Using the 20-pixel camera SHARC , we have surveyed the 350 \micron emission from a 60 \arcmin by 12 \arcmin region in the Galactic center .
A comparable region has been observed at 800 \micron by Lis & Carlstrom ( 1994 ) ; the SHARC map has better spatial resolution and sensitivity to extended emission , however .
This paper introduces several features not visible in prior maps of dust emission .
We have detected a 10+ pc band of emission peaking at l = -0.14 \deg,b = +0.02 \deg , which is probably associated with the ’ negative velocity arc ’ observed in ^ { 13 } CO ( Bally et al .
1988 ) .
We suggest an association of a rounded 350 \micron feature near the Radio Arc with an expanding shell observed in CS ( Tsuboi , Ukita , & Handa 1997 ) .
Faint emission at the same Galactic longitude as the Dust Ridge ( Lis & Carlstrom 1994 ) but at opposite latitude is visible as well as a compact source at the base of a thermal radio filament at negative Galactic latitude .
Diffuse dust emission within a few arcminutes of the Sgr D core is detected for the first time .
350 \micron sources are associated with both H _ { 2 } O masers in Sgr D , but only one out of four OH masers ( Mehringer et al .
1998 ) .
The mean 350 \micron /800 \micron flux ratio for the Galactic center is approximately 17 ( \beta \sim 2.0 ) over the map but is higher ( \beta \sim 2.5 ) in parts of the Dust Ridge and lower in Sgr B2 ( N ) .