We present radio and mm continuum observations of the Galactic center taken with the VLA and ALMA at 44 and 226 GHz , respectively .
We detect radio and mm emission from IRS 3 , lying \sim 4.5 ^ { \prime \prime } NW of Sgr A* , with a spectrum that is consistent with the photospheric emission from an AGB star at the Galactic center .
Millimeter images reveal that the envelope of IRS 3 , the brightest and most extended 3.8 \mu m Galactic center stellar source , consists of two semi-circular dust shells facing the direction of Sgr A* .
The outer circumstellar shell at the distance of 1.6 \times 10 ^ { 4 } AU , appears to break up into “ fingers ” of dust directed toward Sgr A* .
These features coincide with molecular CS ( 5-4 ) emission and a near-IR extinction cloud distributed between IRS 3 and Sgr A* .
The NE-SW asymmetric shape of the IRS 3 shells seen at 3.8 \mu m and radio are interpreted as structures that are tidally distorted by Sgr A* .
Using the kinematics of CS emission and the proper motion of IRS 3 , the tidally distorted outflowing material from the envelope after 5000 years constrains the distance of IRS 3 to \sim 0.7 pc in front of or \sim 0.5 pc behind Sgr A* .
This suggests that the mass loss by stars near Sgr A* can supply a reservoir of molecular material near Sgr A* .
We also present dark features in radio continuum images coincident with the envelope of IRS 3 .
These dusty stars provide examples in which high resolution radio continuum images can identify dust enshrouded stellar sources embedded an ionized medium .