Project Supported by

NSF, National Science Foundation
KICP, Kavli Institute for Cosmological Physics
USAP, United States Antarctic Program
Raytheon Polar Support Corporation


Related Websites

CBI, Cosmic Background Imager
DASI, Degree Angular Scale Interferometer
WMAP, Wilkinson Microwave Anisotropy Probe




 Overview 




This page provides data products associated with the SPT measurement of the CMB power spectrum described in astroph/1105.3182, Keisler et al 2011. The power spectrum is presented over the multipole range 650 < ell < 3000 and can be used to refine cosmological models.
If you have any questions regarding this data set or its use, please contact Ryan Keisler (rkeisler_at_uchicago_edu).


 Figures 




Individual figures are available in PDF format here or bundled in a ZIP file here. Below we show a couple of example figures.

The SPT power spectrum is shown here.
The peak at ell~800 is the third acoustic peak.
The bandpower errors shown do not include beam or calibration uncertainties.
(This is the left panel of Figure 4 in Keisler et al. 2011.)


The SPT bandpowers, WMAP bandpowers, and bestfit LCDM theory spectrum shown with dashed (CMB) and solid (CMB+foregrounds) lines. The bandpower errors do not include beam or calibration uncertainties.
(This is Figure 5 in Keisler et al. 2011.)



 Bandpowers 




These are the SPT 150 GHz Bandpowers from 2008+2009 observations. The bandpowers cover the multipole range 650 < ell < 3000.
Note that these bandpowers include power from foreground components such as SZ and point sources. The contributions from these components must be accounted for in order to properly analyze the SPT bandpowers, as described in Section 4.1 of Keisler et al. For convenience we give the ellspace templates for these components (in "units" of D_ell=C_ell*ell*(ell+1)/2PI and normalized to equal 1 at ell=3000):
The prior on the amplitude of the SZ (tSZ+kSZ) component (template) is D3000 = 5.5 +/ 3.0 uK^2.
The prior on the amplitude of the Poisson point source component (template) is D3000 = 19.3 +/ 3.5 uK^2.
The prior on the amplitude of the clustered point source component (template) is D3000 = 5.0 +/ 2.5 uK^2.
The foreground amplitudes are also required to be positive. The bandpowers, covariances and window functions are here in a gzipped tarball.
A text file with the bandpowers for plotting can be found here .
Each row is one ellbin. The columns are (1) ell_center (2) bandpower for 150x150, (3) bandpower uncertainty for 150x150. Each ell bin has the same width: 50.
If you have any questions regarding this data set or its use, please contact Ryan Keisler (rkeisler_at_uchicago_edu).


 Parameter Tables and Markov Chains 




As described in Keisler et al, the baseline model assumes a spatially flat, LCDM cosmological model. Neff is fixed to 3.046 in all models except for the LCDM+Neff models, in which case Neff is free. The primordial helium abundance is calculated using the PArthENoPE BBN code (Pisanti et al 2008) in all models except the LCDM+helium model, in which case Yp is free. In the LCDM+helium+Neff model, both Yp and Neff are free and independent of each other.
LCDM, SPT+WMAP7, parameters, chain
LCDM+A_L, SPT+WMAP7, parameters, chain
LCDM+tensors, SPT+WMAP7, parameters, chain
LCDM+running, SPT+WMAP7, parameters, chain
LCDM+helium, SPT+WMAP7, parameters, chain
LCDM+Neff, SPT+WMAP7, parameters, chain
LCDM+helium+Neff, SPT+WMAP7, parameters, chain
LCDM, SPT+WMAP7+H0+BAO, parameters, chain
LCDM+A_L, SPT+WMAP7+H0+BAO, parameters, chain
LCDM+tensors, SPT+WMAP7+H0+BAO, parameters, chain
LCDM+running, SPT+WMAP7+H0+BAO, parameters, chain
LCDM+helium, SPT+WMAP7+H0+BAO, parameters, chain
LCDM+Neff, SPT+WMAP7+H0+BAO, parameters, chain
LCDM+running, SPT+WMAP7+H0+BAO+Clusters, parameters, chain
LCDM+helium, SPT+WMAP7+H0+BAO+Clusters, parameters, chain
LCDM+Neff, SPT+WMAP7+H0+BAO+Clusters, parameters, chain
If you have any questions regarding this data set or its use, please contact Ryan Keisler (rkeisler_at_uchicago_edu).


 Likelihood Code 




We provide versions of certain cosmoMC + CAMB files that have been modified to interface with the CMB data presented in the SPT paper, "A Measurement of the Damping Tail of the Cosmic Microwave Background Power Spectrum with the South Pole Telescope", Keisler et al, 2011 ("K11"). The code will automatically marginalize over the three foreground components described in K11 and allow the user to explore constraints on the lensing amplitude, the primordial helium abundance, and the effective number of relativistic species.
This is not the exact likelihood code used in K11, but the differences in parameter constraints are not statistically significant. We provide only those cosmoMC/CAMB files that were modified. Please read the README before using.
README
Code
If you have any questions regarding this data set or its use, please contact Ryan Keisler (rkeisler_at_uchicago_edu).



