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We present the Voigt profile (VP) models, column densities, Doppler bparameters, kinematics, and distribution of components for 422 MgII absorbersfound in a survey of 249 HIRES and UVES quasar spectra. The equivalent widthrange of the sample is 0.006 < W_r(2796) < 6.23 angstroms (A) and the redshiftrange is 0.19 < z < 2.55, with a mean of <z> = 1.18. Based on historicalprecedent, we classified 180 absorbers as weak systems (W_r(2796) < 0.3 A) and242 as strong systems (W_r(2796) >= 0.3 A). Assuming a minimum number ofsignificant components per system, the VP fitting, yielded a total of 2,989components, with an average of 2.7 and 10.3 components found for the weak andstrong MgII subsamples, respectively. The VP component line density for thefull sample is 8.62 +/- 0.23 clouds/A. The distribution of VP component columndensity over the range 12.4 < log[N(MgII)] < 17.0 [ions cm^-2] is well modeledwith a power-law slope of -1.45 +/- 0.01. The median Doppler b parameters are4.5 +/- 3.5 km/s, 6.0 +/- 4.5 km/s and 5.7 +/- 4.4 km/s for the weak, strong,and full samples. We modeled the probability of component velocity splitting(the two-point velocity correlation function, TPCF) of our full sample using athree-component composite Gaussian function. Our resulting velocity dispersionsare 25.4, 68.7, and 207.1 km/s, respectively. These data provide an excellentdatabase for studying the cosmic evolution of MgII absorber kinematicevolution.

MgII Absorbers in High Resolution Quasar Spectra. I. Voigt Profile Models