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We present a study of the influence of the Gaia-Sausage-Enceladus (GSE) onthe density shape of the Galactic stellar halo using 11624 K giants from theLAMOST survey. Every star is assigned a probability of being a member of theGSE based on its spherical velocities and metallicity by a Gaussian MixtureModel. We divide the stellar halo into two parts by the obtained probabilities,of which one is composed of the GSE members and defined as the GSE-relatedhalo, and the other one is referred to as the GSE-removed halo. Using anon-parametric method, the radial number density profiles of the two stellarhalos can be well described by a single power law with a variable flattening$q$ ($r = \sqrt{R^2+[(Z/q(r))]^2}, \nu = {\nu_0}r^{-\alpha}$). The index$\alpha$ is $4.92\pm0.12$ for the GSE-related halo and $4.25\pm0.14$ for theGSE-removed halo. Both the two stellar halos are vertically flattened atsmaller radii but become more spherical at larger radii. We find that theGSE-related halo is less vertically flattened than the GSE-removed halo, andthe difference of $q$ between the two stellar halos ranges from 0.07 to 0.15.However, after the consideration of the bias, it is thought to be within 0.08at most of the radii. Finally, we compare our results with two Milky Wayanalogues which experience a significant major merger in the TNG50 simulation.The study of the two analogues also shows that the major merger-related stellarhalo has a smaller ellipticity than the major merger-removed stellar halo.

Influence of the Gaia-Sausage-Enceladus on the density shape of the Galactic stellar halo revealed by halo K giants from the LAMOST survey