hlavacek-Larrondo, J, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, von der Linden, A, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Rapetti, D, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zenteno, A, Bayliss, MB, Ruel, J, Stubbs, CW, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Capasso, R, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Doucouliagos, AN, Foley, RJ, Forman, WR, Garmire, GP, George, EM, Gladders, MD, Gonzalez, AH, Gupta, N, Halverson, NW, Hlavacek-Larrondo, J, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, von der Linden, A, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Rapetti, D, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, and Zenteno, A

Published
2016

20. Stellar masses and star formation rates of lensed, dusty, star-forming galaxies from the SPT survey

Author

Ma, J, Ma, J, Gonzalez, AH, Spilker, JS, Strandet, M, Ashby, MLN, Aravena, M, Béthermin, M, Bothwell, MS, Breuck, CD, Brodwin, M, Chapman, SC, Fassnacht, CD, Greve, TR, Gullberg, B, Hezaveh, Y, Malkan, M, Marrone, DP, Saliwanchik, BR, Vieira, JD, Weiss, A, Welikala, N, Ma, J, Ma, J, Gonzalez, AH, Spilker, JS, Strandet, M, Ashby, MLN, Aravena, M, Béthermin, M, Bothwell, MS, Breuck, CD, Brodwin, M, Chapman, SC, Fassnacht, CD, Greve, TR, Gullberg, B, Hezaveh, Y, Malkan, M, Marrone, DP, Saliwanchik, BR, Vieira, JD, Weiss, A, and Welikala, N

Abstract

To understand cosmic mass assembly in the universe at early epochs, we primarily rely on measurements of the stellar masses and star formation rates (SFRs) of distant galaxies. In this paper, we present stellar masses and SFRs of six high-redshift (2.8 ≤ z ≤ 5.7) dusty, star-forming galaxies (DSFGs) that are strongly gravitationally lensed by foreground galaxies. These sources were first discovered by the South Pole Telescope (SPT) at millimeter wavelengths and all have spectroscopic redshifts and robust lens models derived from Atacama Large Millimeter/submillimeter Array observations. We have conducted follow-up observations to obtain multi-wavelength imaging data using the Hubble Space Telescope (HST), Spitzer, Herschel, and the Atacama Pathfinder EXperiment. We use the high-resolution HST/Wide Field Camera 3 images to disentangle the background source from the foreground lens in Spitzer/IRAC data. The detections and upper limits provide important constraints on the spectral energy distributions (SEDs) for these DSFGs, yielding stellar masses, IR luminosities, and SFRs. The SED fits of six SPT sources show that the intrinsic stellar masses span a range more than one order of magnitude with a median value ∼5 ×1010 Mo. The intrinsic IR luminosities range from 4 × 1012 Lo to 4 × 1013 Lo. They all have prodigious intrinsic SFRs of 510-4800 Mo yr-1. Compared to the star-forming main sequence (MS), these six DSFGs have specific SFRs that all lie above the MS, including two galaxies that are a factor of 10 higher than the MS. Our results suggest that we are witnessing ongoing strong starburst events that may be driven by major mergers.

Published
2015

21. A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND GRAVITATIONAL LENSING POTENTIAL FROM 100 SQUARE DEGREES OF SPTPOL DATA

Author

Story, KT, Hanson, D, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Liang, C, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenk, V, Zahn, O, Story, KT, Hanson, D, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Liang, C, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenk, V, and Zahn, O

Abstract

We present a measurement of the cosmic microwave background (CMB) gravitational lensing potential using data from the first two seasons of observations with SPTpol, the polarization-sensitive receiver currently installed on the South Pole Telescope (SPT). The observations used in this work cover 100 deg$^2$ of sky with arcminute resolution at 150 GHz. Using a quadratic estimator, we make maps of the CMB lensing potential from combinations of CMB temperature and polarization maps. We combine these lensing potential maps to form a minimum-variance (MV) map. The lensing potential is measured with a signal-to-noise ratio of greater than one for angular multipoles between $100< L <250$. This is the highest signal-to-noise mass map made from the CMB to date and will be powerful in cross-correlation with other tracers of large-scale structure. We calculate the power spectrum of the lensing potential for each estimator, and we report the value of the MV power spectrum between $100< L <2000$ as our primary result. We constrain the ratio of the spectrum to a fiducial $\Lambda$CDM model to be $A_{\rm MV}=0.92 \pm 0.14 {\rm\, (Stat.)} \pm 0.08 {\rm\, (Sys.)}$. Restricting ourselves to polarized data only, we find $A_{\rm POL}=0.92 \pm 0.24 {\rm\, (Stat.)} \pm 0.11 {\rm\, (Sys.)}$. This measurement rejects the hypothesis of no lensing at $5.9 \sigma$ using polarization data alone, and at $14 \sigma$ using both temperature and polarization data.

Published
2015

22. A MEASUREMENT OF GRAVITATIONAL LENSING OF THE COSMIC MICROWAVE BACKGROUND BY GALAXY CLUSTERS USING DATA FROM THE SOUTH POLE TELESCOPE

Author

Baxter, EJ, Keisler, R, Dodelson, S, Aird, KA, Allen, SW, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, de Haan, T, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, Hennig, C, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Jones, C, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Baxter, EJ, Keisler, R, Dodelson, S, Aird, KA, Allen, SW, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, H-M, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, de Haan, T, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, Hennig, C, Hoekstra, H, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Jones, C, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Millea, M, Mocanu, LM, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

Clusters of galaxies are expected to gravitationally lens the cosmic microwave background (CMB) and thereby generate a distinct signal in the CMB on arcminute scales. Measurements of this effect can be used to constrain the masses of galaxy clusters with CMB data alone. Here we present a measurement of lensing of the CMB by galaxy clusters using data from the South Pole Telescope (SPT). We develop a maximum likelihood approach to extract the CMB cluster lensing signal and validate the method on mock data. We quantify the effects on our analysis of several potential sources of systematic error and find that they generally act to reduce the best-fit cluster mass. It is estimated that this bias to lower cluster mass is roughly $0.85\sigma$ in units of the statistical error bar, although this estimate should be viewed as an upper limit. We apply our maximum likelihood technique to 513 clusters selected via their SZ signatures in SPT data, and rule out the null hypothesis of no lensing at $3.1\sigma$. The lensing-derived mass estimate for the full cluster sample is consistent with that inferred from the SZ flux: $M_{200,\mathrm{lens}} = 0.83_{-0.37}^{+0.38}\, M_{200,\mathrm{SZ}}$ (68% C.L., statistical error only).

