Journal
ASTROPHYSICAL JOURNAL
Volume 755, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.1088/0004-637X/755/1/70
Keywords
cosmic background radiation; cosmological parameters; cosmology: observations; diffuse radiation; large-scale structure of universe
Categories
Funding
- National Science Foundation [ANT-0638937, ANT-0130612]
- NSF Physics Frontier Center [PHY-0114422]
- National Sciences and Engineering Research Council of Canada
- Canada Research Chairs program
- Canadian Institute for Advanced Research
- NASA [HF-51275.01]
- KICP
- Alfred P. Sloan Research Fellowship
- Yale University
- NSF [AST-1009811, 0709498]
- Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]
- NASA Office of Space Science
- Kavli Foundation
- Gordon and Betty Moore Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1125897] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0709498] Funding Source: National Science Foundation
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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 mu K-2, and set an upper limit on the kinetic SZ power to be less than 2.8 mu K-2 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-3000(tSZ) + 0.5(3000)(DkSZ) = 4.60 +/- 0.63 mu K-2, consistent with earlier measurements. We use the measured thermal SZ power and an analytic, thermal SZ model calibrated with simulations to determine sigma(8) = 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 sigma(8). 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.
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