The physics and astrophysics of X-ray outflows from Active Galactic
  Nuclei
  The highly energetic outflows from Active Galactic Nuclei detected in X-rays
are one of the most powerful mechanisms by which the central supermassive black
hole (SMBH) interacts with the host galaxy. The last two decades of high
resolution X-ray spectroscopy with XMM and Chandra have improved our
understanding of the nature of these outflowing ionized absorbers and we are
now poised to take the next giant leap with higher spectral resolution and
higher throughput observatories to understand the physics and impact of these
outflows on the host galaxy gas. The future studies on X-ray outflows not only
have the potential to unravel some of the currently outstanding puzzles in
astronomy, such as the physical basis behind the MBH$-\sigma$ relation, the
cooling flow problem in intra-cluster medium (ICM), and the evolution of the
quasar luminosity function across cosmic timescales, but also provide rare
insights into the dynamics and nature of matter in the immediate vicinity of
the SMBH. Higher spectral resolution ($\le 0.5$ eV at $1$ keV) observations
will be required to identify individual absorption lines and study the
asymmetries and shifts in the line profiles revealing important information
about outflow structures and their impact. Higher effective area ($\ge 1000 \rm
\,cm^{2}$) will be required to study the outflows in distant quasars,
particularly at the quasar peak era (redshift $1\le z\le 3$) when the AGN
population was the brightest. Thus, it is imperative that we develop next
generation X-ray telescopes with high spectral resolution and high throughput
for unveiling the properties and impact of highly energetic X-ray outflows. A
simultaneous high resolution UV + X-ray mission will encompass the crucial AGN
ionizing continuum, and also characterize the simultaneous detections of UV and
X-ray outflows, which map different spatial scales along the line of sight.
