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

Abstract

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.

Ionized Gas Outflows in Infrared-bright Dust-obscured Galaxies Selected with WISE and SDSS

“…The IR luminosities of the 36 IR-bright DOG sample are log L IR [L ⊙ ] = 10.5 -13.1, and 25/36 (∼ 69 %) objects are classified as ULIRGs/HyLIRGs (see Table 1). Recently some authors have discovered many (obscured) ULIRGs/HyLIRGs based on the SDSS and WISE data and reported powerful ionized outflows seen in their spectra (Ross et al 2015;Zakamska et al 2016;Bischetti et al 2017;Hamann et al 2017;Zhang et al 2017), although they basically focus on high-z (z > 2) objects.…”

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

“…In this work, we report the extremely reddening and the detection of He I* λ10830 absorption lines at the AGNs' redshift in three NLS1s: SDSS J091848.61+211717.0, SDSS J111354.66+124439.0, and SDSS J122749.13+321458.9 (hereafter SDSS J0918+2117, SDSS J1113+1244, and SDSS J1227+3214), which were initially reported by the red Two Micron All Sky Survey (2MASS; Skrutskie et al 2006) AGNs (Kuraszkiewicz et al 2009) and the FIRST-2MASS red quasars (F2M; Glikman et al 2007;. 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.…”

“…Fortunately, the two facts, i.e., the perfect matching of the optical/NIR spectra simply multiplied by a factor and the broad-band SEDs, and the high consistency of extinctions from the SED fitting and the Balmer decrements (see next section), rule out the possibility of variability affecting on the SED in these three NLS1s. When we take a overview of the features of the SEDs, it is obvious that the observed SEDs of all the three objects show very different shapes from that of the average quasar spectrum, but in contrast to be similar with the heavily obscured quasar SDSS J000610.67+121501.2 reported in Zhang et al (2017). In the optical, and NIR bands, they is much lower than the average quasar spectrum; from the u-or N U V -band up to lower wavelengths, the SEDs slightly turn up (extremely weak in SDSS J0918+2117).…”

“…In the optical, and NIR bands, they is much lower than the average quasar spectrum; from the u-or N U V -band up to lower wavelengths, the SEDs slightly turn up (extremely weak in SDSS J0918+2117). The unique shape is considered to be caused by the spectral combination of two different continuum slopes (Zhang et al 2017). When looking at the emission/absorption lines, the optical and NIR spectra show the significant broad/narrow emission lines, He I * λ10830 and weak Ca II H and K (3969 and 3934Å) absorption lines, which represent the contributions of the AGN and its host galaxy.…”

“…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.…”