  The center of the Milky Way hosts the closest supermassive black hole,
SgrA$^*$. Decades of near-infrared observations of our Galactic Center have
shown the presence of a small population of stars (the so called S-star
cluster) orbiting SgrA$^*$, which were recently reported to be arranged in two
orthogonal disks. In this case, the timescale for Lense-Thirring precession of
S-stars should be longer than their age, implying a low spin for SgrA$^*$. In
contrast, the recent results by the Event Horizon Telescope favor a
highly-spinning SgrA$^*$, which seem to suggest that the S-stars could not be
arranged in disks. Alternatively, the spin of SgrA$^*$ must be small,
suggesting that the models for its observed image are incomplete.
