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We present results from an analysis of all data taken by the BICEP2, KeckArray and BICEP3 CMB polarization experiments up to and including the 2018observing season. We add additional Keck Array observations at 220 GHz andBICEP3 observations at 95 GHz to the previous 95/150/220 GHz data set. The$Q/U$ maps now reach depths of 2.8, 2.8 and 8.8 $\mu{\mathrm K}_{cmb}$ arcminat 95, 150 and 220 GHz respectively over an effective area of $\approx 600$square degrees at 95 GHz and $\approx 400$ square degrees at 150 & 220 GHz. The220 GHz maps now achieve a signal-to-noise on polarized dust emission exceedingthat of Planck at 353 GHz. We take auto- and cross-spectra between these mapsand publicly available WMAP and Planck maps at frequencies from 23 to 353 GHzand evaluate the joint likelihood of the spectra versus a multicomponent modelof lensed-$\Lambda$CDM+$r$+dust+synchrotron+noise. The foreground model hasseven parameters, and no longer requires a prior on the frequency spectralindex of the dust emission taken from measurements on other regions of the sky.This model is an adequate description of the data at the current noise levels.The likelihood analysis yields the constraint $r_{0.05}<0.036$ at 95%confidence. Running maximum likelihood search on simulations we obtain unbiasedresults and find that $\sigma(r)=0.009$. These are the strongest constraints todate on primordial gravitational waves.

physical review letters

BICEP / Keck XIII: Improved Constraints on Primordial Gravitational  Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018  Observing Season