Sgr A* and its Environment: Low Mass Star Formation, the Origin of X-ray
  Gas and Collimated Outflow
  We present high-resolution multiwavelength radio continuum images of the
region within 150$"$ of Sgr A*, revealing a number of new extended features and
stellar sources in this region. First, we detect a continuous 2" east-west
ridge of radio emission, linking Sgr A* and a cluster of stars associated with
IRS 13N and IRS 13E. The ridge suggests that an outflow of east-west blob-like
structures is emerging from Sgr A*. We also find arc-like features within the
ridge with morphologies suggestive of photoevaporative protoplanetary disks. We
use near-IR fluxes to show that the emission has similar characteristics to
those of a protoplanetary disk irradiated by the intense radiation field at the
Galactic center. This suggests that star formation has taken place within the S
cluster 2$"$ from Sgr A*. We suggest that the diffuse X-ray emission associated
with Sgr A* is due to an expanding hot wind produced by the mass loss from
B-type main sequence stars, and/or the disks of photoevaporation of low mass
YSOs at a rate ~10^{-6} solar mass per year. The proposed model naturally
reduces the inferred accretion rate and is an alternative to the inflow-outflow
style models to explain the underluminous nature of Sgr A*. Second, we detect
new cometary radio and nea-IR sources and a striking tower of radio emission
suggesting that they are tracing interaction sites of a mildly relativistic jet
from Sgr A* with the atmosphere of stars and the nonthermal Sgr A East shell at
a PA$\sim50-60^\circ$ with ~10^{-7} solar mass per year, and opening angle 10
degrees.