Published
2015

23. Analysis of Sunyaev-Zel'dovich effect mass-observable relations using South Pole Telescope observations of an X-ray selected sample of low-mass galaxy clusters and groups

Author

Liu, J, Mohr, J, Saro, A, Aird, KA, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Foley, RJ, Gangkofner, D, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, L, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Story, K, Suhada, R, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Liu, J, Mohr, J, Saro, A, Aird, KA, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Foley, RJ, Gangkofner, D, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, L, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Story, K, Suhada, R, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

(Abridged) We use 95, 150, and 220GHz observations from the SPT to examine the SZE signatures of a sample of 46 X-ray selected groups and clusters drawn from ~6 deg^2 of the XMM-BCS. These systems extend to redshift z=1.02, have characteristic masses ~3x lower than clusters detected directly in the SPT data and probe the SZE signal to the lowest X-ray luminosities (>10^42 erg s^-1) yet. We develop an analysis tool that combines the SZE information for the full ensemble of X-ray-selected clusters. Using X-ray luminosity as a mass proxy, we extract selection-bias corrected constraints on the SZE significance- and Y_500-mass relations. The SZE significance- mass relation is in good agreement with an extrapolation of the relation obtained from high mass clusters. However, the fit to the Y_500-mass relation at low masses, while in good agreement with the extrapolation from high mass SPT clusters, is in tension at 2.8 sigma with the constraints from the Planck sample. We examine the tension with the Planck relation, discussing sample differences and biases that could contribute. We also present an analysis of the radio galaxy point source population in this ensemble of X-ray selected systems. We find 18 of our systems have 843 MHz SUMSS sources within 2 arcmin of the X-ray centre, and three of these are also detected at significance >4 by SPT. Of these three, two are associated with the group brightest cluster galaxies, and the third is likely an unassociated quasar candidate. We examine the impact of these point sources on our SZE scaling relation analyses and find no evidence of biases. We also examine the impact of dusty galaxies using constraints from the 220 GHz data. The stacked sample provides 2.8$\sigma$ significant evidence of dusty galaxy flux, which would correspond to an average underestimate of the SPT Y_500 signal that is (17+-9) per cent in this sample of low mass systems.

Published
2015

24. MEASUREMENT OF GALAXY CLUSTER INTEGRATED COMPTONIZATION AND MASS SCALING RELATIONS WITH THE SOUTH POLE TELESCOPE

Author

Saliwanchik, BR, Montroy, TE, Aird, KA, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Nurgaliev, D, Padin, S, Patej, A, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Saliwanchik, BR, Montroy, TE, Aird, KA, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Nurgaliev, D, Padin, S, Patej, A, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

We describe a method for measuring the integrated Comptonization (YSZ) of clusters of galaxies from measurements of the Sunyaev-Zel'dovich (SZ) effect in multiple frequency bands and use this method to characterize a sample of galaxy clusters detected in South Pole Telescope (SPT) data. We test this method on simulated cluster observations and verify that it can accurately recover cluster parameters with negligible bias. In realistic simulations of an SPT-like survey, with realizations of cosmic microwave background anisotropy, point sources, and atmosphere and instrumental noise at typical SPT-SZ survey levels, we find that YSZ is most accurately determined in an aperture comparable to the SPT beam size. We demonstrate the utility of this method to measure YSZ and to constrain mass scaling relations using X-ray mass estimates for a sample of 18 galaxy clusters from the SPT-SZ survey. Measuring YSZ within a 0.75' radius aperture, we find an intrinsic log-normal scatter of 21+/-11% in YSZ at a fixed mass. Measuring YSZ within a 0.3 Mpc projected radius (equivalent to 0.75' at the survey median redshift z = 0.6), we find a scatter of 26+/-9%. Prior to this study, the SPT observable found to have the lowest scatter with mass was cluster detection significance. We demonstrate, from both simulations and SPT observed clusters, that YSZ measured within an aperture comparable to the SPT beam size is equivalent, in terms of scatter with cluster mass, to SPT cluster detection significance.

Published
2015

25. MEASUREMENTS OF SUB-DEGREE B-MODE POLARIZATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA

Author

Keisler, R, Hoover, S, Harrington, N, Henning, JW, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Hanson, D, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Leitch, EM, Li, D, Luong-Van, D, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, Zahn, O, Keisler, R, Hoover, S, Harrington, N, Henning, JW, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Hanson, D, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Leitch, EM, Li, D, Luong-Van, D, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, and Zahn, O

Abstract

We present a measurement of the $B$-mode polarization power spectrum (the $BB$ spectrum) from 100 $\mathrm{deg}^2$ of sky observed with SPTpol, a polarization-sensitive receiver currently installed on the South Pole Telescope. The observations used in this work were taken during 2012 and early 2013 and include data in spectral bands centered at 95 and 150 GHz. We report the $BB$ spectrum in five bins in multipole space, spanning the range $300 \le \ell \le 2300$, and for three spectral combinations: 95 GHz $\times$ 95 GHz, 95 GHz $\times$ 150 GHz, and 150 GHz $\times$ 150 GHz. We subtract small ($< 0.5 \sigma$ in units of statistical uncertainty) biases from these spectra and account for the uncertainty in those biases. The resulting power spectra are inconsistent with zero power but consistent with predictions for the $BB$ spectrum arising from the gravitational lensing of $E$-mode polarization. If we assume no other source of $BB$ power besides lensed $B$ modes, we determine a preference for lensed $B$ modes of $4.9 \sigma$. After marginalizing over tensor power and foregrounds, namely polarized emission from galactic dust and extragalactic sources, this significance is $4.3 \sigma$. Fitting for a single parameter, $A_\mathrm{lens}$, that multiplies the predicted lensed $B$-mode spectrum, and marginalizing over tensor power and foregrounds, we find $A_\mathrm{lens} = 1.08 \pm 0.26$, indicating that our measured spectra are consistent with the signal expected from gravitational lensing. The data presented here provide the best measurement to date of the $B$-mode power spectrum on these angular scales.

Published
2015

26. GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV-ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY

Author

Bleem, LE, Stalder, B, de Haan, T, Aird, KA, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hoekstra, H, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Bleem, LE, Stalder, B, de Haan, T, Aird, KA, Allen, SW, Applegate, DE, Ashby, MLN, Bautz, M, Bayliss, M, Benson, BA, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dietrich, JP, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hoekstra, H, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Schrabback, T, Shirokoff, E, Song, J, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

We present a catalog of galaxy clusters selected via their Sunyaev-Zel'dovich (SZ) effect signature from 2500 deg$^2$ of South Pole Telescope (SPT) data. This work represents the complete sample of clusters detected at high significance in the 2500-square-degree SPT-SZ survey, which was completed in 2011. A total of 677 (409) cluster candidates are identified above a signal-to-noise threshold of $\xi$ =4.5 (5.0). Ground- and space-based optical and near-infrared (NIR) imaging confirms overdensities of similarly colored galaxies in the direction of 516 (or 76%) of the $\xi$>4.5 candidates and 387 (or 95%) of the $\xi$>5 candidates; the measured purity is consistent with expectations from simulations. Of these confirmed clusters, 415 were first identified in SPT data, including 251 new discoveries reported in this work. We estimate photometric redshifts for all candidates with identified optical and/or NIR counterparts; we additionally report redshifts derived from spectroscopic observations for 141 of these systems. The mass threshold of the catalog is roughly independent of redshift above $z$~0.25 leading to a sample of massive clusters that extends to high redshift. The median mass of the sample is $M_{\scriptsize 500c}(\rho_\mathrm{crit})$ ~ 3.5 x 10$^{14} M_\odot h^{-1}$, the median redshift is $z_{med}$ =0.55, and the highest-redshift systems are at $z$>1.4. The combination of large redshift extent, clean selection, and high typical mass makes this cluster sample of particular interest for cosmological analyses and studies of cluster formation and evolution.

