Accretion-disk outflows produce a wide variety of UV absorption lines in quasar spectra, from BALs and mini-BALs to narrow absorption lines (NALs) at speeds from ~0 to ~0.2c and velocity widths from ~10 to ~10,000 km/s. This diversity is critical to our understanding of the outflows. How are the different outflow features related? What can they tell us separately and altogether about the structure, origins, and energetics of quasar outflows? I will discuss several studies that address these questions using multi-epoch spectroscopy and Cloudy photoionization models of lines ranging from BALs to NALs. Our main goal is to derive basic outflow physical properties like the gas densities, total column densities, absorber locations, spatial sizes, and kinetic energies. We specifically examine low-abundance lines like PV 1118,1128 for column density constraints and excited-state lines like SiII*, CIII*, SIV*, HeI*, and FeII* combined with variability data for density and location constraints. I will also briefly describe a newly-discovered population of redshift z~2 extremely red quasars (ERQs) that has extreme outflow properties, perhaps during an early stage of quasar-galaxy evolution.
// by Adi