A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS

By C. Reichardt, L. Shaw, Oliver Zahn, K. Aird, B. Benson, L. Bleem, J. Carlstrom, C. Chang, Hsiao-mei Cho, T. Crawford and 39 more. 2011

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We present the first three-frequency South Pole Telescope (SPT) cosmic microwave background (CMB) power spectra. The band powers presented here cover angular scales 2000 < ℓ < 9400 in frequency bands centered at 95, 150, and 220 GHz. At these frequencies and angular scales, a combination of the primary CMB anisotropy, thermal and kinetic Sunyaev–Zel'dovich (SZ) effects, radio galaxies, and cosmic infrared background (CIB) contributes to the signal. We combine Planck/HFI and SPT data at 220 GHz to constrain the amplitude and shape of the CIB power spectrum and find strong evidence for nonlinear clustering. We explore the SZ results using a variety of cosmological models for the CMB and CIB anisotropies and find them to be robust with one exception: allowing for spatial correlations between the thermal SZ effect and CIB significantly degrades the SZ constraints. Neglecting this potential correlation, we find the thermal SZ power at 150 GHz and ℓ = 3000 to be 3.65 ± 0.69 μK2, and set an upper limit on the kinetic SZ power to be less than 2.8 μK2 at 95% confidence. When a correlation between the thermal SZ and CIB is allowed, we constrain a linear combination of thermal and kinetic SZ power: D tSZ 3000 + 0.5D 3000 kSZ = 4.60 ± 0.63 μK2, consistent with earlier measurements. We use the measured thermal SZ power and an analytic, thermal SZ model calibrated with simulations to determine σ8 = 0.807 ± 0.016. Modeling uncertainties involving the astrophysics of the intracluster medium rather than the statistical uncertainty in the measured band powers are the dominant source of uncertainty on σ8. We also place an upper limit on the kinetic SZ power produced by patchy reionization; a companion paper uses these limits to constrain the reionization history of the universe.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0244ed01e522cd62367042f2c798661522a59bf3

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Citations in the corpus

The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, background): “Gravitational lensing of the CMB and its cross-correlation with galaxy lensing (Blanchard and Schneider, 1987; Cole and Efstathiou, 1989; Bernardeau, 1997; Linder, 1990; Seljak, 1996; Metcalf and Silk, 1997; Zaldarriaga and Seljak, 1998; Hu and Okamoto, 2002; Sherwin et al., 2011; van Engelen et al.”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the full shape of the clustering wedges in the data release 10 and 11 galaxy samples (2013, methodology): “We extend this data set using the high- CMB measurements from the Atacama Cosmology Telescope (ACT; Das et al. 2013) and the South Pole Telescope (SPT; Keisler et al. 2011; Reichardt et al. 2012; Story et al. 2013).”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2014, methodology): “The simulated radio population follows the results of De Zotti et al. (2005), Vieira et al. (2010), and Reichardt et al. (2012).”
The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data (2013, background): “While the B12 normalization lies somewhat below the UPP prediction, we note that even lower normalizations (such as that found in the Nonthermal20 model) are favored by recent measurements of the SZ contribution to the CMB angular power spectrum [28, 90].”
NEW CONSTRAINTS ON COSMIC REIONIZATION FROM THE 2012 HUBBLE ULTRA DEEP FIELD CAMPAIGN (2013, background): “Both the Atacama Cosmology Telescope and the South Pole Telescope have placed upper limits on this signal (Dunkley et al. 2011; Reichardt et al. 2012).”
Signatures of X-rays in the early Universe (2012, methodology): “Indeed, recent SPT measurements place a bound of [∆l3000] 2 < 2.8 µK2 at 95% confidence limit (C.L.), which degrades to [∆l3000]2 < 6 µK2 if a significant correlation between the tSZ and the CIB is allowed (Reichardt et al. 2012).”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, methodology): “These “patchy kSZ” anisotropies have only recently been used to place constraints on the duration of reionization [410, 411, 412, 413].”
Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples (2014, methodology): “Better constraints on the foreground contamination of the temperature spectrum can also be obtained from higher resolution experiments, such as the Atacama Cosmology Telescope (Das et al. 2014) and the South Pole Telescope (Reichardt et al. 2012).”
Cosmology and astrophysics from relaxed galaxy clusters - II. Cosmological constraints (2014, methodology): “…and the Planck satellite (1-year release, including WMAP polarization data; Planck Collaboration 2013b), as well as high-multipole data from the Atacama Cosmology Telescope (ACT; Das et al. 2013) and the South Pole Telescope (SPT; Keisler et al. 2011; Reichardt et al. 2012; Story et al. 2013).”
A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND DAMPING TAIL FROM THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2012, methodology): “As in K11 and Reichardt et al. (2012), the absolute calibration is determined by comparing the SPT and WMAP7 power in several ℓ-bins over the multipole range ℓ ∈ [650, 1000].”
The Atacama Cosmology Telescope: likelihood for small-scale CMB data (2013, methodology): “Spectra are reported in Keisler et al. (2011) for angular scales 650 < ℓ < 3000 at 150 GHz, and in Reichardt et al. (2012) for angular scales 2000 < ℓ < 9400 at 95, 150 and 220 GHz.”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES FROM THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2014, methodology): “Improved SPT measurements of the power spectrum have since been reported by Shirokoff et al. (2011) and Reichardt et al. (2012) (hereafter S11 and R12) using 200 deg2 and 800 deg2 of data respectively.”
SPTpol: an instrument for CMB polarization measurements with the South Pole Telescope (2012, background): “Measurements on these scales will also provide constraints on the evolution of the ionized fraction during the epoch of reionization through the kinetic SZ effect.(9,25) Comparing the gravitational lensing of the CMB to galaxy surveys or other external mass tracers provides another source of constra”