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T, Q, and U maps Figure 1: Planck 353 GHz T, Q, and U maps before (left) and after (right) the application of BICEP2/Keck filtering. In both cases the maps have been multiplied by the BICEP2/Keck apodization mask. The Planck maps are presmoothed to the BICEP2/Keck beam profile and have the mean value subtracted. The filtering, in particular the third order polynominal subtraction to suppress atmospheric pickup, removes large-angular scale signal along the BICEP2/Keck scanning direction (parallel to the right ascension direction in the maps here). PDF / PNG
Spectra between BICEP2/Keck maps at 150 GHz and Planck maps at 353 GHz Figure 2: Single- and cross-frequency spectra between BICEP2/Keck maps at 150 GHz and Planck maps at 353 GHz. The red curves show the lensed-ΛCDM expectations. The left column shows single-frequency spectra of the BICEP2, Keck Array, and combined BICEP2/Keck maps. The BICEP2 spectra are identical to those in BK-I, while the Keck Array and combined are as given in BK-V. The center column shows cross-frequency spectra between BICEP2/Keck maps and Planck 353 GHz maps. The right column shows Planck 353 GHz data-split cross-spectra. In all cases the error bars are the standard deviations of lensed-ΛCDM+noise simulations and hence contain no sample variance on any other component. For EE and BB the χ2 and χ (sum of deviations) versus lensed-ΛCDM for the nine bandpowers shown is marked at upper and lower left (for the combined BICEP2/Keck points and DS1×DS2, respectively). In the bottom row (for BB) the center and right panels have a scaling applied such that signal from dust with the fiducial frequency spectrum would produce signal with the same apparent amplitude as in the 150 GHz panel on the left (as indicated by the right-side y-axes). We see from the significant excess apparent in the bottom center panel that a substantial amount of the signal detected at 150 GHz by BICEP2 and Keck Array indeed appears to be due to dust. PDF / PNG
EE and BB cross-spectra Figure 3: EE (left column) and BB (right column) cross-spectra between BICEP2/Keck maps and all of the polarized frequencies of Planck. In all cases the quantity plotted is ℓ(ℓ+1)C/2π in units of μKCMB2, and the red curves show the lensed-ΛCDM expectations. The error bars are the standard deviations of lensed-ΛCDM+noise simulations and hence contain no sample variance on any other component. Also note that the y-axis scales differ from panel to panel in the right column. The χ2 and χ (sum of deviations) versus lensed-ΛCDM for the five bandpowers shown is marked at upper left. There are no additional strong detections of deviation from lensed-ΛCDM over those already shown in Figure 2 although BK150×P217 shows some evidence of excess. PDF / PNG
Differences between BICEP2 and Keck Array cross-spectra with Planck Figure 4: Differences of B150×P353 and K150×P353 BB cross-spectra. The error bars are the standard deviations of the pairwise differences of signal+noise simulations that share common input skies. The probability to exceed the observed values of χ2 and χ statistics, as evaluated against the simulations, is quoted for bandpower ranges 1–5 (20<ℓ<200) and 1–9 (20<ℓ<330). There is no evidence that these spectra are statistically incompatible. PDF / PNG
Differences between the standard power spectrum estimator and alternate estimators Figure 5: Differences of B150×P353 BB cross-spectra from the standard power spectrum estimator and alternate estimators. The error bars are the standard deviations of the pairwise differences of signal+noise simulations that share common input skies. The probability to exceed the observed values of χ2 and χ statistics, as evaluated against simulations, is quoted for bandpower ranges 1–5 (20<ℓ<200) and 1–9 (20<ℓ<330). We see that the differences of the real spectra are consistent with the differences of the simulations. PDF / PNG
Likelihood results from a lensed-ΛCDM+r+dust model Figure 6: Likelihood results from a basic lensed-ΛCDM+r+dust model, fitting BB auto- and cross-spectra taken between maps at 150 GHz, 217, and 353 GHz. The 217 and 353 GHz maps come from Planck. The primary results (heavy black) use the 150 GHz combined maps from BICEP2/Keck. Alternate curves (light blue and red) show how the results vary when the BICEP2 and Keck Array only maps are used. In all cases a Gaussian prior is placed on the dust frequency spectrum parameter βd = 1.59±0.11. In the right panel the two dimensional contours enclose 68% and 95% of the total likelihood. PDF / PNG
Likelihood results when varying the data sets and model priors Figure 7: Likelihood results when varying the data sets used and the model priors. PDF / PNG
Likelihood results including synchrotron Figure 8: Likelihood results for a fit when adding the lower frequency bands of Planck, and extending the model to include a synchrotron component. The results for two different assumed degrees of correlation between the dust and synchrotron sky patterns are compared to those for the comparable model without synchrotron. PDF / PNG
Likelihood results allowing AL to vary Figure 9: Likelihood results for a fit allowing the lensing scale factor AL to float freely and using all nine bandpowers. Marginalizing over r and Ad, we find that AL=1.13±0.18 and AL=0 is ruled out with 7.0 σ significance. PDF / PNG
Likelihood results from simulations Figure 10: Likelihoods for r and Ad, using BICEP2/Keck and Planck, as plotted in Figure 6, overplotted on constraints obtained from realizations of a lensed-ΛCDM+noise+dust model with dust power similar to that favored by the real data (Ad=3.6 μK2). Half of the r curves peak at zero as expected. PDF / PNG
Likelihood results from Planck Sky Model simulations Figure 11: Constraints obtained when adding dust realizations from the Planck Sky Model version 1.7.8 to the base lensed-ΛCDM+noise simulations. (Curves for 139 regions with peak Ad<20 μK2 are plotted.) We see that the results for r are unbiased in the presence of dust realizations which do not necessarily follow the ℓ-0.42 power law or have Gaussian fluctuations about it. PDF / PNG
BB spectrum before and after dust subtraction and Constraint on r from cleaned spectrum Figure 12: Upper: BB spectrum of the BICEP2/Keck maps before and after subtraction of the dust contribution, estimated from the cross-spectrum with Planck 353 GHz. The error bars are the standard deviations of simulations, which, in the latter case, have been scaled and combined in the same way. The inner error bars are from lensed-ΛCDM+noise simulations as in the previous plots, while the outer error bars are from the lensed-ΛCDM+noise+dust simulations. The red curve shows the lensed-ΛCDM expectation. Lower: Constraint on r derived from the cleaned spectrum compared to the fiducial analysis shown in Figure 6. PDF / PNG
Expectation values and uncertainties for BB in the BICEP2/Keck field Figure 13: Expectation values, and uncertainties thereon, for the ℓ~80 BB bandpower in the BICEP2/Keck field. The green and magenta lines correspond to the expected signal power of lensed-ΛCDM and r=0.05. Since CMB units are used, the levels corresponding to these are flat with frequency. The grey band shows the best fit dust model and the blue shaded region shows the allowed region for synchrotron. The BICEP2/Keck noise uncertainty is shown as a single starred point, and the noise uncertainties of the Planck single-frequency spectra evaluated in the BICEP2/Keck field are shown in red. The blue points show the noise uncertainty of the cross-spectra taken between BICEP2/Keck and, from left to right, Planck 30, 44, 70, 100, 143, 217 and 353 GHz, and plotted at horizontal positions such that they can be compared vertically with the dust and sync curves. PDF / PNG

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