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Published July 2011 | Published
Journal Article Open

The QUaD Galactic Plane Survey. II. A Compact Source Catalog


We present a catalog of compact sources derived from the QUaD Galactic Plane Survey. The survey covers ~800 deg^2 of the inner galaxy (|b| < 4°) in Stokes I, Q, and U parameters at 100 and 150 GHz, with angular resolutions of 5 and 3.5 arcmin, respectively. Five hundred and twenty-six unique sources are identified in I, of which 239 are spatially matched between frequency bands, with 53 (234) detected at 100 (150) GHz alone; 170 sources are identified as ultracompact H II regions. Approximating the distribution of total intensity source fluxes as a power law, we find a slope of γ_(S,100) = –1.8 ± 0.4 at 100 GHz and γ_(S,150) = –2.2 ± 0.4 at 150 GHz. Similarly, the power-law index of the source two-point angular correlation function is γ_(θ,100) = –1.21 ± 0.04 and γ_(θ,150) = –1.25 ± 0.04. The total intensity spectral index distribution peaks at α_I ~ 0.25, indicating that dust emission is not the only source of radiation produced by these objects between 100 and 150 GHz; free-free radiation is likely significant in the 100 GHz band. Four sources are detected in polarized intensity P, of which three have matching counterparts in I. Three of the polarized sources lie close to the Galactic center, Sagittarius A^*, Sagittarius B2, and the Galactic Radio Arc, while the fourth is RCW 49, a bright H II region. An extended polarized source, undetected by the source extraction algorithm on account of its ~0°5 size, is identified visually, and is an isolated example of large-scale polarized emission oriented distinctly from the bulk Galactic dust polarization.

Additional Information

© 2011 The American Astronomical Society. Received 2010 May 20; accepted 2011 May 20; published 2011 June 29. This paper is dedicated to the memory of Andrew Lange, who gave wisdom and guidance to so many members of the astrophysics and cosmology community. His presence is sorely missed. We thank our colleagues on the BICEP experiment for useful discussions. QUaD is funded by the National Science Foundation in the USA, through grants ANT-0338138, ANT-0338335, and ANT-0338238, by the Science and Technology Facilities Council (STFC) in the UK, and by the Science Foundation Ireland. We thank the staff of the Amundsen- Scott South Pole Station and all involved in the United States Antarctic Program for the superb support operation which makes the science presented here possible. Special thanks go to our intrepid winter scientist Robert Schwarz who spent three consecutive winter seasons tending the QUaD experiment. The BOOMERanG collaboration kindly allowed the use of their CMB maps for our calibration purposes. M.L.B. acknowledges the award of a PPARC Fellowship. S.E.C. acknowledges support from a Stanford Terman Fellowship. J.R.H. acknowledges the support of an NSF Graduate Research Fellowship and a Stanford Graduate Fellowship. C.P. acknowledges partial support from the Kavli Institute for Cosmological Physics through the grant NSF PHY-0114422. E.Y.W. acknowledges receipt of an NDSEG fellowship. J.M.K. acknowledges support from a John B. and Nelly L. Kilroy Foundation Fellowship.

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Published - Culverhouse2011p15393Astrophys_J_Suppl_S.pdf


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August 22, 2023
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