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An excess of $\sim$10-20 GeV cosmic-ray antiprotons has been identified inthe spectrum reported by the AMS-02 Collaboration. The systematic uncertaintiesassociated with this signal, however, have made it difficult to interpret theseresults. In this paper, we revisit the uncertainties associated with the time,charge and energy-dependent effects of solar modulation, the antiprotonproduction cross section, and interstellar cosmic-ray propagation. Afteraccounting for these uncertainties, we confirm the presence of a 4.7$\sigma$antiproton excess, consistent with that arising from a $m_{\chi} \approx 64-88$GeV dark matter particle annihilating to $b\bar{b}$ with a cross section of$\sigma v \simeq (0.8-5.2) \times 10^{-26}$ cm$^{3}$/s. If we allow for thestochastic acceleration of secondary antiprotons in supernova remnants, thedata continues to favor a similar range of dark matter models ($m_{\chi}\approx46-94$ GeV, $\sigma v \approx (0.7-3.8)\times 10^{-26}$ cm$^3/$s) with asignificance of 3.3$\sigma$. The same range of dark matter models that arefavored to explain the antiproton excess can also accommodate the excess ofGeV-scale gamma rays observed from the Galactic Center.

A Robust Excess in the Cosmic-Ray Antiproton Spectrum: Implications for Annihilating Dark Matter