  We present 44 and 226 GHz observations of the Galactic center within 20$"$ of
Sgr A*. Millimeter continuum emission at 226 GHz is detected from eight stars
that have previously been identified at near-IR and radio wavelengths. We also
detect a 5.8 mJy source at 226 GHz coincident with the magnetar SGR~J1745-29
located 2.39$"$ SE of Sgr A* and identify a new 2.5$"\times1.5"$ halo of mm
emission centered on Sgr A*. The X-ray emission from this halo has been
detected previously and is interpreted in terms of a radiatively inefficient
accretion flow. The mm halo surrounds an EW linear feature which appears to
arise from Sgr A* and coincides with the diffuse X-ray emission and a minimum
in the near-IR extinction. We argue that the millimeter emission is produced by
synchrotron emission from relativistic electrons in equipartition with a $\sim
1.5$mG magnetic field. The origin of these is unclear but its coexistence with
hot gas supports scenarios in which the gas is produced by the interaction of
winds either from the fast moving S-stars, the photo-evaporation of low-mass
YSO disks or by a jet-driven outflow from Sgr A*. The spatial anti-correlation
of the X-ray, radio and mm emission from the halo and the low near-IR
extinction provides compelling evidence for an outflow sweeping up the
interstellar material, creating a dust cavity within 2$"$ of Sgr A*. Finally,
the radio and mm counterparts to eight near-IR identified stars within
$\sim$10\arcs\ of Sgr A* provide accurate astrometry to determine the
positional shift between the peak emission at 44 and 226 GHz.
