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We present results from an analysis of all data taken by the BICEP2/Keck CMBpolarization experiments up to and including the 2015 observing season. Thisincludes the first Keck Array observations at 220 GHz and additionalobservations at 95 & 150 GHz. The $Q/U$ maps reach depths of 5.2, 2.9 and 26$\mu$K$_{cmb}$ arcmin at 95, 150 and 220 GHz respectively over an effectivearea of $\approx 400$ square degrees. The 220 GHz maps achieve asignal-to-noise on polarized dust emission approximately equal to that ofPlanck at 353 GHz. We take auto- and cross-spectra between these maps andpublicly available WMAP and Planck maps at frequencies from 23 to 353 GHz. Weevaluate the joint likelihood of the spectra versus a multicomponent model oflensed-$\Lambda$CDM+$r$+dust+synchrotron+noise. The foreground model has sevenparameters, and we impose priors on some of these using external informationfrom Planck and WMAP derived from larger regions of sky. The model is shown tobe an adequate description of the data at the current noise levels. Thelikelihood analysis yields the constraint $r_{0.05}<0.07$ at 95% confidence,which tightens to $r_{0.05}<0.06$ in conjunction with Planck temperaturemeasurements and other data. The lensing signal is detected at $8.8 \sigma$significance. Running maximum likelihood search on simulations we obtainunbiased results and find that $\sigma(r)=0.020$. These are the strongestconstraints to date on primordial gravitational waves.

BICEP2 / Keck Array x: Constraints on Primordial Gravitational Waves using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season