THE BOLOCAM GALACTIC PLANE SURVEY: λ = 1.1 AND 0.35 mm DUST CONTINUUM EMISSION IN THE GALACTIC CENTER REGION

Abstract

The Bolocam Galactic Plane Survey (BGPS) data for a six square degree region\nof the Galactic plane containing the Galactic center is analyzed and compared\nto infrared and radio continuum data. The BGPS 1.1 mm emission consists of\nclumps interconnected by a network of fainter filaments surrounding cavities, a\nfew of which are filled with diffuse near-IR emission indicating the presence\nof warm dust or with radio continuum characteristic of HII regions or supernova\nremnants. New 350 {\\mu}m images of the environments of the two brightest\nregions, Sgr A and B, are presented. Sgr B2 is the brightest mm-emitting clump\nin the Central Molecular Zone and may be forming the closest analog to a super\nstar cluster in the Galaxy. The Central Molecular Zone (CMZ) contains the\nhighest concentration of mm and sub-mm emitting dense clumps in the Galaxy.\nMost 1.1 mm features at positive longitudes are seen in silhouette against the\n3.6 to 24 {\\mu}m background observed by the Spitzer Space Telescope. However,\nonly a few clumps at negative longitudes are seen in absorption, confirming the\nhypothesis that positive longitude clumps in the CMZ tend to be on the\nnear-side of the Galactic center, consistent with the suspected orientation of\nthe central bar in our Galaxy. Some 1.1 mm cloud surfaces are seen in emission\nat 8 {\\mu}m, presumably due to polycyclic aromatic hydrocarbons (PAHs). A\n~0.2\\degree (~30 pc) diameter cavity and infrared bubble between l \\approx\n0.0\\degree and 0.2\\degree surrounds the Arches and Quintuplet clusters and Sgr\nA. The bubble contains several clumpy dust filaments that point toward Sgr\nA\\ast; its potential role in their formation is explored. [abstract truncated]\n