2003
DOI: 10.1086/345974
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Abstract: The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 square degrees, an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalogue. The mosaic achieves a 1σ rms noise of 12 µJy at its most sensitive, and a homogeneous radio-selected ca… Show more

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Cited by 152 publications
(186 citation statements)
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References 30 publications
(74 reference statements)
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“…These source counts are broadly consistent with previous results at 1.4 GHz (e.g. the compilation of Windhorst et al 1993; the PHOENIX Deep Survey, Hopkins et al 2003; and the shallow NEP survey of Kollgaard et al 1994).…”
Section: Differential Countssupporting
confidence: 91%
See 2 more Smart Citations
“…These source counts are broadly consistent with previous results at 1.4 GHz (e.g. the compilation of Windhorst et al 1993; the PHOENIX Deep Survey, Hopkins et al 2003; and the shallow NEP survey of Kollgaard et al 1994).…”
Section: Differential Countssupporting
confidence: 91%
“…However, for completeness, we will repeat the Hopkins et al (2003) equations using the terminology in the present paper, which reduce to those presented by Rengelink et al (1997). For point sources, Hopkins et al (2003) show that the total relative uncertainty in the integrated flux density is given by:…”
Section: Noise Flux Accuracymentioning
confidence: 98%
See 1 more Smart Citation
“…This resulted in a reasonably even distribution of the number of sources per bin. The source counts of all sources, the VLBA-detected sources, and the source counts by Hopkins et al (2003) are shown in Fig. 16.…”
Section: Source Countsmentioning
confidence: 99%
“…In recent decades, radio interferometers, such as the Karl G. Jansky Very Large Array (VLA), Australia Telescope Compact Array (ATCA), and Giant Meterwave Radio Telescope (GMRT), have surveyed fields of different sizes (ranging from tens of square arcminutes to thousands of square degrees), depths (microjansky to jansky), and multiwavelength coverage (e.g., Becker et al 1995;Condon et al 1998Condon et al , 2003Condon et al , 2012Ciliegi et al 1999;Georgakakis et al 1999;Bock et al 1999;Prandoni et al 2001;Hopkins et al 2003;Schinnerer et al 2004;Bondi et al 2003Bondi et al , 2007Norris et al 2005;Schinnerer et al 2007Schinnerer et al , 2010; Afonso et al 2005;Tasse et al 2007;Smolčić et al 2008Smolčić et al , 2014Owen & Morrison 2008;Miller et al 2008Miller et al , 2013Owen et al 2009;Hales et al 2014). These past surveys have shown that deep observations at high angular resolution ( 1 ) with exquisite panchromatic coverage are critical to comprehensively study the radio properties of the main galaxy populations, avoiding cosmic variance with large area coverage (e.g., Padovani et al 2009;Padovani 2011;Smolčić et al 2008Smolčić et al , 2009bSmolčić 2009;Smolčić & Riechers 2011;Seymour et al 2008;Bonzini et al 2012Bonzini et al , 2013.…”
Section: Introductionmentioning
confidence: 99%