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tokens: [Fe/H] ∼ −1.6 and an outer halo of [Fe/H] ∼ −2.2 (Carollo et al. 2007 ). Although both components are expected to have contributions from accreted stars, it is the outer halo that is dominated by accreted stars (Tissera, White Scannapieco 2012 ). In the suite of eight MW-like model galaxies in the simulation by Tissera et al. ( 2012 ) the stars accreted from satellites have ages between 9.8 and 12.6 Gyr and metallicities of −1.45 [Fe/H] −0.86. Such ages and metallicities are consistent with the initial epoch of star formation and metallicity upper limits for the five disrupted satellites in our work (see Table 2 ). Using MW-like model galaxies based on the Evolution and Assembly of GaLaxies and their Environments (EAGLE) simulations by Mackereth et al. ( 2019 ) concluded that the MW’s assembly history was dominated by the accretion of a small number of satellites of stellar mass 10 8.5−9 M ⊙ , in reasonable agreement with our findings (see Table 2 ). 7.1 The Kraken/Koala satellite K19 describe their simulation of 25 galaxies with MW-like masses within the EAGLE galaxy formation model (Crain et al. 2015 ). Their suite of MW-like model galaxies undergoes an average of 4.4 ± 2.3 minor mergers. with mass ratios of 1:100 up to 1:4. This corresponds to satellite masses of 10 8−9 M ⊙ at the time of infall. They suggest that the vast bulk of the accreted GCs come from two nearly equal mass (∼10 9 M ⊙ ) satellites that merged in the last 10 Gyr. A third lower mass (∼10 8 M ⊙ ) satellite brings in a handful of GCs. Additional accreted satellites are of very low mass, containing few, if any, GCs. They associated the low-mass satellite with the Sgr dwarf galaxy and one of the massive satellites with the Canis Major dwarf galaxy (here called Gaia -Enceladus). The remaining, and perhaps most massive satellite, was not associated with any known feature of the MW by K19 but instead was given the name Kraken . They suggested the Kraken had a stellar mass of 2 × 10 9 M ⊙ and was accreted 6–9 Gyr ago. Although K19 do not associate any particular MW GC with the Kraken, they do list 18 GCs with the potential to be from the disrupted Kraken satellite. Here we have assigned those 18 GCs across the Gaia -Enceladus, Sequoia, Koala, Helmi satellites, and the high-energy group. So, while we do suggest that the MW accreted an additional satellite of mass M * ∼ 10 9 M ⊙ (i.e. Koala), we make different GC assignments to K19 . In their terminology, satellite 3 is the Sgr dwarf, satellite 2 is Gaia -Enceladus/Canis Major, and satellite 1 could be the Koala galaxy with ω Cen as its former nucleus. Our analysis indicates that the MW has accreted five satellites of mass 10 8−9 M ⊙ consistent with K19 . Overall, K19 concluded that the MW formed quite rapidly with no major mergers since z = 4 (i.e. the last 12.3 Gyr). This makes it somewhat atypical compared to their suite of 25 MW-like models. 8 CONCLUSIONS Using the IOM, the AMRs, and alpha-element ratios of MW GCs we