Published
2015

27. MEASUREMENTS OF E-MODE POLARIZATION AND TEMPERATURE-E-MODE CORRELATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA

Author

Crites, AT, Henning, JW, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, De Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Hanson, D, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Liang, C, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, Zahn, O, Crites, AT, Henning, JW, Ade, PAR, Aird, KA, Austermann, JE, Beall, JA, Bender, AN, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crawford, TM, De Haan, T, Dobbs, MA, Everett, W, Gallicchio, J, Gao, J, George, EM, Gilbert, A, Halverson, NW, Hanson, D, Harrington, N, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Li, D, Liang, C, Luong-Van, D, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Whitehorn, N, Yefremenko, V, and Zahn, O

Abstract

We present measurements of $E$-mode polarization and temperature-$E$-mode correlation in the cosmic microwave background (CMB) using data from the first season of observations with SPTpol, the polarization-sensitive receiver currently installed on the South Pole Telescope (SPT). The observations used in this work cover 100~\sqdeg\ of sky with arcminute resolution at $150\,$GHz. We report the $E$-mode angular auto-power spectrum ($EE$) and the temperature-$E$-mode angular cross-power spectrum ($TE$) over the multipole range $500 < \ell \leq5000$. These power spectra improve on previous measurements in the high-$\ell$ (small-scale) regime. We fit the combination of the SPTpol power spectra, data from \planck\, and previous SPT measurements with a six-parameter \LCDM cosmological model. We find that the best-fit parameters are consistent with previous results. The improvement in high-$\ell$ sensitivity over previous measurements leads to a significant improvement in the limit on polarized point-source power: after masking sources brighter than 50\,mJy in unpolarized flux at 150\,GHz, we find a 95\% confidence upper limit on unclustered point-source power in the $EE$ spectrum of $D_\ell = \ell (\ell+1) C_\ell / 2 \pi < 0.40 \ \mu{\mbox{K}}^2$ at $\ell=3000$, indicating that future $EE$ measurements will not be limited by power from unclustered point sources in the multipole range $\ell < 3600$, and possibly much higher in $\ell.$

Published
2015

28. X-ray cavities in a sample of 83 SPT-selected clusters of galaxies: Tracing the evolution of AGN feedback in clusters of galaxies out to z=1.2

Author

Hlavacek-Larrondo, J, McDonald, M, Benson, BA, Forman, WR, Allen, SW, Bleem, LE, Ashby, MLN, Bocquet, S, Brodwin, M, Dietrich, JP, Jones, C, Liu, J, Saliwanchik, BR, Saro, A, Schrabback, T, Song, J, Stalder, B, Vikhlinin, A, Zenteno, A, Hlavacek-Larrondo, J, McDonald, M, Benson, BA, Forman, WR, Allen, SW, Bleem, LE, Ashby, MLN, Bocquet, S, Brodwin, M, Dietrich, JP, Jones, C, Liu, J, Saliwanchik, BR, Saro, A, Schrabback, T, Song, J, Stalder, B, Vikhlinin, A, and Zenteno, A

Abstract

X-ray cavities are key tracers of mechanical (or radio mode) heating arising from the active galactic nuclei (AGN) in brightest cluster galaxies. We report on a survey for X-ray cavities in 83 massive, high-redshift (0.40.5) redshift. Despite these limitations, our results suggest that the power generated by AGN feedback in brightest cluster galaxies has remained unchanged for over half of the age of the Universe (>7 Gyrs at z=0.8). On average, the detected X-ray cavities have powers of 0.8-5*10^45 erg/s, enthalpies of 3-6*10^59 erg, and radii of 17 kpc. Integrating over 7 Gyrs, we find that the supermassive black holes in the brightest cluster galaxies may have accreted 10^8 to several 10^9M_sun of material to power these outflows. This level of accretion indicates that significant supermassive black hole growth may occur not only at early times, in the quasar era, but at late times as well. We also find that X-ray cavities at high-redshift may inject an excess heat of 0.1-1.0 keV per particle into the hot intracluster medium above and beyond the energy needed to offset cooling. This value is similar to the energy needed to preheat clusters, break self-similarity, and explain the excess entropy in hot atmospheres.

Published
2015

29. SPT-3G: A Next-Generation Cosmic Microwave Background Polarization Experiment on the South Pole Telescope

Author

Holland, WS, Zmuidzinas, J, Benson, BA, Ade, PAR, Ahmed, Z, Allen, SW, Arnold, K, Austermann, JE, Bender, AN, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Cliche, JF, Crawford, TM, Cukierman, A, de Haan, T, Dobbs, MA, Dutcher, D, Everett, W, Gilbert, A, Halverson, NW, Hanson, D, Harrington, NL, Hattori, K, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Irwin, KD, Keisler, R, Knox, L, Kubik, D, Kuo, CL, Lee, AT, Leitch, EM, Li, D, McDonald, M, Meyer, SS, Montgomery, J, Myers, M, Natoli, T, Nguyen, H, Novosad, V, Padin, S, Pan, Z, Pearson, J, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Simard, G, Smecher, G, Sayre, JT, Shirokoff, E, Stark, AA, Story, K, Suzuki, A, Thompson, KL, Tucker, C, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Wang, G, Yefremenko, V, Yoon, KW, Holland, WS, Zmuidzinas, J, Benson, BA, Ade, PAR, Ahmed, Z, Allen, SW, Arnold, K, Austermann, JE, Bender, AN, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Cliche, JF, Crawford, TM, Cukierman, A, de Haan, T, Dobbs, MA, Dutcher, D, Everett, W, Gilbert, A, Halverson, NW, Hanson, D, Harrington, NL, Hattori, K, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Irwin, KD, Keisler, R, Knox, L, Kubik, D, Kuo, CL, Lee, AT, Leitch, EM, Li, D, McDonald, M, Meyer, SS, Montgomery, J, Myers, M, Natoli, T, Nguyen, H, Novosad, V, Padin, S, Pan, Z, Pearson, J, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Simard, G, Smecher, G, Sayre, JT, Shirokoff, E, Stark, AA, Story, K, Suzuki, A, Thompson, KL, Tucker, C, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Wang, G, Yefremenko, V, and Yoon, KW

Published
2014

30. Optical Spectroscopy and Velocity Dispersions of Galaxy Clusters from the SPT-SZ Survey

Author

Ruel, J, Bazin, G, Bayliss, M, Brodwin, M, Foley, RJ, Stalder, B, Aird, KA, Armstrong, R, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Bocquet, S, Carlstrom, JE, Chang, CL, Chapman, SC, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Nurgaliev, D, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, v Suhada, R, Spieler, HG, Stanford, SA, Staniszewski, Z, Starsk, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Ruel, J, Bazin, G, Bayliss, M, Brodwin, M, Foley, RJ, Stalder, B, Aird, KA, Armstrong, R, Ashby, MLN, Bautz, M, Benson, BA, Bleem, LE, Bocquet, S, Carlstrom, JE, Chang, CL, Chapman, SC, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Nurgaliev, D, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, v Suhada, R, Spieler, HG, Stanford, SA, Staniszewski, Z, Starsk, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

We present optical spectroscopy of galaxies in clusters detected through the Sunyaev-Zel'dovich (SZ) effect with the South Pole Telescope (SPT). We report our own measurements of $61$ spectroscopic cluster redshifts, and $48$ velocity dispersions each calculated with more than $15$ member galaxies. This catalog also includes $19$ dispersions of SPT-observed clusters previously reported in the literature. The majority of the clusters in this paper are SPT-discovered; of these, most have been previously reported in other SPT cluster catalogs, and five are reported here as SPT discoveries for the first time. By performing a resampling analysis of galaxy velocities, we find that unbiased velocity dispersions can be obtained from a relatively small number of member galaxies ($\lesssim 30$), but with increased systematic scatter. We use this analysis to determine statistical confidence intervals that include the effect of membership selection. We fit scaling relations between the observed cluster velocity dispersions and mass estimates from SZ and X-ray observables. In both cases, the results are consistent with the scaling relation between velocity dispersion and mass expected from dark-matter simulations. We measure a $\sim$30% log-normal scatter in dispersion at fixed mass, and a $\sim$10% offset in the normalization of the dispersion-mass relation when compared to the expectation from simulations, which is within the expected level of systematic uncertainty.

