The Phoenix Deep Survey: 1.4-GHz source counts

Hopkins, A. M.; Mobasher, Bahram; Cram, L. E.; Rowan-Robinson, M.

doi:10.1046/j.1365-8711.1998.01403.x

Cited by 109 publications

(184 citation statements)

References 5 publications

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“…In the southern hemisphere, the Australia Telescope Compact Array, (ATCA) has been used to study the Phoenix field (Hopkins et al 1998;, the Hubble Deep FieldYSouth ( Huynh et al 2005), and the Chandra Deep FieldYSouth and ELAIS SWIRE fields Afonso et al 2006). Combined VLA and MERLIN observations of the HDFN (Muxlow et al 2005) with a resolution of 0.2 00 show the complexity of the microjansky radio emission suggesting a mixture of AGNs and star formation which contributes to the submillijansky radio population.…”

Section: Radio Studiesmentioning

confidence: 99%

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The VLA Survey of the Chandra Deep Field–South. I. Overview and the Radio Data

Kellermann

Fomalont

Mainieri

et al. 2008

Astrophysical Journal Supplement Series, The

103

142

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We report 20 and 6 cm VLA deep observations of the CDF-S including the Extended CDF-S. We discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20 cm completeness level reaching down to 43 Jy at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20 cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, we have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20 cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources above a conservative 3 detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, we still find an apparent significant contribution from low-luminosity AGN as well as from star formation.

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Section: Radio Studiesmentioning

confidence: 99%

“…References to other counts are PDFS and PDF ( Hopkins et al 1998), MC85 ( Mitchell & Condon 1985), OW84 (Oort & Windhorst 1985), ELIAS (Ciliegi et al 1999), HDF ( Richards 2000), and SSA13 ( Fomalont et al 2006). The highest flux density points are based on a compilation from Condon (1984).…”

Section: Source Countmentioning

confidence: 99%

The VLA Survey of the Chandra Deep Field–South. I. Overview and the Radio Data

Kellermann

Fomalont

Mainieri

et al. 2008

Astrophysical Journal Supplement Series, The

103

142

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“…The upturn in the source counts was initially explained through modelling of source populations with no need to include a substantial AGN contribution (e.g. Hopkins et al 1998). However, a growing number of studies are finding that lower luminosity AGN, both radio-loud and weakly radio emitting sources (radio-loud and radio-quiet AGN respectively), make a significant contribution to the sub-mJy population (Jarvis & Rawlings 2004;Huynh et al 2008;Seymour et al 2008;Smolčić et al 2008;Padovani et al 2009Padovani et al , 2011Bonzini et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The ATLAS 5.5 GHz survey of the extendedChandraDeep Field South: the second data release

Huynh¹,

Bell²,

Hopkins³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a new image of the 5.5 GHz radio emission from the extended Chandra Deep Field South. Deep radio observations at 5.5 GHz were obtained in 2010 and presented in the first data release. A further 76 hours of integration has since been obtained, nearly doubling the integration time. This paper presents a new analysis of all the data. The new image reaches 8.6 µJy rms, an improvement of about 40% in sensitivity. We present a new catalogue of 5.5 GHz sources, identifying 212 source components, roughly 50% more than were detected in the first data release. Source counts derived from this sample are consistent with those reported in the literature for S 5.5GHz > 0.1 mJy but significantly lower than published values in the lowest flux density bins (S 5.5GHz < 0.1 mJy), where we have more detected sources and improved statistical reliability. The 5.5 GHz radio sources were matched to 1.4 GHz sources in the literature and we find a mean spectral index of −0.35 ± 0.10 for S 5.5GHz > 0.5 mJy, consistent with the flattening of the spectral index observed in 5 GHz sub-mJy samples. The median spectral index of the whole sample is α med = −0.58, indicating that these observations may be starting to probe the star forming population. However, even at the faintest levels (0.05 < S 5.5GHz < 0.1 mJy), 39% of the 5.5 GHz sources have flat or inverted radio spectra. Four flux density measurements from our data, across the full 4.5 to 6.5 GHz bandwidth, are combined with those from literature and we find 10% of sources (S 5.5GHz 0.1 mJy) show significant curvature in their radio spectral energy distribution spanning 1.4 to 9 GHz.

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“…The dominance of starburst galaxies in the sub-mJy population is already well established (Gruppioni et al 2008), where the number of blue galaxies with star-forming spectral signatures is seen to increase strongly. Rowan-Robinson et al (1993), Hopkins et al (1998), and others have concluded that the source counts at these faintest levels require two populations, AGNs and starburst galaxies. This latter population can best be modelled as a dusty star-forming population, under the assumption that they are the higher redshift analogues of the IRAS star-forming population (Rowan-Robinson et al 1993;Pearson & Rowan-Robinson 1996).…”

Section: Differential Countsmentioning

confidence: 98%

“…Note that Huynh et al (2005) used the radio luminosity function of Condon et al (2002) and derived a best fitting evolution parameterisation ∝(1 + z) 2.7 , slightly lower than the work presented here although the values are broadly consistent and differences can be due to the assumed SED and luminosity function. Hopkins (2004) and Hopkins et al (1998) used radio and infrared luminosity functions respectively obtaining evolution in the sub-mJy population ∝(1 + z) 2.7 and ∝(1 + z) 3.3 . It does however appear that the counts measured in this study lie at the lower end of the emerging picture on excess sub-mJy radio counts, as shown in Fig.…”

Section: Differential Countsmentioning

confidence: 99%

A deep survey of the AKARI north ecliptic pole field

White

Pearson

Braun

et al. 2010

A&A

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Aims. The Westerbork Radio Synthesis Telescope, WSRT, has been used to make a deep radio survey of an ∼1.7 degree 2 field coinciding with the AKARI north ecliptic pole deep field. The observations, data reduction and source count analysis are presented, along with a description of the overall scientific objectives. Methods. The survey consisted of 10 pointings, mosaiced with enough overlap to maintain a similar sensitivity across the central region that reached as low as 21 μJy beam −1 at 1.4 GHz. Results. A catalogue containing 462 sources detected with a resolution of 17.0 × 15.5 is presented. The differential source counts calculated from the WSRT data have been compared with those from the shallow VLA − NEP survey of Kollgaard et al. 1994, and show a pronounced excess for sources fainter than ∼1 mJy, consistent with the presence of a population of star forming galaxies at sub-mJy flux levels. Conclusions. The AKARI north ecliptic pole deep field is the focus of a major observing campaign conducted across the entire spectral region. The combination of these data sets, along with the deep nature of the radio observations will allow unique studies of a large range of topics including the redshift evolution of the luminosity function of radio sources, the clustering environment of radio galaxies, the nature of obscured radio-loud active galactic nuclei, and the radio/far-infrared correlation for distant galaxies. This catalogue provides the basic data set for a future series of paper dealing with source identifications, morphologies, and the associated properties of the identified radio sources.

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The Phoenix Deep Survey: 1.4-GHz source counts

Cited by 109 publications

References 5 publications

The VLA Survey of the Chandra Deep Field–South. I. Overview and the Radio Data

The VLA Survey of the Chandra Deep Field–South. I. Overview and the Radio Data

The ATLAS 5.5 GHz survey of the extendedChandraDeep Field South: the second data release

A deep survey of the AKARI north ecliptic pole field

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