Discovery of Faint Radio Structures over 50 Square Degrees Down to 3 arcmin Scales near the NGP

Details Discovery of Faint Radio Structures over 50 Square Degrees Down to 3 arcmin Scales near the NGP Discovery of Faint Radio Structures over 50 Square Degrees Down to 3 arcmin Scales near the NGP

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.5301k&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #53.01; Bulletin of the American Astronomical Society, V

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We present a deep, 8o diameter, 0.4 GHz radio image near the North Galactic Pole using a first time combination of the Arecibo 305-m telescope and the wide-angle interferometer at the DRAO. The uniquely complementary nature of these two instruments permits a distortion-free image sensitive to radiation on all scales from 8o down to that of an individual galaxy halo at the 100 Mpc distance of the Great Wall, all in a single pointing. Faint, previously unseen diffuse patches of distributed radio ``glow'' are detected, well above our detection limit, and on a range of angular scales. The emission could compete with CMB fluctuations as a CMB foreground at high multipole scales around 30GHz if its radio spectrum continues up to these GHz bands. This new faint radio emission appears to be a mix of foreground Galactic, and extragalactic ``glow’. The latter implies i.g. magnetic field strengths at or above 0.1 microgauss on Mpc scales in certain areas. A striking anticorrelation is also found between the diffuse radio glow and some regions of high optical galaxy surface density. This suggests that cosmological Large Scale Structure (LSS), normally defined by the baryonic (and/or dark) matter density, is not uniquely traced by the faint continuum radio glow. More likely, the radio glow is a proxy for IGM energy density, at least in the low redshift universe. Its detailed relation to the WHIM, and diffuse X-ray glow is unclear, and must await future, more sensitive detectors for these latter two IGM components. Support for this project is acknowledged from the DOE's LDRD program at LANL, the Natural Sciences and Engineering Research Council of Canada (NSERC), and the National Science Foundation.

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