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We present continued analysis of a sample of low-redshift iron low-ionizationbroad absorption-line quasars (FeLoBALQs). Choi et al. (2022) presented$SimBAL$ spectral analysis of BAL outflows in 50 objects. Leighly et al. (2022)analyzed optical emission lines of 30 of those 50 objects and found that theyare characterized by either a high accretion rate($L_\mathrm{Bol}/L_\mathrm{Edd}>0.3$) or low accretion rate($0.03<L_\mathrm{Bol}/L_\mathrm{Edd}<0.3$). We report that the outflow velocityis inversely correlated with the BAL location among the high accretion rateobjects, with the highest velocities observed in the parsec-scale outflows. Incontrast, the low Eddington ratio objects showed the opposite trend. Weconfirmed the known relationship between outflow velocity and$L_\mathrm{Bol}/L_\mathrm{Edd}$, and found that the scatter plausiblyoriginates in the force multiplier (launch radius) in the low (high) accretionrate objects. A log volume filling factor between $-6$ and $-4$ was found inmost outflows, but was as high as $-1$ for low-velocity compact outflows. Weinvestigated the relationship between the observed [O III] emission and thatpredicted from the BAL gas. We found that these could be reconciled if theemission-line covering fraction depends on Seyfert type and BAL location. Thedifference between the predicted and observed [O III] luminosity is correlatedwith the outflow velocity, suggesting that [O III] emission in high Eddingtonratio objects may be broad and hidden under Fe II emission. We suggest that thephysical differences in the outflow properties as a function of location in thequasar and accretion rate point to different formation, acceleration, andconfinement mechanisms for the two FeLoBALQ types.

The Properties of Low-Redshift FeLoBAL Quasars: III. The Location and Geometry of the Outflows