We present a spectroscopic and imaging analysis of the z₆₀₋ 1. 1334 ultra-strong MgII absorption system identified in the VLT/UVES spectrum of a background quasar located at ρ 18 kpc from a star-forming galaxy. Low ionization metal lines like MgI, FeII, and CaII are also detected for this absorber. The HI lines are outside of the wavelength coverage. The MgII has a rest-frame equivalent width of Wᵣ (2796) =3. 185 +/- 0. 032 A^, with the absorption spread across Δv 460 km~s^-1 in several components. A component-by-component ionization modeling shows several of these components having solar and higher metallicities. The models also predict a total HI column density of logN (HI) /cm^-2 22. 5, consistent with ultra-strong MgII absorbers being sub-Damped Lyman Alpha and Damped Lyman Alpha systems. The absorber is well within the virial radius of the nearest galaxy which has a stellar mass M_* = 4. 7 10^10~M_, and a star formation rate of 8. 3~M_~yr^-1. The absorption is along the projected major axis of the galaxy with a velocity spread that is wider than the galaxy's disk rotation. From the kinematic analysis of the absorber and the galaxy, the origin of the absorption can be attributed to a combination of circumgalactic gas structures, some corotating with the disk and the rest at line-of-sight velocities outside of the disk rotation.
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