Search for annihilating dark matter in the Sun with 3 years of IceCube data (vol 77, pg 146, 2017)

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.