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ABSTRACT In the Hubble Space Telescope/Cosmic Origins Spectrograph spectrum of the Seyfert 1 galaxy 2MASX J14292507+4518318, we have identified a narrow absorption line outflow system with a velocity of −151 km s−1. This outflow exhibits absorption troughs from the resonance states of ions like C iv, N v, S iv, and Si ii, as well as excited states from C ii* and Si ii*. Our investigation of the outflow involved measuring ionic column densities and conducting photoionization analysis. These allow the total column density of the outflow to be estimated as log NH = 19.84 cm−2, its ionization parameter to be log UH = −2.0, and its electron number density to be log ne = 2.75 cm−3. These measurements enabled us to determine the mass-loss rate and the kinetic luminosity of the outflow system to be $$\dot{M}$$ = 0.22 $$\mathrm{ M}_{\odot } \, \mathrm{ yr}^{-1}$$ and $$\log \dot{E_{\mathrm{ K}}}$$ = 39.3 erg s−1, respectively. We have also measured the location of the outflow system to be at ∼275 pc from the central source. This outflow does not contribute to the active galactic nucleus (AGN) feedback processes due to the low ratio of the outflow’s kinetic luminosity to the AGN’s Eddington luminosity ($$\dot{E_{\mathrm{ K}}}/{L_{\mathrm{ Edd}}}\approx 0.00025 {{\, \rm per\, cent}}$$). This outflow is remarkably similar to the two bipolar lobe outflows observed in the Milky Way by XMM–Newton and Chandra.
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High mass flow rate in a BAL outflow of quasar SDSS J1130 + 0411
ABSTRACT We present the analysis of the absorption troughs of six outflows observed in quasar SDSS J1130 + 0411 ($$z$$ ≈ 3.98) with radial velocities ranging from −2400 to $$-15\, 400$$ km s−1. These spectra were taken with the Very Large Telescope/Ultraviolet and Visual Echelle Spectrograph over the rest-frame wavelength range of 1135–1890 Å. In the main outflow system ($$v$$ ≈ −3200 km s−1), we identify Fe ii and several Fe ii* absorption troughs, as well as Si ii and Si ii* troughs, which we use to determine the electron number density $$\log n_e = 2.6_{-0.7}^{+0.8}$$ cm−3. Using the column densities of these and other ions, we determine a photoionization solution with hydrogen column density $$\log N_H = 21.44_{-0.33}^{+0.24}$$ cm−2 and ionization parameter $$\log U_H = -1.75_{-0.45}^{+0.28}$$. From these values, we derive the distance $$R = 16_{-11}^{+23}$$ kpc, the average mass flow rate $$\dot{M} = 4100_{-2400}^{+6600}$$ M⊙ yr−1, and the kinetic luminosity $$\log \dot{E}_k = 46.13_{-0.37}^{+0.41}$$ erg s−1. This $$\dot{E}_k$$ is $$1.4_{-0.8}^{+2.2}$$ per cent of the quasar’s Eddington luminosity, and therefore contributes significantly to AGN feedback.
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- Award ID(s):
- 2106249
- PAR ID:
- 10372027
- Publisher / Repository:
- Oxford University Press
- Date Published:
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Volume:
- 516
- Issue:
- 3
- ISSN:
- 0035-8711
- Page Range / eLocation ID:
- p. 3778-3785
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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