19 pages, 21 figures, accepted for publication in ApJ; new revision includes tests of spectral line contribution. The maps analyzed in this paper are available for public download at http://find.spa.umn.edu/quad/quad_galactic/International audienceWe present a survey of ~800 deg2 of the galactic plane observed with the QUaD telescope. The primary products of the survey are maps of Stokes I, Q, and U parameters at 100 and 150 GHz, with spatial resolution of 5' and 3farcm5, respectively. Two regions are covered, spanning approximately 245°-295° and 315°-5° in the galactic longitude l and -4° < b < +4° in the galactic latitude b. At 0fdg02 square pixel size, the median sensitivity is 74 and 107 kJy sr-1 at 100 GHz and 150 GHz respectively in I, and 98 and 120 kJy sr-1 for Q and U. In total intensity, we find an average spectral index of α = 2.35 ± 0.01(stat) ± 0.02(sys) for |b| <= 1°, indicative of emission components other than thermal dust. A comparison to published dust, synchrotron, and free-free models implies an excess of emission in the 100 GHz QUaD band, while better agreement is found at 150 GHz. A smaller excess is observed when comparing QUaD 100 GHz data to the WMAP five-year W band; in this case, the excess is likely due to the wider bandwidth of QUaD. Combining the QUaD and WMAP data, a two-component spectral fit to the inner galactic plane (|b| <= 1°) yields mean spectral indices of α s = -0.32 ± 0.03 and α d = 2.84 ± 0.03; the former is interpreted as a combination of the spectral indices of synchrotron, free-free, and dust, while the second is largely attributed to the thermal dust continuum. In the same galactic latitude range, the polarization data show a high degree of alignment perpendicular to the expected galactic magnetic field direction, and exhibit mean polarization fraction 1.38 ± 0.08(stat) ± 0.1(sys)% at 100 GHz and 1.70 ± 0.06(stat) ± 0.1(sys)% at 150 GHz. We find agreement in polarization fraction between QUaD 100 GHz and the WMAP W band, the latter giving 1.1% ± 0.4%

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oaioai:HAL:hal-00736868v1Last time updated on 11/12/2016

This paper was published in HAL-CEA.

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