  The Galactic bulge and bar are critical to our understanding of the Milky
Way. However, due to the lack of reliable stellar distances, the structure and
kinematics of the bulge/bar beyond the Galactic center have remained largely
unexplored. Here, we present a method to measure distances of luminous red
giants using a period-amplitude-luminosity relation anchored to the Large
Magellanic Cloud, with random uncertainties of 10-15% and systematic errors
below 1-2%. We apply this method to data from the Optical Gravitational Lensing
Experiment (OGLE) to measure distances to $190,302$ stars in the Galactic bulge
and beyond out to 20 kpc. Using this sample we measure a distance to the
Galactic center of $R_0$ = $8108\pm106_{\rm stat}\pm93_{\rm sys}$ pc,
consistent with astrometric monitoring of stars orbiting Sgr A*. We cross-match
our distance catalog with Gaia DR3 and use the subset of $39,566$ overlapping
stars 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 Galactic
center, indicating that the bar is both bi-symmetric and aligned with the inner
disk, and therefore dynamically settled along its full extent. We also find
that the vertical height $V_Z$ map has no major structure in the region of the
Galactic bulge, which is inconsistent with a current episode of bar buckling.
Finally, we demonstrate with N-body simulations that distance uncertainty plays
a major factor in the alignment of the major and kinematic axes of the bar and
distribution of velocities, necessitating caution when interpreting results for
distant stars.
