IMPROVED CONSTRAINTS ON COSMIC MICROWAVE BACKGROUND SECONDARY ANISOTROPIES FROM THE COMPLETE 2008 SOUTH POLE TELESCOPE DATA
- Department of Physics, University of California, Berkeley, CA 94720 (United States)
- Department of Physics, Yale University, P.O. Box 208210, New Haven, CT 06520-8120 (United States)
- Department of Physics, University of California, One Shields Avenue, Davis, CA 95616 (United States)
- Department of Physics and Astronomy, Cardiff University, CF24 3YB (United Kingdom)
- University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States)
- Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States)
- NIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, CO 80305 (United States)
- Department of Physics, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8 (Canada)
We report measurements of the cosmic microwave background (CMB) power spectrum from the complete 2008 South Pole Telescope (SPT) data set. We analyze twice as much data as the first SPT power spectrum analysis, using an improved cosmological parameter estimator which fits multi-frequency models to the SPT 150 and 220 GHz bandpowers. We find an excellent fit to the measured bandpowers with a model that includes lensed primary CMB anisotropy, secondary thermal (tSZ) and kinetic (kSZ) Sunyaev-Zel'dovich anisotropies, unclustered synchrotron point sources, and clustered dusty point sources. In addition to measuring the power spectrum of dusty galaxies at high signal-to-noise, the data primarily constrain a linear combination of the kSZ and tSZ anisotropy contributions at 150 GHz and l = 3000: D{sup tSZ}{sub 3000} + 0.5 D{sup kSZ}{sub 3000} = 4.5 {+-} 1.0 {mu}K{sup 2}. The 95% confidence upper limits on secondary anisotropy power are D{sup tSZ}{sub 3000} < 5.3 {mu}K{sup 2} and D{sup kSZ}{sub 3000} < 6.5 {mu}K{sup 2}. We also consider the potential correlation of dusty and tSZ sources and find it incapable of relaxing the tSZ upper limit. These results increase the significance of the lower than expected tSZ amplitude previously determined from SPT power spectrum measurements. We find that models including non-thermal pressure support in groups and clusters predict tSZ power in better agreement with the SPT data. Combining the tSZ power measurement with primary CMB data halves the statistical uncertainty on {sigma}{sub 8}. However, the preferred value of {sigma}{sub 8} varies significantly between tSZ models. Improved constraints on cosmological parameters from tSZ power spectrum measurements require continued progress in the modeling of the tSZ power.
- OSTI ID:
- 21578304
- Journal Information:
- Astrophysical Journal, Vol. 736, Issue 1; Other Information: DOI: 10.1088/0004-637X/736/1/61; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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