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Slow stellar halo rotation as a signature of disc flips and GES-like mergers
The stellar halo of the Milky Way (MW) exhibits a weak net prograde rotational signal ($v_ϕ \lesssim 25$ km~s$^{-1}$), yet its origin remains unexplained. To investigate this, we use the Auriga cosmological simulation suite of MW-mass haloes to probe the rotation of stellar haloes over the redshift
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