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04 December 2021
  » arxiv » astro-ph/0407130

 Article overview

First results from the ATCA 18 GHz pilot survey
R. Ricci ; E. M. Sadler ; R. D. Ekers ; L. Staveley-Smith ; W. E. Wilson ; M. J. Kesteven ; R. Subrahmanyan ; M. A. Walker ; C. A. Jackson ; G. De Zotti ;
Date 7 Jul 2004
Subject astro-ph
Affiliation1,2), E. M. Sadler , R. D. Ekers , L. Staveley-Smith , W. E. Wilson , M. J. Kesteven , R. Subrahmanyan , M. A. Walker (1,3), C. A. Jackson , G. De Zotti (4,2), ( ATNF, SISSA, Sydney University, Padua Observatory
AbstractAs a pilot study for the first all-sky radio survey at short wavelengths, we have observed 1216 sq. deg. of the southern sky at 18GHz (16mm) using a novel wide-band (3.4GHz bandwidth) analogue correlator on one baseline of the Australia Telescope Compact Array (ATCA). We scanned a region of sky between declination -71 and -59 degrees with an rms noise level of 15mJy. Follow-up radio imaging of candidate sources above a 4 sigma detection limit of 60mJy resulted in 221 confirmed detections, for which we have measured accurate positions and flux densities. For extragalactic sources, the survey is roughly 70% complete at a flux density of 126mJy and 95% complete above 300mJy. Almost half the detected sources lie within a few degrees of the Galactic plane, but there are 123 sources with |b|>5 degrees which can be assumed to be extragalactic. The differential source counts for extragalactic sources in the range 0.1Jy < S_{18GHz} < 3Jy are well fitted by a relation of the form n(S)=57(S/{Jy})^{-2.2pm0.2} [Jy^-1 sr^-1], in good agreement with the 15GHz counts published by Taylor et al. (2001) and Waldram et al. (2003). Over 70% of the extragalactic sources have a flat radio spectrum (alpha_{0.843}^{18}> -0.5, S_{ u}propto u^{alpha}), and 29% have inverted radio spectra (alpha_{0.843}^{18}> 0). The optical identification rate is high: 51% of the extragalactic sources are identified with stellar objects (candidate QSOs), 22% with galaxies and only 27% with faint optical objects or blank fields.
Source arXiv, astro-ph/0407130
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