### Abstract:

In the analysis published in 1, constraints on the number of signal events \(n_s\) can be interpreted as constraints on the volumetric neutrino to muon conversion rate \(\Lambda_{\nu\overline{\nu}\to\mu^{+}\mu{-}}\), \(\Lambda_{\nu\overline{\nu}\to\mu^{+}\mu{-}}^{90\%C.L.}\) = \(\frac{n_s^{90\%C.L.}}{\Sigma_jT_{live}^jV_{eff}^j}\), where \(T_{live}\) and \(V_{eff}\) are the livetime and effective volume of the data sample of index \(j\). These can then be interpreted as constraints on the muon flux \(\phi_{\mu^++\mu^-}\), dark matter (DM) annihilation rate in the Sun \(\Gamma_{\chi\chi\to SM}\), as well as the spindependent (SD) and spin-independent (SI) scattering cross sections \(\sigma_{SD}\) and \(\sigma_{SI}\) using WimpSim [2]. In Table 4 of Ref. [1], the labels and units of columns 7 and 8 suggest that the muon flux \(\phi_{\mu^++\mu^-}\) (in units km⁻² year⁻¹) is being presented. However for the first 12 rows, corresponding to points in which the DeepCore (DC) dataset was included, the volumetric neutrino to muon conversion rate \(\Lambda_{\nu\overline{\nu}\to\mu^{+}\mu{-}}\) (in units km⁻³ year⁻¹) were erroneously reported instead. The corrected table (Table 1) is presented hereby. All other columns remain unchanged. All quantities that go into the right hand side of Eq. 1 are presented in the table, as well as median sensitivities and 90% C.L. upper limits on themuon flux \(\phi_{\mu^++\mu^-}\) derived usingWimpSim[2]. The final results and conclusions presented in Ref. [1] in terms of constraints on theSDand SI scattering cross sections \(\sigma_{SD}\) and \(\sigma_{SI}\) as well as the DM annihilation rate in the Sun \(\Gamma_{\chi\chi\to SM}\), remain unchanged. In Section 4.2 of Ref. [1], themaximum zenith angle of the Sun is erroneously mentioned as 104°. The correct maximum zenith angle of the Sun is 114° at the South Pole.