3.1. Kinematic Models
Two of the simplest types of organized kinematics in galaxies are illustrated in Figure 5: clouds distributed in a rotating disk, and radial infall of clouds in a spherical distribution. Here, Mg II absorbers are used as an example, but the same kinematic arguments would apply to other transitions. For radial infall, clouds can be distributed over the range of velocities, with a tendency for a ``double peak'' from material that is redshifted and blueshifted but with a considerable amount of variation if there are typically several discrete clouds along the line of sight. A rotating disk with a vertical velocity dispersion characteristic of a spiral galaxy disk (10-20 km s-1) will have clouds superimposed in velocity space, and an overall kinematic spread of tens of km s-1. Strong Mg II absorption has been found to arise along nearly all lines of within ~ 40 kpc of normal galaxies (i.e. the covering factor is nearly unity within that radius). The large variety of kinematics evident in Mg II absorption profiles is, in fact, consistent with a superposition of disk and radial infall (halo) motions, and not with just one or the other. In addition to these simple, toy models, insights can be gleaned by passing lines of sight through the structures in cosmological N-body/hydrodynamic simulations. In a few studies, metals have been added uniformly throughout the simulation box and photoionization models used to predict the absorption expected from different structures. This is especially important for establishing the kinematics that would be observed from the process of structure formation at high redshifts.