The stellar kinematics in dwarf galaxies can provide a wealth of information about its underlying dark matter distribution. Using Gaia DR3 data, we examine the kinematics of the central core of the Sagittarius (Sgr) dwarf spheroidal galaxy using data which includes proper motions and line-of-sight velocities for member stars in addition to their projected positions. We extract a sample of bright stars that are high-probability members of Sgr. We obtain a velocity anisotropy of βa=−2.24±1.99, which implies a system with tangentially-biased orbits. Proper motions and complete position information could be used to break the existing velocity anisotropy and central density degeneracy; however without accurate distances to these stars, a 6D Jeans analysis cannot be performed. From Gaia only 5D data plus mock distances, we project that the data will significantly improve upon measurements of the log-slope of the dark matter density profile and the stellar velocity anisotropy. Tests with mock distance data show an improvement of anisotropy errors of approximately an order of magnitude, and log slope at the half light radius of approximately half an order of magnitude, indicating stronger future constraints on dark matter density profiles.
