The SPT 150 GHz bandpowers, WMAP7 bandpowers, ACBAR bandpowers, QUaD bandpowers, and ACT 150 GHz bandpowers plotted against the best-fit lensed LCDM CMB spectrum. The damping tail of the primary CMB anisotropy is apparent below ell = 3000. Above ell = 3000, there is a clear excess due to secondary anisotropies and residual point sources that has now been measured by both SPT and ACT. Note that the source masking threshold in the SPT data (6.4 mJy) is lower than that in the ACT data so we expect less radio source power on small angular scales. We have multiplied the SPT bandpowers by the best-fit calibration of 0.92 as determined in parameter fits. (This is Figure 4 in Shirokoff et al. 2010.)

Top panel: From left to right, the SPT 150 GHz, 150 x 220 GHz and 220 GHz bandpowers. Overplotted is the best-fit model line (red line) with components shown individually. The lensed primary CMB anisotropy is marked by an orange line. The best-fit tSZ (purple line) and predicted kSZ (purple dashed line) power spectra are also shown. The predicted radio source term is represented by the blue dots. The DSFG Poisson term at each frequency is denoted by the green dashedline and the clustered DSFG component by the green dot-dash line. The damping tail of the primary CMB anisotropy is apparent below ell = 3000. Above ell = 3000, there is a clear excess with an angular dependence consistent with point sources. These sources have low flux (as sources detected at >5 sigma in either band have been masked) and a rising frequency spectrum, consistent with expectations for Poisson distributed DSFGs. Bottom panel: Plot of the residual between the measured bandpowers and best-fit spectrum. (This is Figure 3 in Shirokoff et al. 2010.)

These bandpowers are calculated for 150x150, 150x220 and 220x220 spectra.

The bandpowers, covariances, window functions and beam error files are here in a gzipped tarball.

A text file with the bandpowers for plotting can be found here .
Each row is one ell-bin. The columns are (1) ell_lower, (2) ell_upper, (3) ell_effective, (4) bandpower for 150x150, (5) bandpower uncertainty for 150x150, (6) bandpower for 150x220, (7) bandpower uncertainty for 150x220, (8) bandpower for 220x220, and (9) bandpower uncertainty for 220x220.

If you have any questions regarding this data set or its use please contact Erik Shirokoff (shiro_at_bolo.berkeley.edu).

These bandpowers are calculated for a linear combination of the 150 and 220 GHz maps (map150 - 0.325 * map220) designed to remove foreground emission from dusty star-forming galaxies.

The CosmoMC data files are here in a gzipped tarball.
The contents of the tarball consist of .newdat file and directory with window functions in text format. Spectrum_dsfg.newdat has bandpowers, uncertainties, and beam & calibration uncertainties. The window functions can be found in window_spt/window_XX, where XX is the bin number. In the window function files, the first column is ell and the second column is W_ell/ell.

A text file with the bandpowers for plotting can be found here .
Each row is one ell-bin. The columns are (1) ell_lower, (2) ell_upper, (3) ell_effective, (4) bandpower, and (5) bandpower uncertainty.

The code modules and instructions for incorporating the modules into the May 2010 version of cosmomc are here in a gzipped tarball.