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This Letter presents a study of the geometry and motion of the Galactic diskusing open clusters in the Gaia era. The findings suggest that the inclinationof the Galactic disk increases gradually from the inner to the outer disk, witha shift in orientation at the Galactocentric radius of approximately 5 to 7kpc. Furthermore, this study brings forth the revelation that the mid-plane ofthe Milky Way may not possess a stationary or fixed position. A plausibleexplanation is that the inclined orbits of celestial bodies within our Galaxyexhibit a consistent pattern of elliptical shapes, deviating from perfectcircularity; however, more observations are needed to confirm this. An analysisof the vertical motion along the Galactocentric radius reveals that the diskhas warped with precession, and that the line-of-nodes shifts at differentradii, aligning with the results from the classical Cepheids. Although there isuncertainty for precession/peculiar motion in Solar orbit, after consideringthe uncertainty, the study derives a median value of precession rate = 6.8km/s/kpc in the Galaxy. This value for the derived precession in the outer diskis lower than those in the literature due to the systematic motion in Solarorbit (inclination angle = 0.6 deg). The study also finds that theinclinational variation of the disk is significant and can cause systematicmotion, with the inclinational variation rate decreasing along the Galacticradius with a slope of -8.9 uas/yr/kpc. Moreover, the derived inclinationalvariation rate in Solar orbit is 59.1+-11.2(sample)+-7.7(VZsun) uas/yr, whichmakes it observable for high precision astrometry. The all-sky open clustercatalog based on Gaia DR3 and Galactic precession/inclinational variation fitsas well as Python code related to these fits are available athttps://nadc.china-vo.org/res/r101288/

Geometry and Kinematics of a Dancing Milky Way: Unveiling the Precession and Inclination Variation across the Galactic Plane via Open Clusters