Published
2014

31. THE REDSHIFT EVOLUTION OF THE MEAN TEMPERATURE, PRESSURE, AND ENTROPY PROFILES IN 80 SPT-SELECTED GALAXY CLUSTERS

Author

McDonald, M, Benson, BA, Vikhlinin, A, Aird, KA, Allen, SW, Bautz, M, Bayliss, M, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McMahon, JJ, Meyer, SS, Miller, ED, Mocanu, L, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, Zenteno, A, McDonald, M, Benson, BA, Vikhlinin, A, Aird, KA, Allen, SW, Bautz, M, Bayliss, M, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hlavacek-Larrondo, J, Holder, GP, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McMahon, JJ, Meyer, SS, Miller, ED, Mocanu, L, Mohr, JJ, Murray, SS, Padin, S, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Stanford, SA, Staniszewski, Z, Stark, AA, Story, KT, Stubbs, CW, Vanderlinde, K, Vieira, JD, Williamson, R, Zahn, O, and Zenteno, A

Published
2014

32. Constraints on the CMB temperature evolution using multiband measurements of the Sunyaev-Zel'dovich effect with the South Pole Telescope

Author

Saro, A, Liu, J, Mohr, JJ, Aird, KA, Ashby, MLN, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Dolag, K, Dudley, JP, Foley, RJ, Gangkofner, D, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hlavacek-Larrondo, J, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Murray, SS, Nurgaliev, D, Padin, S, Patej, A, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Story, K, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Saro, A, Liu, J, Mohr, JJ, Aird, KA, Ashby, MLN, Bayliss, M, Benson, BA, Bleem, LE, Bocquet, S, Brodwin, M, Carlstrom, JE, Chang, CL, Chiu, I, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Dolag, K, Dudley, JP, Foley, RJ, Gangkofner, D, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Hennig, C, Hlavacek-Larrondo, J, Holzapfel, WL, Hrubes, JD, Jones, C, Keisler, R, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Montroy, TE, Murray, SS, Nurgaliev, D, Padin, S, Patej, A, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Story, K, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

The adiabatic evolution of the temperature of the cosmic microwave background (CMB) is a key prediction of standard cosmology. We study deviations from the expected adiabatic evolution of the CMB temperature of the form $T(z) =T_0(1+z)^{1-\alpha}$ using measurements of the spectrum of the Sunyaev Zel'dovich Effect with the South Pole Telescope (SPT). We present a method for using the ratio of the Sunyaev Zel'dovich signal measured at 95 and 150 GHz in the SPT data to constrain the temperature of the CMB. We demonstrate that this approach provides unbiased results using mock observations of clusters from a new set of hydrodynamical simulations. We apply this method to a sample of 158 SPT-selected clusters, spanning the redshift range $0.05 < z < 1.35$, and measure $\alpha = 0.017^{+0.030}_{-0.028}$, consistent with the standard model prediction of $\alpha=0$. In combination with other published results, we constrain $\alpha = 0.011 \pm 0.016$, an improvement of $\sim 20\%$ over published constraints. This measurement also provides a strong constraint on the effective equation of state in models of decaying dark energy $w_\mathrm{eff} = -0.987^{+0.016}_{-0.017}$.

Published
2014

33. SPT-CL J2040-4451: AN SZ-SELECTED GALAXY CLUSTER AT z=1.478 WITH SIGNIFICANT ONGOING STAR FORMATION

Author

Bayliss, MB, Ashby, MLN, Ruel, J, Brodwin, M, Aird, KA, Bautz, MW, Benson, BA, Bleem, LE, Bocquet, S, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiattii, A, Crawford, TM, Crites, AT, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gettings, D, Gladders, MD, Gonzalez, AH, de Haan, T, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, Mawatari, K, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Miller, ED, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Song, J, Stalder, B, Suhada, R, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, R, Zenteno, A, Bayliss, MB, Ashby, MLN, Ruel, J, Brodwin, M, Aird, KA, Bautz, MW, Benson, BA, Bleem, LE, Bocquet, S, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiattii, A, Crawford, TM, Crites, AT, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gettings, D, Gladders, MD, Gonzalez, AH, de Haan, T, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, Mawatari, K, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Miller, ED, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shirokoff, E, Song, J, Stalder, B, Suhada, R, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, R, and Zenteno, A

Abstract

SPT-CLJ2040-4451 -- spectroscopically confirmed at z = 1.478 -- is the highest redshift galaxy cluster yet discovered via the Sunyaev-Zel'dovich effect. SPT-CLJ2040-4451 was a candidate galaxy cluster identified in the first 720 deg^2 of the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey, and confirmed in follow-up imaging and spectroscopy. From multi-object spectroscopy with Magellan-I/Baade+IMACS we measure spectroscopic redshifts for 15 cluster member galaxies, all of which have strong [O II] 3727 emission. SPT-CLJ2040-4451 has an SZ-measured mass of M_500,SZ = 3.2 +/- 0.8 X 10^14 M_Sun/h_70, corresponding to M_200,SZ = 5.8 +/- 1.4 X 10^14 M_Sun/h_70. The velocity dispersion measured entirely from blue star forming members is sigma_v = 1500 +/- 520 km/s. The prevalence of star forming cluster members (galaxies with > 1.5 M_Sun/yr) implies that this massive, high-redshift cluster is experiencing a phase of active star formation, and supports recent results showing a marked increase in star formation occurring in galaxy clusters at z >1.4. We also compute the probability of finding a cluster as rare as this in the SPT-SZ survey to be >99%, indicating that its discovery is not in tension with the concordance Lambda-CDM cosmological model.

Published
2014

34. SPT-CL J0205-5829: A z=1.32 EVOLVED MASSIVE GALAXY CLUSTER IN THE SOUTH POLE TELESCOPE SUNYAEV-ZEL'DOVICH EFFECT SURVEY

Author

Stalder, B, Ruel, J, Suhada, R, Brodwin, M, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gettings, D, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Nurgaliev, D, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Stalder, B, Ruel, J, Suhada, R, Brodwin, M, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gettings, D, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Nurgaliev, D, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stanford, SA, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

The galaxy cluster SPT-CL J0205-5829 currently has the highest spectroscopically-confirmed redshift, z=1.322, in the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey. XMM-Newton observations measure a core-excluded temperature of Tx=8.7keV producing a mass estimate that is consistent with the Sunyaev-Zel'dovich derived mass. The combined SZ and X-ray mass estimate of M500=(4.9+/-0.8)e14 h_{70}^{-1} Msun makes it the most massive known SZ-selected galaxy cluster at z>1.2 and the second most massive at z>1. Using optical and infrared observations, we find that the brightest galaxies in SPT-CL J0205-5829 are already well evolved by the time the universe was <5 Gyr old, with stellar population ages >3 Gyr, and low rates of star formation (<0.5Msun/yr). We find that, despite the high redshift and mass, the existence of SPT-CL J0205-5829 is not surprising given a flat LambdaCDM cosmology with Gaussian initial perturbations. The a priori chance of finding a cluster of similar rarity (or rarer) in a survey the size of the 2500 deg^2 SPT-SZ survey is 69%.

