Erratum: Constraints on dark photon dark matter using data from LIGO’s and Virgo’s third observing run [Phys. Rev. D 105, 063030 (2022)]

An oversight in the analysis presented in the original article led to an overly optimistic estimate of the sensitivity of the cross-correlation search to a dark photon dark matter signal. Specifically, the overlap reduction function (ORF) used for the contribution of the finite light speed effect (“common-mode” mirror motion within either interferometer arm leading to an apparent differential strain) [1] was taken to be the same as the ORF for the true differential-mode mirror motion. As reported in [2], the ORF for the finite speed effect ( -0.18 ) is, instead, significantly smaller than that for true differential motion ( -0.9 ). Since the ORF values are squared in computing the coupling strength e2, the sensitivity reduction of the cross-correlation results depicted in Fig. 3 in the original article is substantial. Hence, we include here a revised Fig. 3 to supersede that in the original article. Because the relative importance of the finite speed contribution is larger at higher frequencies, the sensitivity degradation is greater at higher frequencies. The results from the BSD analysis, which does not rely upon cross-correlation, are unchanged from those shown in the original article and now provide more constraining upper limits on the coupling strength of dark matter to baryons across most of the frequency range. Following the same notations in the original article, the square root of the amplitude ratio of the cross-correlation for two signal channels in the frequency domain is given by. (Formula Presented).