  We study the Satellite Plane Problem of the Milky Way\ (MW) by using the
recently published simulation data of TNG50-1. Here, we only consider the
satellite plane consisting of the brightest 14 MW satellites \ (11 classical
satellites plus Canes Venatici I\ (CVn I), Crater II and Antlia II). One halo\
(haloID=395, at z=0, hereafter halo395 ) of 231 MW like candidates, possesses a
satellite plane as spatially thin and kinematically coherent as the observed
one has been found. Halo395 resembles the MW in a number of intriguing ways: it
hosts a spiral central galaxy and its satellite plane is almost ($\sim
87^{\circ}$)perpendicular to the central stellar disk. In addition, halo395 is
embedded in a sheet plane, with a void on the top and bottom, similar to the
local environment of MW. More interestingly, we found that the 11 of 14 of the
satellites on the plane of halo395, arise precisely from the peculiar geometry
of its large-scale environment\ (e.g. sheet and voids). The remaining three
members appeared at the right place with the right velocity by chance at z=0.
Our results support previous studies wherein the Satellite Plane Problem is not
seen as a serious challenge to the $\Lambda$CDM model and its formation is
ascribed to the peculiarities of our environment.