Published
2013

35. COSMOLOGICAL CONSTRAINTS FROM SUNYAEV-ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY

Author

Benson, BA, de Haan, T, Dudley, JP, Reichardt, CL, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, N, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Padin, S, Plagge, T, Pryke, C, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Suhada, R, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Benson, BA, de Haan, T, Dudley, JP, Reichardt, CL, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Bleem, LE, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, Desai, S, Dobbs, MA, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, N, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Montroy, TE, Murray, SS, Natoli, T, Padin, S, Plagge, T, Pryke, C, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Suhada, R, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

We use measurements from the South Pole Telescope (SPT) Sunyaev Zel'dovich (SZ) cluster survey in combination with X-ray measurements to constrain cosmological parameters. We present a statistical method that fits for the scaling relations of the SZ and X-ray cluster observables with mass while jointly fitting for cosmology. The method is generalizable to multiple cluster observables, and self-consistently accounts for the effects of the cluster selection and uncertainties in cluster mass calibration on the derived cosmological constraints. We apply this method to a data set consisting of an SZ-selected catalog of 18 galaxy clusters at z > 0.3 from the first 178 deg2 of the 2500 deg2 SPT-SZ survey, with 14 clusters having X-ray observations from either Chandra or XMM. Assuming a spatially flat LCDM cosmological model, we find the SPT cluster sample constrain sigma_8 (Omega_m/0.25)^0.30 = 0.785 +- 0.037. In combination with measurements of the CMB power spectrum from the SPT and the seven-year WMAP data, the SPT cluster sample constrain sigma_8 = 0.795 +- 0.016 and Omega_m = 0.255 +- 0.016, a factor of 1.5 improvement on each parameter over the CMB data alone. We consider several extensions beyond the LCDM model by including the following as free parameters: the dark energy equation of state (w), the sum of the neutrino masses (sum mnu), the effective number of relativistic species (Neff), and a primordial non-Gaussianity (fNL). We find that adding the SPT cluster data significantly improves the constraints on w and sum mnu beyond those found when using measurements of the CMB, supernovae, baryon acoustic oscillations, and the Hubble constant. Considering each extension independently, we best constrain w=-0.973 +- 0.063 and the sum of neutrino masses sum mnu < 0.28 eV at 95% confidence, a factor of 1.25 and 1.4 improvement, respectively, over the constraints without clusters. [abbrev.]

Published
2013

36. GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV-ZEL'DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY

Author

Reichardt, CL, Stalder, B, Bleem, LE, Montroy, TE, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Natoli, T, Padin, S, Plagge, T, Pryke, C, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Suhada, R, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, Zenteno, A, Reichardt, CL, Stalder, B, Bleem, LE, Montroy, TE, Aird, KA, Andersson, K, Armstrong, R, Ashby, MLN, Bautz, M, Bayliss, M, Bazin, G, Benson, BA, Brodwin, M, Carlstrom, JE, Chang, CL, Cho, HM, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, Forman, WR, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, Harrington, NL, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Jones, C, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Liu, J, Lueker, M, Luong-Van, D, Mantz, A, Marrone, DP, McDonald, M, McMahon, JJ, Mehl, J, Meyer, SS, Mocanu, L, Mohr, JJ, Murray, SS, Natoli, T, Padin, S, Plagge, T, Pryke, C, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Sayre, JT, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Staniszewski, Z, Stark, AA, Story, K, Stubbs, CW, Suhada, R, van Engelen, A, Vanderlinde, K, Vieira, JD, Vikhlinin, A, Williamson, R, Zahn, O, and Zenteno, A

Abstract

We present a catalog of 224 galaxy cluster candidates, selected through their Sunyaev-Zel'dovich (SZ) effect signature in the first 720 deg2 of the South Pole Telescope (SPT) survey. This area was mapped with the SPT in the 2008 and 2009 austral winters to a depth of 18 uK-arcmin at 150 GHz; 550 deg2 of it was also mapped to 44 uK-arcmin at 95 GHz. Based on optical imaging of all candidates and near-infrared imaging of the majority of candidates, we have found optical and/or infrared counterparts for 158 clusters. Of these, 135 were first identified as clusters in SPT data, including 117 new discoveries reported in this work. This catalog triples the number of confirmed galaxy clusters discovered through the SZ effect. We report photometrically derived (and in some cases spectroscopic) redshifts for confirmed clusters and redshift lower limits for the remaining candidates. The catalog extends to high redshift with a median redshift of z = 0.55 and maximum redshift of z = 1.37. Based on simulations, we expect the catalog to be nearly 100% complete above M500 ~ 5e14 Msun h_{70}^-1 at z > 0.6. There are 121 candidates detected at signal-to-noise greater than five, at which the catalog purity is measured to be 95%. From this high-purity subsample, we exclude the z < 0.3 clusters and use the remaining 100 candidates to improve cosmological constraints following the method presented by Benson et al., 2011. Adding the cluster data to CMB+BAO+H0 data leads to a preference for non-zero neutrino masses while only slightly reducing the upper limit on the sum of neutrino masses to sum mnu < 0.38 eV (95% CL). For a spatially flat wCDM cosmological model, the addition of this catalog to the CMB+BAO+H0+SNe results yields sigma8=0.807+-0.027 and w = -1.010+-0.058, improving the constraints on these parameters by a factor of 1.4 and 1.3, respectively. [abbrev]

Published
2013

37. Design and characterization of 90 GHz feedhorn-coupled TES polarimeter pixels in the SPTpol camera

Author

Holland, WS, Zmuidzinas, J, Sayre, JT, Ade, P, Aird, KA, Austermann, JE, Beall, JA, Becker, D, Benson, BA, Bleem, LE, Britton, J, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, Datesman, A, de Haan, T, Dobbs, MA, Everett, W, Ewall-Wice, A, George, EM, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holzapfel, WL, Hubmayr, J, Irwin, KD, Karfunkle, M, Keisler, R, Kennedy, J, Lee, AT, Leitch, E, Li, D, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Montgomery, J, Montroy, TE, Nagy, J, Natoli, T, Nibarger, JP, Niemack, MD, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Shirokoff, E, Story, K, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Williamson, R, Yefremenko, V, Yoon, KW, Young, E, Holland, WS, Zmuidzinas, J, Sayre, JT, Ade, P, Aird, KA, Austermann, JE, Beall, JA, Becker, D, Benson, BA, Bleem, LE, Britton, J, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, Datesman, A, de Haan, T, Dobbs, MA, Everett, W, Ewall-Wice, A, George, EM, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holzapfel, WL, Hubmayr, J, Irwin, KD, Karfunkle, M, Keisler, R, Kennedy, J, Lee, AT, Leitch, E, Li, D, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Montgomery, J, Montroy, TE, Nagy, J, Natoli, T, Nibarger, JP, Niemack, MD, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Schaffer, KK, Shirokoff, E, Story, K, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Williamson, R, Yefremenko, V, Yoon, KW, and Young, E

Abstract

The SPTpol camera is a two-color, polarization-sensitive bolometer receiver, and was installed on the 10 meter South Pole Telescope in January 2012. SPTpol is designed to study the faint polarization signals in the Cosmic Microwave Background, with two primary scientific goals. One is to constrain the tensor-to-scalar ratio of perturbations in the primordial plasma, and thus constrain the space of permissible inflationary models. The other is to measure the weak lensing effect of large-scale structure on CMB polarization, which can be used to constrain the sum of neutrino masses as well as other growth-related parameters. The SPTpol focal plane consists of seven 84-element monolithic arrays of 150 GHz pixels (588 total) and 180 individual 90 GHz single-pixel modules. In this paper we present the design and characterization of the 90 GHz modules.

