2022ApJ...929...81L

We present a detailed analysis of the rest-frame UV and optical emission-line spectrum of the partially obscured quasar J121704.70+023417.1 (hereafter J1217+0234). Here the obscuring material, very likely the dusty torus invoked by the AGN unification models, acts as a natural coronagraph, which greatly suppresses both the continuum and broad-line emission in the UV and enables a clear detection of three emission-line components at and beyond the dusty torus scale: (1) The component, with a blueshift of v ≃ 1200 km s^–1 and a line width of FWHM ≃ 2600 km s^–1, shows exceptionally large intensity ratios, such as N V/Lyα ≃ 2.3 and O VI/Lyα ≃ 1.4, indicating that the emitting gas is highly ionized and has a very high density up to n_H ∼ 10¹³ cm^–3, possibly associated with the dusty torus. (2) The largely unshifted narrow-line component, with FWHM ≃ 510 km s^–1, is completely absent in all UV lines but Lyα and is significantly detected in the forbidden lines of [O III], [O II], and [Ne III] in the optical, implying massive low-density (n_H ∼ 10² cm^–3) gas ∼40 kpc from the galactic center. (3) The intermediate component is only detected in [O III] with a blueshift and line width between (1) and (2), which might bridge the gases from the circumnuclear to the circumgalactic scales. Follow-up observations with high spatial resolution and high sensitivity are needed to confirm the speculation and are helpful to reveal outflows at multiscales in J1217+0234.