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This work provides evidence that a large fraction of \ion{C}{IV} narrowabsorption lines (NALs) seen along the line of sight to distant quasars are dueto accretion disk winds, while also seeking to understand the relationshipbetween NALs and certain quasar-intrinsic properties. We extend the resultsfrom past work in the literature using $\sim105,000$ NALs from a sample of$\sim58,000$ SDSS quasars. The primary results of this work are summarized asfollows: (1) the velocity distribution (${\rm d}N/{\rm d}\beta$) of NALs is nota function of radio loudness (or even detection) once marginalized byoptical/UV luminosity; (2) there are significant differences in the number anddistribution of NALs as a function of both radio spectral index and optical/UVluminosity, and these two findings are not entirely interdependent; (3)improvements in quasar systemic redshift measurements and differences in theNAL distribution as a combined function of optical luminosity and radiospectral index together provide evidence that a significant portion of NALs aredue to outflows; (4) the results are consistent with standard models ofaccretion disk winds governed by the $L_{\rm UV}$-$\alpha_{ox}$ relationshipand line-of-sight orientation indicated by radio spectral index, and (5)possibly support a magnetically arrested disk model as an explanation for thesemi-stochastic nature of strong radio emission in a fraction of quasars.

Narrow, Intrinsic CIV Absorption in Quasars as it Relates to Outflows, Orientation, and Radio Properties