Published
2012

38. Feedhorn-Coupled TES Polarimeter Camera Modules at 150 GHz for CMB Polarization Measurements with SPTpol

Author

Holland, WS, Zmuidzinas, J, Henning, JW, Ade, P, Aird, KA, Austermann, JE, Beall, JA, Becker, D, Benson, BA, Bleem, LE, Britton, J, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, Datesman, A, de Haan, T, Dobbs, MA, Everett, W, Ewall-Wice, A, George, EM, Halverson, NW, Harrington, N, Hilton, GC, Holzapfel, WL, Hubmayr, J, Irwin, KD, Karfunkle, M, Keisler, R, Kennedy, J, Lee, AT, Leitch, E, Li, D, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Montgomery, J, Montroy, TE, Nagy, J, Natoli, T, Nibarger, JP, Niemack, MD, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Stroy, K, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Williamson, R, Yefremenko, V, Yoon, KW, Young, E, Holland, WS, Zmuidzinas, J, Henning, JW, Ade, P, Aird, KA, Austermann, JE, Beall, JA, Becker, D, Benson, BA, Bleem, LE, Britton, J, Carlstrom, JE, Chang, CL, Cho, H-M, Crawford, TM, Crites, AT, Datesman, A, de Haan, T, Dobbs, MA, Everett, W, Ewall-Wice, A, George, EM, Halverson, NW, Harrington, N, Hilton, GC, Holzapfel, WL, Hubmayr, J, Irwin, KD, Karfunkle, M, Keisler, R, Kennedy, J, Lee, AT, Leitch, E, Li, D, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Montgomery, J, Montroy, TE, Nagy, J, Natoli, T, Nibarger, JP, Niemack, MD, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Stroy, K, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Williamson, R, Yefremenko, V, Yoon, KW, and Young, E

Abstract

The SPTpol camera is a dichroic polarimetric receiver at 90 and 150 GHz. Deployed in January 2012 on the South Pole Telescope (SPT), SPTpol is looking for faint polarization signals in the Cosmic Microwave Background (CMB). The camera consists of 180 individual Transition Edge Sensor (TES) polarimeters at 90 GHz and seven 84-polarimeter camera modules (a total of 588 polarimeters) at 150 GHz. We present the design, dark characterization, and in-lab optical properties of the 150 GHz camera modules. The modules consist of photolithographed arrays of TES polarimeters coupled to silicon platelet arrays of corrugated feedhorns, both of which are fabricated at NIST-Boulder. In addition to mounting hardware and RF shielding, each module also contains a set of passive readout electronics for digital frequency-domain multiplexing. A single module, therefore, is fully functional as a miniature focal plane and can be tested independently. Across the modules tested before deployment, the detectors average a critical temperature of 478 mK, normal resistance R_N of 1.2 Ohm, unloaded saturation power of 22.5 pW, (detector-only) optical efficiency of ~ 90%, and have electrothermal time constants < 1 ms in transition.

Published
2012

39. Performance and on-sky optical characterization of the SPTpol instrument

Author

Holland, WS, Zmuidzinas, J, George, EM, Ade, P, Aird, KA, Austermann, JE, Beall, JA, Becker, D, Bender, A, Benson, BA, Bleem, LE, Britton, J, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Crawford, TM, Crites, AT, Datesman, A, de Haan, T, Dobbs, MA, Everett, W, Ewall-Wice, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holzapfel, WL, Hoover, S, Huang, N, Hubmayr, J, Irwin, KD, Karfunkle, M, Keisler, R, Kennedy, J, Lee, AT, Leitch, E, Li, D, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Montgomery, J, Montroy, TE, Nagy, J, Natoli, T, Nibarger, JP, Niemack, MD, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Story, K, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Williamson, R, Yefremenko, V, Yoon, KW, Young, E, Holland, WS, Zmuidzinas, J, George, EM, Ade, P, Aird, KA, Austermann, JE, Beall, JA, Becker, D, Bender, A, Benson, BA, Bleem, LE, Britton, J, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Crawford, TM, Crites, AT, Datesman, A, de Haan, T, Dobbs, MA, Everett, W, Ewall-Wice, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holzapfel, WL, Hoover, S, Huang, N, Hubmayr, J, Irwin, KD, Karfunkle, M, Keisler, R, Kennedy, J, Lee, AT, Leitch, E, Li, D, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Montgomery, J, Montroy, TE, Nagy, J, Natoli, T, Nibarger, JP, Niemack, MD, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Story, K, Tucker, C, Vanderlinde, K, Vieira, JD, Wang, G, Williamson, R, Yefremenko, V, Yoon, KW, and Young, E

Abstract

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.

Published
2012

40. SPTpol: an instrument for CMB polarization measurements with the South Pole Telescope

Author

Holland, WS, Zmuidzinas, J, Austermann, JE, Aird, KA, Beall, JA, Becker, D, Bender, A, Benson, BA, Bleem, LE, Britton, J, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Crawford, TM, Crites, AT, Datesman, A, de Haan, T, Dobbs, MA, George, EM, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Kennedy, J, Knox, L, Lee, AT, Leitch, E, Li, D, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Montroy, TE, Natoli, T, Nibarger, JP, Niemack, MD, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Stark, AA, Story, K, Vanderlinde, K, Vieira, JD, Wang, G, Williamson, R, Yefremenko, V, Woon, KW, Zahn, O, Holland, WS, Zmuidzinas, J, Austermann, JE, Aird, KA, Beall, JA, Becker, D, Bender, A, Benson, BA, Bleem, LE, Britton, J, Carlstrom, JE, Chang, CL, Chiang, HC, Cho, H-M, Crawford, TM, Crites, AT, Datesman, A, de Haan, T, Dobbs, MA, George, EM, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hoover, S, Huang, N, Hubmayr, J, Irwin, KD, Keisler, R, Kennedy, J, Knox, L, Lee, AT, Leitch, E, Li, D, Lueker, M, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Montroy, TE, Natoli, T, Nibarger, JP, Niemack, MD, Novosad, V, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Stark, AA, Story, K, Vanderlinde, K, Vieira, JD, Wang, G, Williamson, R, Yefremenko, V, Woon, KW, and Zahn, O

Abstract

SPTpol is a dual-frequency polarization-sensitive camera that was deployed on the 10-meter South Pole Telescope in January 2012. SPTpol will measure the polarization anisotropy of the cosmic microwave background (CMB) on angular scales spanning an arcminute to several degrees. The polarization sensitivity of SPTpol will enable a detection of the CMB "B-mode" polarization from the detection of the gravitational lensing of the CMB by large scale structure, and a detection or improved upper limit on a primordial signal due to inflationary gravity waves. The two measurements can be used to constrain the sum of the neutrino masses and the energy scale of inflation. These science goals can be achieved through the polarization sensitivity of the SPTpol camera and careful control of systematics. The SPTpol camera consists of 768 pixels, each containing two transition-edge sensor (TES) bolometers coupled to orthogonal polarizations, and a total of 1536 bolometers. The pixels are sensitive to light in one of two frequency bands centered at 90 and 150 GHz, with 180 pixels at 90 GHz and 588 pixels at 150 GHz. The SPTpol design has several features designed to control polarization systematics, including: single-moded feedhorns with low cross-polarization, bolometer pairs well-matched to difference atmospheric signals, an improved ground shield design based on far-sidelobe measurements of the SPT, and a small beam to reduce temperature to polarization leakage. We present an overview of the SPTpol instrument design, project status, and science projections.

