In order to calibrate the telescope and instrument polarization we will rely on observations of planets, and a program of laboratory measurements of polarization by reflection that is now underway at Northwestern University. The photometric observations of the Galaxy will require approximately a full winter to obtain a map of one-third of the Galactic plane. Unlike submillimeter surveys that have been carried out from space, our Galactic survey will have sufficient angular resolution to resolve individual Giant Molecular Clouds in distant regions of the Galaxy. This colder dust accounts for most of the dust mass in the Galaxy. Existing large-scale surveys of molecular lines will provide the velocity information that will be lacking in our own observations.
Dust absorbs starlight, thus heating the interstellar medium.
Where the opacity is great enough, the dust shields the interstellar matter from the starlight, leading to the formation of Giant Molecular Clouds. It is likely that this picture will improve our understanding of the role of dust in the formation of Giant Molecular Clouds and in star formation. Planned submillimeter polarimetry of the extended Galactic Center region. The submillimeter brightness is sufficient for us to be able to obtain an accurate polarimetric map of the entire region enclosed within the dark contour in 12 weeks of observations during the Antarctic winter. The upper and lower star symbols show the positions of Sgr B2 and Sgr A, respectively.