ABOUT LAMBDA

TE and EE Power Spectrum Plot Data Sources

Here is a text file containing the data points used to generate the TE plot.

Here is a text file containing the data points used to generate the EE plot.


ACTPol

  • The Atacama Cosmology Telescope: A Measurement of the Cosmic Microwave Background Power Spectra
    at 98 and 150 GHz, Choi et al. 2020, ADS
  • CMB only spectra
    CMB-only bandpowers, marginalized over astrophysical foregrounds. These spectra are released
    for plotting purposes and do not include the full covariance.

BICEP2+Keck

  • BICEP2/Keck Array VI: Improved Constraints On Cosmology and Foregrounds When Adding 95 GHz Data From Keck
    Array, Ade et.al. 2015, astro-ph

    BK_bandpowers_sample_20150129.txt
    The plotted bandpower error bars include statistical uncertainty and sample variance.

Planck

  • Planck 2018 results. VI. Cosmological parameters, Planck Collaboration, astro-ph

    Unbinned measurements available from the Planck Legacy archive are plotted at l < 30,
    and binned measurements provided to LAMBDA by the Planck team are plotted at higher l.

    The EE measurements at l > 1500 are not included in the plot because their uncertainties are large.

POLARBEAR

  • A measurement of the CMB E-mode angular power spectrum at subdegree scales from 670 square degrees of POLARBEAR data,
    Adachi et al. 2020, ADS

    The plotted bandpowers and uncertainties are from Table 1.

SPTpol

  • Measurements of the Temperature and E-Mode Polarization of the CMB from 500 Square Degrees of SPTpol Data,
    Henning, J. W., et al., 2017, astro-ph

    bandpowers_sptpol_500deg2_TTEETE.txt

    The plotted bandpower error bars include sample and noise variance, and do not include calibration or beam uncertainty.

SPT-3G

  • Measurements of the E-Mode Polarization and Temperature-E-Mode Correlation of the CMB from SPT-3G 2018 Data, Dutcher, D., et al., 2021, ADS

    The plotted bandpowers and uncertainties are from Table IV. The uncertainties are the square root of the diagonal elements of the covariance matrix and do not include beam or calibration uncertainties.

WMAP

  • Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Final Maps and Results
    Bennett, C.L., et.al., 2013, ApJS., 208, 20B
    ADS / astro-ph

  • Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmology Results
    Hinshaw, G.F., et.al., 2013, ApJS., 208, 19H
    ADS / astro-ph

    wmap_binned_te_spectrum_9yr_v5.txt
    wmap_binned_ee_spectrum_9yr_v5.txt

    TE measurements for l > 600 and EE measurements for l > 200 are not included in the plots because their uncertainties are large.

A service of the HEASARC and of the Astrophysics Science Division at NASA/GSFC
Goddard Space Flight Center, National Aeronautics and Space Administration
HEASARC Director: Dr. Alan P. Smale
LAMBDA Director: Dr. Eric R. Switzer
NASA Official: Dr. Eric R. Switzer
Web Curator: Mr. Michael R. Greason