SDSS J163459.82+204936.0: A Ringed Infrared-Luminous Quasar With Outflows in Both Absorption and Emission Lines

Shi

et al. 2017

ApJ

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We report the detection of heavy reddening and the He I* λ10830 absorption lines at the AGNs' redshift in three Narrow-line Seyfert 1 galaxies: SDSS J091848.61+211717.0, SDSS J111354.66+124439.0, and SDSS J122749.13+321458.9. They exhibit very red optical to nearinfrared colors, narrow Balmer/Paschen broad emission lines and He I* λ10830 absorption lines. The ultraviolet-optical-infrared nucleus continua are reddened by the SMC extinction law of E(B − V ) ∼ 0.74, 1.17, and 1.24 mag for three objects, which are highly consistent with the values obtained from the broad-line Balmer decrements, but larger than those of narrow emission lines. The reddening analysis suggests the extinction dust simultaneously obscure the accretion disk, the broad emission line region, and the hot dust from the inner edge of the torus. It is possible that the dust obscuring the AGN structures are the dusty torus itself. Furthermore, the Cloudy analysis of the He I* λ10830 absorption lines propose the distance of the absorption materials to be the extend scale of the torus. That greatly increases probabilities of the obscure and absorption materials being the dusty torus.

Section: Broadband Spectral Energy Distributionmentioning

confidence: 99%

“…We picked them up again during the series study of the reddening AGNs (e.g., Li et al 2015;Liu et al 2016;Pan et al 2017;Zhang et al 2017). We study the He I* λ10830 absorption lines (the first detection reported by Leighly et al 2011) as well as the continuum, and hydrogen Balmer/Paschen broad emission lines of these objects.…”

Section: Introductionmentioning

confidence: 99%

Reddening and He i^∗ λ10830 Absorption Lines in Three Narrow-line Seyfert 1 Galaxies

Zhang

Shi

et al. 2017

ApJ

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“…The fraction is generally 10%-20% in optical-selected quasars (e.g., Trump et al 2006;Gibson et al 2010;Zhang et al 2014) and~30% (e.g., Maddox et al 2008) or even 44% (Dai et al 2008) in NIR-selected quasars. We consider that BAL and BEL outflows may be different appearances viewed from different inclination angles but representing the same physical component, which is suggested by many works (e.g., Richards et al 2011;Wang et al 2011;Liu et al 2016); the global covering fraction of BEL outflows will follow these values. The value we obtained in SDSS J0006+1215 is slightly smaller than those estimated from optical-selected BAL quasars.…”

Section: Kinetic Luminosity and Mass Flux Of The Outflowsmentioning

confidence: 99%

“…This is because the BALs have high-speed blueshifted (up to a velocity ofṽ c 0.2 ) and broad-width (at least 2000 km s −1 ) troughs from a wide range of species, such as Mg II, Al III, Fe II, N V, C IV, Si IV, and O VI (e.g., Weymann et al 1991;Hall et al 2002;Reichard et al 2003; Trump et al 2006; Gibson et al 2010;Zhang et al 2010), and even from the hydrogen Balmer series (e.g., Hall 2007;Ji et al 2012Ji et al , 2013Zhang et al 2015b) and metastable He I (e.g., Liu et al 2015Liu et al , 2016, whose obvious features allow the BALs to be easily detected and measured. Unfortunately, the broad and narrow blueshifted-ELs (BBELs and BNELs) are generally mixed with the normal broad or narrow lines.…”

