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The Galactic bulge and bar are critical to our understanding of the MilkyWay. However, due to the lack of reliable stellar distances, the structure andkinematics of the bulge/bar beyond the Galactic center have remained largelyunexplored. Here, we present a method to measure distances of luminous redgiants using a period-amplitude-luminosity relation anchored to the LargeMagellanic Cloud, with random uncertainties of 10-15% and systematic errorsbelow 1-2%. We apply this method to data from the Optical Gravitational LensingExperiment (OGLE) to measure distances to $190,302$ stars in the Galactic bulgeand beyond out to 20 kpc. Using this sample we measure a distance to theGalactic center of $R_0$ = $8108\pm106_{\rm stat}\pm93_{\rm sys}$ pc,consistent with astrometric monitoring of stars orbiting Sgr A*. We cross-matchour distance catalog with Gaia DR3 and use the subset of $39,566$ overlappingstars to provide the first constraints on the Milky Way's velocity field($V_R,V_\phi,V_z$) beyond the Galactic center. We show that the $V_R$quadrupole from the bar's near side is reflected with respect to the Galacticcenter, indicating that the bar is both bi-symmetric and aligned with the innerdisk, and therefore dynamically settled along its full extent. We also findthat the vertical height $V_Z$ map has no major structure in the region of theGalactic bulge, which is inconsistent with a current episode of bar buckling.Finally, we demonstrate with N-body simulations that distance uncertainty playsa major factor in the alignment of the major and kinematic axes of the bar anddistribution of velocities, necessitating caution when interpreting results fordistant stars.

The far side of the Galactic bar/bulge revealed through semi-regular variables