Published
2012

41. SOUTH POLE TELESCOPE DETECTIONS OF THE PREVIOUSLY UNCONFIRMED PLANCK EARLY SUNYAEV-ZEL'DOVICH CLUSTERS IN THE SOUTHERN HEMISPHERE

Author

Story, K, Aird, KA, Andersson, K, Armstrong, R, Bazin, G, Benson, BA, Bleem, LE, Bonamente, M, Brodwin, M, Carlstrom, JE, Chang, CL, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Stubbs, CW, Vanderlinde, K, Vieira, JD, Williamson, R, Zenteno, A, Story, K, Aird, KA, Andersson, K, Armstrong, R, Bazin, G, Benson, BA, Bleem, LE, Bonamente, M, Brodwin, M, Carlstrom, JE, Chang, CL, Clocchiatti, A, Crawford, TM, Crites, AT, de Haan, T, Desai, S, Dobbs, MA, Dudley, JP, Foley, RJ, George, EM, Gladders, MD, Gonzalez, AH, Halverson, NW, High, FW, Holder, GP, Holzapfel, WL, Hoover, S, Hrubes, JD, Joy, M, Keisler, R, Knox, L, Lee, AT, Leitch, EM, Lueker, M, Luong-Van, D, Marrone, DP, McMahon, JJ, Mehl, J, Meyer, SS, Mohr, JJ, Montroy, TE, Padin, S, Plagge, T, Pryke, C, Reichardt, CL, Rest, A, Ruel, J, Ruhl, JE, Saliwanchik, BR, Saro, A, Schaffer, KK, Shaw, L, Shirokoff, E, Song, J, Spieler, HG, Stalder, B, Staniszewski, Z, Stark, AA, Stubbs, CW, Vanderlinde, K, Vieira, JD, Williamson, R, and Zenteno, A

Abstract

We present South Pole Telescope (SPT) observations of the five galaxy cluster candidates in the southern hemisphere which were reported as unconfirmed in the Planck Early Sunyaev-Zel'dovich (ESZ) sample. One cluster candidate, PLCKESZ G255.62-46.16, is located in the 2500-square-degree SPT SZ survey region and was reported previously as SPT-CL J0411-4819. For the remaining four candidates, which are located outside of the SPT SZ survey region, we performed short, dedicated SPT observations. Each of these four candidates was strongly detected in maps made from these observations, with signal-to-noise ratios ranging from 6.3 to 13.8. We have observed these four candidates on the Magellan-Baade telescope and used these data to estimate cluster redshifts from the red sequence. Resulting redshifts range from 0.24 to 0.46. We report measurements of Y_0.75', the integrated Comptonization within a 0.75' radius, for all five candidates. We also report X-ray luminosities calculated from ROSAT All-Sky Survey catalog counts, as well as optical and improved SZ coordinates for each candidate. The combination of SPT SZ measurements, optical red-sequence measurements, and X-ray luminosity estimates demonstrates that these five Planck ESZ cluster candidates do indeed correspond to real galaxy clusters with redshifts and observable properties consistent with the rest of the ESZ sample.

Published
2011

42. First Constraints on the Epoch of Reionization Using the Non-Gaussianity of the Kinematic Sunyaev-Zel'dovich Effect from the South Pole Telescope and Herschel-SPIRE Observations.

Author

Raghunathan S, Ade PAR, Anderson AJ, Ansarinejad B, Archipley M, Austermann JE, Balkenhol L, Beall JA, Benabed K, Bender AN, Benson BA, Bianchini F, Bleem LE, Bock J, Bouchet FR, Bryant L, Camphuis E, Carlstrom JE, Cecil TW, Chang CL, Chaubal P, Chiang HC, Chichura PM, Chou TL, Citron R, Coerver A, Crawford TM, Crites AT, Cukierman A, Daley C, Dibert KR, Dobbs MA, Doussot A, Dutcher D, Everett W, Feng C, Ferguson KR, Fichman K, Foster A, Galli S, Gallicchio J, Gambrel AE, Gardner RW, Ge F, George EM, Goeckner-Wald N, Gualtieri R, Guidi F, Guns S, Gupta N, de Haan T, Halverson NW, Hivon E, Holder GP, Holzapfel WL, Hood JC, Hrubes JD, Hryciuk A, Huang N, Hubmayr J, Irwin KD, Kéruzoré F, Khalife AR, Knox L, Korman M, Kornoelje K, Kuo CL, Lee AT, Levy K, Li D, Lowitz AE, Lu C, Maniyar A, Martsen ES, McMahon JJ, Menanteau F, Millea M, Montgomery J, Corbett Moran C, Nakato Y, Natoli T, Nibarger JP, Noble GI, Novosad V, Omori Y, Padin S, Pan Z, Paschos P, Patil S, Phadke KA, Prabhu K, Pryke C, Quan W, Rahimi M, Rahlin A, Reichardt CL, Rouble M, Ruhl JE, Saliwanchik BR, Schaffer KK, Schiappucci E, Sievers C, Smecher G, Sobrin JA, Stark AA, Stephen J, Suzuki A, Tandoi C, Thompson KL, Thorne B, Trendafilova C, Tucker C, Umilta C, Veach T, Vieira JD, Viero MP, Wan Y, Wang G, Whitehorn N, Wu WLK, Yefremenko V, Young MR, Zebrowski JA, and Zemcov M

Abstract

We report results from an analysis aimed at detecting the trispectrum of the kinematic Sunyaev-Zel'dovich (kSZ) effect by combining data from the South Pole Telescope (SPT) and Herschel-SPIRE experiments over a 100  deg^{2} field. The SPT observations combine data from the previous and current surveys, namely SPTpol and SPT-3G, to achieve depths of 4.5, 3, and 16  μK-arcmin in bands centered at 95, 150, and 220 GHz. For SPIRE, we include data from the 600 and 857 GHz bands. We reconstruct the velocity-induced large-scale correlation of the small-scale kSZ signal with a quadratic estimator that uses two cosmic microwave background (CMB) temperature maps, constructed by optimally combining data from all the frequency bands. We reject the null hypothesis of a zero trispectrum at 10.3σ level. However, the measured trispectrum contains contributions from both the kSZ and other undesired components, such as CMB lensing and astrophysical foregrounds, with kSZ being sub-dominant. We use the agora simulations to estimate the expected signal from CMB lensing and astrophysical foregrounds. After accounting for the contributions from CMB lensing and foreground signals, we do not detect an excess kSZ-only trispectrum and use this nondetection to set constraints on reionization. By applying a prior based on observations of the Gunn-Peterson trough, we obtain an upper limit on the duration of reionization of Δz&#95;{re,50}<4.5 (95% confidence level). We find these constraints are fairly robust to foregrounds assumptions. This trispectrum measurement is independent of, but consistent with, Planck's optical depth measurement. This result is the first constraint on the epoch of reionization using the non-Gaussian nature of the kSZ signal.