Section: Introductionmentioning

confidence: 99%

“…They are potentially one of the most important pieces of feedback from AGNs and may play a crucial role in galaxy formation and evolution, connecting the central supermassive black holes (SMBHs) to their host galaxies and regulating their coevolution (e.g., Granato et al 2004;Scannapieco & Oh 2004;Hopkins et al 2008). Previous works suggested that the AGN outflows can reach from the small scale (at or outside of the broad emission line region [BELR]; e.g., Zhang et al 2015c;Williams et al 2016) to the intermediate scale (the dusty torus; e.g., Leighly et al 2015;Zhang et al 2015b;Shi et al 2016), the large scale (the inner narrow emission line region [NELR]; e.g., Komossa et al 2008;Crenshaw et al 2010;Ji et al 2015;Liu et al 2016), and even the entire host galaxy of the quasar (e.g., Zakamska et al 2016). There is general agreement that there has to be a radial component of motion and some opacity source; however, questions regarding the origins, whether homologous or not, and the properties themselves of the blueshifted-ELs and BALs remain interesting subjects of debate.…”

Section: Introductionmentioning

confidence: 99%

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Ultraviolet and Optical Emission Line Outflows in the Heavily Obscured Quasar SDSS J000610.67+121501.2: At the Scale of the Dusty Torus and Beyond

Zhang

Shi

et al. 2017

ApJ

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Broad emission line outflows of active galactic nuclei have been proposed for many years but are very difficult to quantitatively study because of the coexistence of the gravitationally bound and outflow emission. We present detailed analysis of a heavily reddened quasar, SDSS J000610.67+121501.2, whose normal ultraviolet broad emission lines (BELs) are heavily suppressed by the dusty torus as a natural "coronagraph," and thus the blueshifted BELs (BBELs) can be reliably measured. The physical properties of the emission-line outflows are derived as follows: ionization parameter~-U 10 0.5 , column densityÑ 10 H 22.0 cm −2 , covering fraction of ∼0.1, and upper limit density ofñ 10 H 5.8 cm −3 . The outflow gases are located at least 41 pc away from the central engine, which suggests that they have expanded to the scale of the dust torus or beyond. Besides, Lyα shows a narrow symmetric component, to our surprise, which is undetected in any other lines. After inspecting the narrow emission line region and the star-forming region as the origin of the Lyα narrow line, we propose that the end result of outflows, diffusing gases in the larger region, acts as the screen of Lyα photons. Future high spatial resolution spectrometry and/or spectropolarimetric observations are needed to make a final clarification.

A broad absorption line outflow associated with the broad emission line region in the quasar SDSS J075133.35+134548.3

Liu

Res. Astron. Astrophys.

Shu

et al. 2021

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We report on the discovery of unusual broad absorption lines (BALs) in the bright quasar SDSS J075133.35+134548.3 at z ∼ 1, using archival and newly obtained optical and NIR spectroscopic data. The BALs are detected reliably in He i* λ3889, He i* λ10830 and tentatively in Al iii, Mg ii. These BALs show complex velocity structures consisting of two major components: a high-velocity component (HV), with a blueshifted velocity range of Δv HV ∼ −9300 − −3500 km s−1, which can be reliably detected in He i* λ10830, and tentatively in Al iii and Mg ii, whereas it is undetectable in He i* λ3889 and a low-velocity component (LV), with Δ v LV ∼ −3500 − −1800 km s−1, is only detected in He i* and He i* λ10830. With the BALs from different ions, the HV outflowing gas can be constrained to have a density of n H ∼1010.3–1011.4 cm−3, a column density of N H ∼ 1021 cm−2 and an ionization parameter of U ∼10−1.83–10−1.72; inferring a distance of R HV∼0.5 pc from the central continuum source with a monochromatic luminosity λ Lλ (5100) = 7.0×1045 erg s−1 at 5100 Å. This distance is remarkably similar to that of the normal broad line region (BLR) estimated from reverberation experiments, suggesting association of the BLR and the HV BAL outflowing gas. Interestingly, a blueshifted component is also detected in Al iii and Mg ii broad emission lines (BELs), and the Al iii/Mg ii of such a BEL component can be reproduced by the physical parameters inferred from the HV BAL gas. The LV BAL gas likely has a larger column density, a higher ionization level and hence a smaller distance than the HV BAL gas. Further spectroscopy with a high S/N ratio and broader wavelength coverage is needed to confirm this to shed new light on the possible connection between BALs and BELs.