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A Measurement of Secondary Cosmic Microwave Background Anisotropies from the 2500 Square-degree SPT-SZ Survey

George, E. M. and Crites, A. T. and Lueker, M. and Padin, S. (2015) A Measurement of Secondary Cosmic Microwave Background Anisotropies from the 2500 Square-degree SPT-SZ Survey. Astrophysical Journal, 799 (2). Art. No. 177. ISSN 0004-637X.

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We present measurements of secondary cosmic microwave background (CMB) anisotropies and cosmic infrared background (CIB) fluctuations using data from the South Pole Telescope (SPT) covering the complete 2540 deg^2 SPT-SZ survey area. Data in the three SPT-SZ frequency bands centered at 95, 150, and 220 GHz, are used to produce six angular power spectra (three single-frequency auto-spectra and three cross-spectra) covering the multipole range 2000 < ℓ < 11, 000 (angular scales 5' gsim θ gsim 1'). These are the most precise measurements of the angular power spectra at ℓ > 2500 at these frequencies. The main contributors to the power spectra at these angular scales and frequencies are the primary CMB, CIB, thermal and kinematic Sunyaev-Zel'dovich effects (tSZ and kSZ), and radio galaxies. We include a constraint on the tSZ power from a measurement of the tSZ bispectrum from 800 deg^2 of the SPT-SZ survey. We measure the tSZ power at 143 GHz to be D^(tSZ)_(3000) = 4.08^(+0.58)_(-0.67) µK^2 and the kSZ power to be D^(kSZ)_(3000) = 2.9 \pm 1.3 µK^2. The data prefer positive kSZ power at 98.1% CL. We measure a correlation coefficient of ξ = 0.113^(+0.057)_(-0.054) between sources of tSZ and CIB power, with ξ < 0 disfavored at a confidence level of 99.0%. The constraint on kSZ power can be interpreted as an upper limit on the duration of reionization. When the post-reionization homogeneous kSZ signal is accounted for, we find an upper limit on the duration Δz < 5.4 at 95% CL.

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Additional Information:© 2015 American Astronomical Society. Received 2014 August 17; accepted 2014 November 30; published 2015 January 28. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. R. Keisler acknowledges support from NASA Hubble Fellowship grant HF-51275.01. M. Dobbs acknowledges support from an Alfred P. Sloan Research Fellowship. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science.
Funding AgencyGrant Number
NSF Physics Frontier CenterPHY-1125897
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore FoundationGBMF 947
National Sciences and Engineering Research Council of CanadaUNSPECIFIED
Canada Research Chairs programUNSPECIFIED
Canadian Institute for Advanced ResearchUNSPECIFIED
NASA Hubble FellowshipHF-51275.01
Alfred P. Sloan Research FellowshipUNSPECIFIED
Department of Energy (DOE) Office of ScienceDE-AC02- 05CH11231
NASA Office of Space ScienceUNSPECIFIED
Subject Keywords: cosmic background radiation; cosmology: observations; dark ages, reionization, first stars; diffuse radiation; large-scale structure of universe
Issue or Number:2
Record Number:CaltechAUTHORS:20150306-141643827
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Official Citation: A Measurement of Secondary Cosmic Microwave Background Anisotropies from the 2500 Square-degree SPT-SZ Survey E. M. George et al. 2015 ApJ 799 177
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:55610
Deposited By: Ruth Sustaita
Deposited On:06 Mar 2015 23:09
Last Modified:03 Oct 2019 08:07

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