Published
2024
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43. Detection of CMB-Cluster Lensing using Polarization Data from SPTpol.

Author

Raghunathan S, Patil S, Baxter E, Benson BA, Bleem LE, Crawford TM, Holder GP, McClintock T, Reichardt CL, Varga TN, Whitehorn N, Ade PAR, Allam S, Anderson AJ, Austermann JE, Avila S, Avva JS, Bacon D, Beall JA, Bender AN, Bianchini F, Bocquet S, Brooks D, Burke DL, Carlstrom JE, Carretero J, Castander FJ, Chang CL, Chiang HC, Citron R, Costanzi M, Crites AT, da Costa LN, Desai S, Diehl HT, Dietrich JP, Dobbs MA, Doel P, Everett S, Evrard AE, Feng C, Flaugher B, Fosalba P, Frieman J, Gallicchio J, García-Bellido J, Gaztanaga E, George EM, Giannantonio T, Gilbert A, Gruendl RA, Gschwend J, Gupta N, Gutierrez G, de Haan T, Halverson NW, Harrington N, Henning JW, Hilton GC, Hollowood DL, Holzapfel WL, Honscheid K, Hrubes JD, Huang N, Hubmayr J, Irwin KD, Jeltema T, Kind MC, Knox L, Kuropatkin N, Lahav O, Lee AT, Li D, Lima M, Lowitz A, Maia MAG, Marshall JL, McMahon JJ, Melchior P, Menanteau F, Meyer SS, Miquel R, Mocanu LM, Mohr JJ, Montgomery J, Moran CC, Nadolski A, Natoli T, Nibarger JP, Noble G, Novosad V, Ogando RLC, Padin S, Plazas AA, Pryke C, Rapetti D, Romer AK, Roodman A, Rosell AC, Rozo E, Ruhl JE, Rykoff ES, Saliwanchik BR, Sanchez E, Sayre JT, Scarpine V, Schaffer KK, Schubnell M, Serrano S, Sevilla-Noarbe I, Sievers C, Smecher G, Smith M, Soares-Santos M, Stark AA, Story KT, Suchyta E, Swanson MEC, Tarle G, Tucker C, Vanderlinde K, Veach T, De Vicente J, Vieira JD, Vikram V, Wang G, Wu WLK, Yefremenko V, and Zhang Y

Abstract

We report the first detection of gravitational lensing due to galaxy clusters using only the polarization of the cosmic microwave background (CMB). The lensing signal is obtained using a new estimator that extracts the lensing dipole signature from stacked images formed by rotating the cluster-centered Stokes QU map cutouts along the direction of the locally measured background CMB polarization gradient. Using data from the SPTpol 500  deg^{2} survey at the locations of roughly 18 000 clusters with richness λ≥10 from the Dark Energy Survey (DES) Year-3 full galaxy cluster catalog, we detect lensing at 4.8σ. The mean stacked mass of the selected sample is found to be (1.43±0.40)×10^{14}M&#95;{⊙} which is in good agreement with optical weak lensing based estimates using DES data and CMB-lensing based estimates using SPTpol temperature data. This measurement is a key first step for cluster cosmology with future low-noise CMB surveys, like CMB-S4, for which CMB polarization will be the primary channel for cluster lensing measurements.

Published
2019
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44. Detection of B-mode polarization in the cosmic microwave background with data from the South Pole Telescope.

Author

Hanson D, Hoover S, Crites A, Ade PA, Aird KA, Austermann JE, Beall JA, Bender AN, Benson BA, Bleem LE, Bock JJ, Carlstrom JE, Chang CL, Chiang HC, Cho HM, Conley A, Crawford TM, de Haan T, Dobbs MA, Everett W, Gallicchio J, Gao J, George EM, Halverson NW, Harrington N, Henning JW, Hilton GC, Holder GP, Holzapfel WL, Hrubes JD, Huang N, Hubmayr J, Irwin KD, Keisler R, Knox L, Lee AT, Leitch E, Li D, Liang C, Luong-Van D, Marsden G, McMahon JJ, Mehl J, Meyer SS, Mocanu L, Montroy TE, Natoli T, Nibarger JP, Novosad V, Padin S, Pryke C, Reichardt CL, Ruhl JE, Saliwanchik BR, Sayre JT, Schaffer KK, Schulz B, Smecher G, Stark AA, Story KT, Tucker C, Vanderlinde K, Vieira JD, Viero MP, Wang G, Yefremenko V, Zahn O, and Zemcov M

Abstract

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 gravity-wave 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 nonzero 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.

Published
2013
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45. A massive, cooling-flow-induced starburst in the core of a luminous cluster of galaxies.

Author

McDonald M, Bayliss M, Benson BA, Foley RJ, Ruel J, Sullivan P, Veilleux S, Aird KA, Ashby ML, Bautz M, Bazin G, Bleem LE, Brodwin M, Carlstrom JE, Chang CL, Cho HM, Clocchiatti A, Crawford TM, Crites AT, de Haan T, Desai S, Dobbs MA, Dudley JP, Egami E, Forman WR, Garmire GP, George EM, Gladders MD, Gonzalez AH, Halverson NW, Harrington NL, High FW, Holder GP, Holzapfel WL, Hoover S, Hrubes JD, Jones C, Joy M, Keisler R, Knox L, Lee AT, Leitch EM, Liu J, Lueker M, Luong-Van D, Mantz A, Marrone DP, McMahon JJ, Mehl J, Meyer SS, Miller ED, Mocanu L, Mohr JJ, Montroy TE, Murray SS, Natoli T, Padin S, Plagge T, Pryke C, Rawle TD, Reichardt CL, Rest A, Rex M, Ruhl JE, Saliwanchik BR, Saro A, Sayre JT, Schaffer KK, Shaw L, Shirokoff E, Simcoe R, Song J, Spieler HG, Stalder B, Staniszewski Z, Stark AA, Story K, Stubbs CW, Suhada R, van Engelen A, Vanderlinde K, Vieira JD, Vikhlinin A, Williamson R, Zahn O, and Zenteno A

Abstract

In the cores of some clusters of galaxies the hot intracluster plasma is dense enough that it should cool radiatively in the cluster's lifetime, leading to continuous 'cooling flows' of gas sinking towards the cluster centre, yet no such cooling flow has been observed. The low observed star-formation rates and cool gas masses for these 'cool-core' clusters suggest that much of the cooling must be offset by feedback to prevent the formation of a runaway cooling flow. Here we report X-ray, optical and infrared observations of the galaxy cluster SPT-CLJ2344-4243 (ref. 11) at redshift z = 0.596. These observations reveal an exceptionally luminous (8.2 × 10(45) erg s(-1)) galaxy cluster that hosts an extremely strong cooling flow (around 3,820 solar masses a year). Further, the central galaxy in this cluster appears to be experiencing a massive starburst (formation of around 740 solar masses a year), which suggests that the feedback source responsible for preventing runaway cooling in nearby cool-core clusters may not yet be fully established in SPT-CLJ2344-4243. This large star-formation rate implies that a significant fraction of the stars in the central galaxy of this cluster may form through accretion of the intracluster medium, rather than (as is currently thought) assembling entirely via mergers.

Published
2012
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