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The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows

Journal Article · · The Astrophysical Journal
 [1];  [1];  [2];  [3];  [4];  [5]
  1. Univ. of Oklahoma, Norman, OK (United States)
  2. Univ. of Oklahoma, Norman, OK (United States); Vanderbilt Univ., Nashville, TN (United States)
  3. Univ. of Oklahoma, Norman, OK (United States); The Ohio State Univ., Columbus, OH (United States)
  4. Univ. of Western Ontario, London, ON (Canada); Canadian Space Agency (Canada)
  5. Drexel Univ., Philadelphia, PA (United States)
+ Show Author Affiliations
We present continued analysis of a sample of low-redshift iron low-ionization broad-absorption-line quasars (FeLoBALQs). Choi et al. presented SimBAL spectral analysis of broad-absorption-line (BAL) outflows in 50 objects. Leighly et al. analyzed the optical emission lines of 30 of those 50 objects and found that they are characterized by either a high accretion rate (LBol/LEdd > 0.3) or low accretion rate (0.03 < LBol/LEdd < 0.3). We report that the outflow velocity is inversely correlated with the BAL location among the high-accretion-rate objects, with the highest velocities observed in parsec-scale outflows. In contrast, the low-Eddington-ratio objects showed the opposite trend. We confirmed the known relationship between the outflow velocity and LBol/LEdd and found that the scatter plausibly originates in the force multiplier (launch radius) in the low(high)-accretion-rate objects. A log volume filling factor between –6 and –4 was found in most outflows but was as high as –1 for low-velocity compact outflows. We investigated the relationship between the observed [O III] emission and that predicted from the BAL gas. We found that these could be reconciled if the emission-line covering fraction depends on the Seyfert type and BAL location. The difference between the predicted and observed [O III] luminosity is correlated with the outflow velocity, suggesting that [O III] emission in high-Eddington-ratio objects may be broad and hidden under Fe ii emission. We suggest that the physical differences in the outflow properties as a function of location in the quasar and accretion rate point to different formation, acceleration, and confinement mechanisms for the two FeLoBALQ types.
Research Organization:
US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
Sponsoring Organization:
Alfred P. Sloan Foundation; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); USDOE Office of Science (SC)
Contributing Organization:
Brookhaven National Laboratory (BNL); Fermi National Accelerator Laboratory (FNAL); Lawrence Berkeley National Laboratory (LBNL); Los Alamos National Laboratory (LANL)
OSTI ID:
1983294
Journal Information:
The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 2 Vol. 936; ISSN 0004-637X
Publisher:
IOP PublishingCopyright Statement
Country of Publication:
United States
Language:
English

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Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
Active galactic nuclei
Broad-absorption line quasar
Quasars