Context.Quasar outflows are often analyzed to determine their ability to contribute to active galactic nucleus (AGN) feedback. We identified a broad absorption line (BAL) outflow in the VLT/UVES spectrum of the quasar SDSS J1321−0041. The outflow shows troughs from Fe II, and is thus categorized as an FeLoBAL. This outfow is unusual among the population of FeLoBAL outflows, as it displays C IIand Si IIBALs. Aims.Outflow systems require a kinetic luminosity above ∼0.5% of the quasar’s luminosity to contribute to AGN feedback. For this reason, we analyzed the spectrum of J1321−0041 to determine the outflow’s kinetic luminosity, as well as the quasar’s bolometric luminosity. Methods.We measured the ionic column densities from the absorption troughs in the spectrum and determined the hydrogen column density and ionization parameter using those column densities as our constraints. We also determined the electron number density,ne, based on the ratios between the excited-state and resonance-state column densities of Fe IIand Si II. This allowed us to find the distance of the outflow from its central source, as well as its kinetic luminosity. Results.We determined the kinetic luminosity of the outflow to be 8.4−5.4+13.7 × 1045 erg s−1and the quasar’s bolometric luminosity to be 1.72 ± 0.13 × 1047 erg s−1, resulting in a ratio ofĖk/LBol = 4.8−3.1+8.0%. We conclude that this outflow has a sufficiently high kinetic luminosity to contribute to AGN feedback.
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Physical characterization of the FeLoBAL outflow in SDSS J0932+0840: Analysis of VLT/UVES observations
Context.The study of quasar outflows is essential for understanding the connection between active galactic nuclei (AGN) and their host galaxies. We analyzed the VLT/UVES spectrum of quasar SDSS J0932+0840 and identified several narrow and broad outflow components in absorption, with multiple ionization species including Fe II. This places it among the rare class of outflows known as iron low-ionization broad absorption line outflows (FeLoBALs). Aims.We studied one of the outflow components to determine its physical characteristics by determining the total hydrogen column density, the ionization parameter, and the hydrogen number density. Through these parameters, we obtained the distance of the outflow from the central source, its mass outflow rate, and its kinetic luminosity, and we constrained the contribution of the outflow to the AGN feedback. Methods.We obtained the ionic column densities from the absorption troughs in the spectrum and used photoionization modeling to extract the physical parameters of the outflow, including the total hydrogen column density and ionization parameter. The relative population of the observed excited states of Fe IIwas used to model the hydrogen number density of the outflow. Results.We used the Fe IIexcited states to model the electron number density (ne) and hydrogen number density (nH) independently and obtainedne≃ 103.4cm−3andnH≃ 104.8cm−3. Our analysis of the physical structure of the cloud shows that these two results are consistent with each other. This places the outflow system at a distance of 0.7−0.4+0.9kpc from the central source, with a mass flow rate (Ṁ) of 43−26+65 M⊙yr−1and a kinetic luminosity (Ėk) of 0.7−0.4+1.1× 1043erg s−1. This is 0.5−0.3+0.7× 10−4of the Eddington luminosity (LEdd) of the quasar, and we thus conclude that this outflow is not powerful enough to contribute significantly toward AGN feedback.
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- Award ID(s):
- 2106249
- PAR ID:
- 10613907
- Publisher / Repository:
- Astronomy & Astrophysics
- Date Published:
- Journal Name:
- Astronomy & Astrophysics
- Volume:
- 693
- ISSN:
- 0004-6361
- Page Range / eLocation ID:
- A254
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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