  Recent radiation-magnetohydrodynamic simulations of active galactic nuclei
predict the presence of the disk winds, which may get unstable and turn into
fragmented clumps far from the central black hole. These inner winds and the
outer clumps may be observed as the ultrafast outflows (UFOs) and the partial
absorbers, respectively. However, it is challenging to observationally
constrain their origins because of the complicated spectral features and
variations. To resolve such degeneracies of the clumpy absorbers and other
components, we developed a novel ``spectral-ratio model fitting'' technique
that estimates the variable absorbing parameters from the ratios of the
partially absorbed spectra to the non-absorbed one, canceling the complex
non-variable spectral features. We applied this method to the narrow-line
Seyfert 1 galaxy \iras observed by \xmm in 2016 for $\sim$1.5 Ms. As a result,
we found that the soft spectral variation is mostly caused by changes in the
partial covering fraction of the mildly-ionized clumpy absorbers, whose outflow
velocities are similar to those of the UFO ($\sim$0.2--0.3 $c$). Furthermore,
the velocities of the clumpy absorbers and UFOs increase similarly with the
X-ray fluxes, consistent with the change in the UV-dominant continuum flux. We
also discovered a striking correlation between the clump covering fraction and
the equivalent width of the UFO absorption lines, which indicates that
increasing the outflow in the line-of-sight lead to more prominent UFOs and
more partial absorption. These findings strongly suggest that the clumpy
absorbers and the UFO share the same origin, driven by the same UV-dominant
continuum radiation.
