South Pole Telescope (SPT)

Spectra 2009 Data

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Point-source-subtracted 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. These files use the CosmoMC extension produced by the QUaD collaboration. 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 and 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 is also provided. Each row is one ell-bin. The columns are (1) ell_lower, (2) ell_upper, (3) ell_effective, (4) bandpower, and (5) bandpower uncertainty.

Single-frequency bandpowers are calculated for 150x150, 150x220 and 220x220 spectra. The CosmoMC data files are here in a gzipped tarball. These files use the CosmoMC extension produced by the QUaD collaboration which is available here. A text file with the bandpowers is also provided. 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.

Additional Details:

  • "Lueker et al. 2010, "Measurements of Secondary Cosmic Microwave Background Anisotropies with the South Pole Telescope", arXiv:0912.4317v1, ADS.

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Goddard Space Flight Center, National Aeronautics and Space Administration
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LAMBDA Director: Dr. Thomas M. Essinger-Hileman
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