MgII Absorbers in High Resolution Quasar Spectra. I. Voigt Profile
  Models
  We present the Voigt profile (VP) models, column densities, Doppler b
parameters, kinematics, and distribution of components for 422 MgII absorbers
found in a survey of 249 HIRES and UVES quasar spectra. The equivalent width
range of the sample is 0.006 < W_r(2796) < 6.23 angstroms (A) and the redshift
range is 0.19 < z < 2.55, with a mean of <z> = 1.18. Based on historical
precedent, we classified 180 absorbers as weak systems (W_r(2796) < 0.3 A) and
242 as strong systems (W_r(2796) >= 0.3 A). Assuming a minimum number of
significant components per system, the VP fitting, yielded a total of 2,989
components, with an average of 2.7 and 10.3 components found for the weak and
strong MgII subsamples, respectively. The VP component line density for the
full sample is 8.62 +/- 0.23 clouds/A. The distribution of VP component column
density over the range 12.4 < log[N(MgII)] < 17.0 [ions cm^-2] is well modeled
with a power-law slope of -1.45 +/- 0.01. The median Doppler b parameters are
4.5 +/- 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 a
three-component composite Gaussian function. Our resulting velocity dispersions
are 25.4, 68.7, and 207.1 km/s, respectively. These data provide an excellent
database for studying the cosmic evolution of MgII absorber kinematic
evolution.
