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In addition to its potential to probe the Inflationary cosmological paradigm,millimeter-wave polarimetry is a powerful tool for studying the Milky Waygalaxy's composition and magnetic field structure. Towards this end, presentedhere are Stokes I, Q, and U maps of the Galactic plane from the millimeter-wavepolarimeter BICEP covering the Galactic longitude range 260 - 340 degrees inthree atmospheric transmission windows centered on 100, 150, and 220 GHz. Themaps sample an optical depth 1 < AV < 30, and are consistent with previouscharacterizations of the Galactic millimeter-wave frequency spectrum and thelarge-scale magnetic field structure permeating the interstellar medium.Polarized emission is detected over the entire region within two degrees of theGalactic plane and indicates that the large-scale magnetic field is orientedparallel to the plane of the Galaxy. An observed trend of decreasingpolarization fraction with increasing total intensity rules out the simplestmodel of a constant Galactic magnetic field throughout the Galaxy. IncludingWMAP data in the analysis, the degree-scale frequency spectrum of Galacticpolarization fraction is plotted between 23 and 220 GHz for the first time. Agenerally increasing trend of polarization fraction with electromagneticfrequency is found, which varies from 0.5%-1.5%at frequencies below 50 GHz to2.5%-3.5%above 90 GHz. The BICEP and WMAP data are fit to a two-component(synchrotron and dust) model showing that the higher frequency BICEP data arenecessary to tightly constrain the amplitude and spectral index of Galacticdust. Furthermore, the dust amplitude predicted by this two-component fit isconsistent with model predictions of dust emission in the BICEP bands.

A Millimeter-Wave Galactic Plane Survey With The BICEP Polarimeter