Detection of $B$-Mode Polarization at Degree Angular Scales by BICEP2

The BICEP2 collaboration Ade, P.A.R. ; Aikin, R.W. ; Barkats, D. ; et al.
Phys.Rev.Lett. 112 (2014) 241101, 2014.
Inspire Record 1286113 DOI 10.17182/hepdata.62706
2 data tables

BICEP2 TT, TE, EE, BB, TB, and EB bandpowers, ell*(ell+1)*C(ell)/(2*PI), and uncertainties, corresponding to Figure 2. Uncertainties are statistical only, the standard deviation of the constrained lensed-LambdaCDM+noise simulations, and are calculated as the square root of diagonal elements of the bandpower covariance matrix. The nature of the simulations constrains T to match the observed sky, thus TT, TE, and TB uncertainties do not include appropriate sample variance, and sample variance for a tensor BB signal is not included either. The calibration procedure uses TB and EB to constrain the polarization angle, thus TB and EB cannot be used to measure astrophysical polarization rotation.

Likelihood for the tensor-to-scalar ratio, r, derived from the BICEP2 BB spectrum, corresponding to the black curve from the middle panel of Figure 10, and calculated via the "direct likelihood" method described in Section 11.1.