TY - JOUR
T1 - THE QUaD GALACTIC PLANE SURVEY. I. MAPS AND ANALYSIS OF DIFFUSE EMISSION
AU - QUaD Collaboration
AU - Culverhouse, T.
AU - Ade, P.
AU - Bock, J.
AU - Bowden, M.
AU - Brown, M. L.
AU - Cahill, G.
AU - Castro, P. G.
AU - Church, S. E.
AU - Friedman, R.
AU - Ganga, K.
AU - Gear, W. K.
AU - Gupta, S.
AU - Hinderks, J. R.
AU - Kovac, J.
AU - Lange, A. E.
AU - Leitch, E.
AU - Melhuish, S. J.
AU - Memari, Y.
AU - Murphy, J. A.
AU - Orlando, A.
AU - Schwarz, R.
AU - O'Sullivan, C.
AU - Piccirillo, L.
AU - Pryke, C.
AU - Rajguru, N.
AU - Rusholme, B.
AU - Taylor, A. N.
AU - Thompson, K. L.
AU - Turner, A. H.
AU - Wu, E. Y. S.
AU - Zemcov, M.
PY - 2010/10/20
Y1 - 2010/10/20
N2 - We present a survey of similar to 800 deg(2) 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 3'.5, respectively. Two regions are covered, spanning approximately 245 degrees-295 degrees and 315 degrees-5 degrees in the galactic longitude l and -4 degrees < b < +4 degrees in the galactic latitude b.At 0 degrees.02 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 alpha = 2.35 +/- 0.01 (stat) +/- 0.02 (sys) for vertical bar b vertical bar <= 1 degrees, 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 (vertical bar b vertical bar <= 1 degrees) yields mean spectral indices of alpha(s) = -0.32 +/- 0.03 and alpha(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%.
AB - We present a survey of similar to 800 deg(2) 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 3'.5, respectively. Two regions are covered, spanning approximately 245 degrees-295 degrees and 315 degrees-5 degrees in the galactic longitude l and -4 degrees < b < +4 degrees in the galactic latitude b.At 0 degrees.02 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 alpha = 2.35 +/- 0.01 (stat) +/- 0.02 (sys) for vertical bar b vertical bar <= 1 degrees, 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 (vertical bar b vertical bar <= 1 degrees) yields mean spectral indices of alpha(s) = -0.32 +/- 0.03 and alpha(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%.
UR - http://www.scopus.com/inward/record.url?scp=78149275387&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/722/2/1057
DO - 10.1088/0004-637X/722/2/1057
M3 - Article
SN - 0004-637X
VL - 722
SP - 1057
EP - 1077
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -