  Using visible, radio, microwave, and sub-mm data, we study several lines of
sight toward stars generally closer than 1 kpc on a component-by-component
basis. We derive the component structure seen in absorption at visible
wavelengths from Ca II, Ca I, K I, CH, CH$^{+}\!,$ and CN and compare it to
emission from H I, CO and its isotopologues, and C$^{+}$ from the GOT C+
survey. The correspondence between components in emission and absorption help
create a more unified picture of diffuse atomic and molecular gas in the
interstellar medium. We also discuss how these tracers are related to the
CO-dark H$_{2}$ gas probed by C$^{+}$ emission and discuss the kinematic
connections among the species observed.
