Graphics: Power SpectraExperimentagnostic graphics suitable for use in scientific presentations and papers, but not in cosmological calculations, are provided here. Note that some values are truncated or rounded in the plots and in accompanying data tables. Please acknowledge LAMBDA when using these images. Observed Bmode Polarization: DetectionsObserved Bmode power from CMB experiments with significant detections and 95% confidence upper limits from other selected experiments. Detections from BICEP2+Keck October 2018, BICEP2+Keck/Planck January 2015, POLARBEAR, and SPTpol are included; click here for more information regarding data sources. The BICEP2+Keck data points show the CMB component from a decomposition of the BB spectrum into CMB, dust, and synchrotron components. The BICEP2+Keck/Planck data points show results with dust foreground subtraction based on measured crosspower between Planck and BICEP2+Keck. The other points show results without any foreground subtraction. For comparison, a theoretical curve is shown for a ΛCDM model with tensortoscalar ratio r=0.1. The gravitational lensing component is shown as a dotted curve and the inflationary component including the reionization bump at l < 10 is shown as a dashed curve. Observed Bmode Polarization: Bounds95% confidence upper limits for Bmode power from different CMB experiments. Data from ABS, ACTPol, BICEP1, BOOMERanG, CAPMAP, CBI, DASI, MAXIPOL, Planck, POLARBEAR, QUaD, QUIETQ, QUIETW, and WMAP are included; click here for more information regarding data sources. For comparison, theoretical curves are shown for a ΛCDM model with tensortoscalar ratio r=0.1 and r=0.01. The gravitational lensing component is shown as a dotted curve and inflationary components including the reionization bump at l < 10 are shown as dashed curves. Observed Gravitational Lensing Power SpectrumRecent measurements from CMB experiments of gravitational lensing due to the largescale distribution of matter in the universe. The plots show the power spectrum of the gravitational lensing potential on a linear scale (Top) and a logarithmic scale (Bottom). Data from ACT, ACTPol, BICEP2/Keck, Planck, POLARBEAR, SPT, and SPTPol are included; click here for more information regarding data sources. The black curve shows the theoretical lensing power spectrum for the bestfit LCDM parameters obtained from the Planck 2018 temperature and polarization data. CMBonly TT Power SpectrumThe plot shows CMB lensed bandpowers from recent ACTPol, Planck, and SPT measurements marginalized over Galactic and extragalactic foreground emission and SunyaevZel'dovich effects. Click here for more information regarding data sources. For comparison, a theoretical curve is shown that was calculated by the LAMBDA group using parameters of the Planck team 2015 bestfit PlanckTT+lowP ΛCDM model. CMB TE and EE Power SpectraCMB TE and EE bandpowers marginalized over foreground emission from recent experiments. Click here for more information regarding data sources. For comparison, theoretical curves are shown from the Planck 2018 best fit TT, EE, EE+lowE+lensing ΛCDM model for l < 2500 and from a calculation by the LAMBDA group for the Planck team 2015 bestfit PlanckTT+lowP ΛCDM model for higher l. Image Credit: NASA / LAMBDA Archive Team
Image Credit: NASA / LAMBDA Archive Team
