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Constraints on Cosmology from the Cosmic Microwave Background Power Spectrum of the 2500-square degree SPT-SZ Survey

Hou, Z. and Reichardt, C. L. and Story, K. T. and Follin, B. and Keisler, R. and Aird, K. A. and Benson, B. A. and Bleem, L. E. and Carlstrom, J. E. and Chang, C. L. and Cho, H-M. and Crawford, T. M. and Crites, A. T. and de Haan, T. and de Putter, R. and Dobbs, M. A. and Dodelson, S. and Dudley, J. and George, E. M. and Halverson, N. W. and Holder, G. P. and Holzapfel, W. L. and Hoover, S. and Hrubes, J. D. and Joy, M. and Knox, L. and Lee, A. T. and Leitch, E. M. and Lueker, M. and Luong-Van, D. and McMahon, J. J. and Mehl, J. and Meyer, S. S. and Millea, M. and Mohr, J. J. and Montroy, T. E. and Padin, S. and Plagge, T. and Pryke, C. and Ruhl, J. E. and Sayre, J. T. and Schaffer, K. K. and Shaw, L. and Shirokoff, E. and Spieler, H. G. and Staniszewski, Z. and Stark, A. A. and van Engelen, A. and Vanderlinde, K. and Vieira, J. D. and Williamson, R. and Zahn, O. (2012) Constraints on Cosmology from the Cosmic Microwave Background Power Spectrum of the 2500-square degree SPT-SZ Survey. . (Submitted) http://resolver.caltech.edu/CaltechAUTHORS:20130116-103559968

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Abstract

We explore extensions to the standard LCDM cosmological model using new measurements of the cosmic microwave background (CMB) from the South Pole Telescope (SPT). Adding SPT measurements to WMAP7 significantly improves constraints on possible extensions to the LCDM model; the addition of low-redshift measurements of H0 and BAO leads to further improvements. Before combining these datasets, we check for consistency in the LCDM model between measurements of the CMB (SPT+WMAP7), H0 and BAO, and find evidence for some tension between the datasets. Within the CMB data alone, we find only weak support for physics beyond the LCDM model due to a slight trend of decreasing power at smaller angular scales, relative to the prediction of the LCDM model. This trend could be due to a logarithmic scale dependence of the power-law index of the primordial power spectrum, nrun. Alternatively, the trend could arise either from adjustments at small or large scales. The power at small scales is sensitive to the damping scale which is influenced by both the helium abundance, Yp and the effective number of neutrino species, Neff. The power at large scales is affected by the ISW effect which is sensitive to the sum of neutrino masses, mnu. These extensions have similar observational consequences and are partially degenerate when considered simultaneously. These degeneracies can weaken or enhance the apparent deviation of any single extension from the LCDM model. Of the 6 one-parameter model extensions considered, we find the CMB data to have the largest statistical preference for running within [-0.046, -0.003] at 95% confidence...[abridged]


Item Type:Report or Paper (Working Paper)
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http://arxiv.org/abs/1212.6267v1arXivUNSPECIFIED
Additional Information:Imported from arXiv. The SPT is supported by the National Science Foun- dation through grant ANT-0638937, with partial sup- port provided by NSF grant PHY-1125897, the Kavli Foundation, and the Gordon and Betty Moore Foun- dation. 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, B.A. Benson a KICP Fellowship, M. Dobbs an Alfred P. Sloan Research Fellowship, O. Zahn a BCCP fellowship. This research used resources of the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE- AC02-05CH11231, and the resources of the University of Chicago Computing Cooperative (UC3), supported in part by the Open Science Grid, NSF grant NSF PHY 1148698. 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
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFANT-0638937
NSFPHY-1125897
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore FoundationUNSPECIFIED
National Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canada Research ChairsUNSPECIFIED
Canadian Institute for Advanced ResearchUNSPECIFIED
NASA Hubble FellowshipHF-51275.01
Department of EnergyDE- AC02-05CH11231
NSFPHY-1148698
NASA Office of Space ScienceUNSPECIFIED
Record Number:CaltechAUTHORS:20130116-103559968
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20130116-103559968
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36424
Collection:CaltechAUTHORS
Deposited By: JoAnn Boyd
Deposited On:07 Feb 2013 11:39
Last Modified:14 Feb 2013 23:03

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