Spectroscopic Observations of the Outflowing Wind in the Lensed Quasar SDSS J1001+5027

We performed spectroscopic observations of the small-separation lensed quasar SDSS J1001+5027, whose images have an angular separation ⊖ = 2.″86, and placed constraints on the physical properties of gas clouds in the vicinity of the quasar (i.e., in the outflowing wind launched from the accretion disk). The two cylinders of sight to the two lensed images go through the same region of the outflowing wind and they become fully separated with no overlap at a very large distance from the source (∼ 330 pc). We discovered a clear difference in the profile of the C IV broad absorption line (BAL) detected in the two lensed images in two observing epochs. Because the kinematic components in the BAL profile do not vary in concert, the observed variations cannot be reproduced by a simple change of ionization state. If the variability is due to gas motion around the background source (i.e., the continuum source), the corresponding rotational velocity is v_rot≥18,000 km s^-1, and their distance from the source is r ≤ 0.06 pc assuming Keplerian motion. Among three Mg II and three C IV NAL systems that we detected in the spectra, only the Mg II system at zabs = 0.8716 shows a hint of variability in its Mg I profile on a rest-frame timescale of Δ_trest ≤ 191 days and an obvious velocity shear between the sightlines whose physical separation is ∼ 7 kpc. We interpret this as the result of motion of a cosmologically intervening absorber, perhaps located in a foreground galaxy.