Multi-wavelength features of Fermi Bubbles as signatures of a Galactic
  wind
  Using hydrodynamical simulations, we show for the first time that an episode
of star formation in the center of the Milky Way, with a star-formation-rate
(SFR) $\sim 0.5$ M$_\odot$ yr$^{-1}$ for $\sim 30$ Myr, can produce bubbles
that resemble the Fermi Bubbles (FBs), when viewed from the solar position. The
morphology, extent and multi-wavelength observations of FBs, especially X-rays,
constrain various physical parameters such as SFR, age, and the circum-galactic
medium (CGM) density. We show that the interaction of the CGM with the Galactic
wind driven by a star formation in the central region can explain the observed
surface brightness and morphological features of X-rays associated with the
Fermi Bubbles. Furthermore, assuming that cosmic ray electrons are accelerated
{\it in situ} by shocks and/or turbulence, the brightness and morphology of
gamma-ray emission and the microwave haze can be explained. The kinematics of
the cold and warm clumps in our model also matches with recent observations of
absorption lines through the bubbles.
