Resolving the Clumpy Structure of the Outflow Winds in the
  Gravitationally Lensed Quasar SDSS J1029+2623
  We study the geometry and the internal structure of the outflowing wind from
the accretion disk of a quasar by observing multiple sightlines with the aid of
strong gravitational lensing. Using Subaru/HDS, we performed high-resolution
($R$ $\sim$ 36,000) spectroscopic observations of images A and B of the
gravitationally lensed quasar SDSS J1029+2623 (at $z_{em}$ $\sim$ 2.197) whose
image separation angle, $\theta$ $\sim$ 22$^{\prime\prime}\!\!$.5, is the
largest among those discovered so far. We confirm that the difference in
absorption profiles in the images A and B discovered by Misawa et al. (2013)
remains unchanged since 2010, implying the difference is not due to time
variability of the absorption profiles over the delay between the images,
$\Delta t$ $\sim$ 744 days, but rather due to differences along the sightlines.
We also discovered time variation of C IV absorption strength in both images A
and B, due to change of ionization condition. If a typical absorber's size is
smaller than its distance from the flux source by more than five orders of
magnitude, it should be possible to detect sightline variations among images of
other smaller separation, galaxy-scale gravitationally lensed quasars.
