Radio Polarimetry of the ELAIS N1 Field: Polarized Compact Sources

Taylor, A. R.; Stil, J. M.; Grant, J. K.; Landecker, T. L.; Kothes, R.; Reid, Robert I.; Gray, A. D.; Scott, D.; Martín, P. G.; Boothroyd, Arnold I.; Joncas, G.; Lockman, Felix J.; English, Jayanne; Sajina, Anna; Bond, J. R.

doi:10.1086/519786

Cited by 65 publications

(147 citation statements)

References 25 publications

(42 reference statements)

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“…These results indicate that for steep-spectrum radio sources, the mean fractional polarization increases as flux density decreases. This was confirmed by Taylor et al (2007) for sources with P > 500 microJy.…”

Section: Introductionsupporting

confidence: 54%

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DRAO deep polarization study at 1.4 GHz

et al. 2008

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Abstract. The Dominion Radio Astrophysical Observatory synthesis telescope (DRAO-ST) was used to produce a deep polarization mosaic at 1.4 GHz to a noise level of 45 microJy beam −1 for both Stokes Q and U at 1 resolution. The DRAO deep field covers 8.6 sq. degrees in polarization centered on the ELAIS N1 field. We identified over 1700 total intensity (Stokes I) radio sources of which 197 are linearly polarized down to a flux density level of 203 microJy. The fractional polarization of faint polarized sources are flat down to a polarized flux density of about 4 mJy, at which point the numbers increase, until the counts drop for polarized flux densities below 1 mJy. These faint polarized radio sources are mostly AGNs with luminosities below the traditional FRI/FRII boundary. Follow-up observations with the VLA show that the origin of the polarization of the radio sources down to a polarized flux of 1 mJy comes from both the lobes and central region of these objects.

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Section: Introductionsupporting

confidence: 54%

“…The European Large Area ISO Survey North 1 (ELAIS N1) is the area for the DRAO ELAIS N1 deep field (Taylor et al 2007). This area was selected for deep polarization imaging as a window on the extragalactic sky previously observed by ISO (Oliver et al 2000) and the Spitzer Wide Area Extragalactic Survey (SWIRE, Lonsdale et al 2003).…”

Section: Introductionmentioning

confidence: 99%

DRAO deep polarization study at 1.4 GHz

et al. 2008

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“…This has limited investigations of the polarization properties of EGS to the bright ( ∼ > 80 mJy) radio source population, dominated by powerful, radio loud AGN. There are some indications from these bright sources that at least fainter steep-spectrum radio sources are more highly polarized (Mesa et al 2002;Tucci et al 2004), up to a median Π of ∼ 1.8% in the flux density range 100 -200 mJy and even higher for sources below 100 mJy (Taylor et al 2007). …”

Section: Polarization Sciencementioning

confidence: 92%

“…The presence of such a minimum in the distribution depends on the importance of Faraday depolarization and the importance of poloidal magnetic fields in the halo of these galaxies. We can measure this minimum by including the lowestorder antisymmetric deviations from a Gaussian in our Monte-Carlo analysis of a sufficiently large number of galaxies (Taylor et al 2007). The projected large frequency coverage of ASKAP will allow us to distinguish between highly frequency-dependent Faraday depolarization, and magnetic field structure that should not change with observing frequency.…”

Section: Polarization Sciencementioning

confidence: 99%

Science with the Australian Square Kilometre Array Pathfinder

Johnston

Bailes

Bartel

et al. 2007

Publ. – Astron. Soc. Aust

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The future of cm and m-wave astronomy lies with the Square Kilometre Array (SKA), a telescope under development by a consortium of 17 countries that will be 50 times more sensitive than any existing radio facility. Most of the key science for the SKA will be addressed through largearea imaging of the Universe at frequencies from a few hundred MHz to a few GHz. The Australian SKA Pathfinder (ASKAP) is a technology demonstrator aimed in the mid-frequency range, and achieves instantaneous wide-area imaging through the development and deployment of phased-array feed systems on parabolic reflectors. The large field-of-view makes ASKAP an unprecedented synoptic telescope that will make substantial advances in SKA key science. ASKAP will be located at the Murchison Radio Observatory in inland Western Australia, one of the most radio-quiet locations on the Earth and one of two sites selected by the international community as a potential location for the SKA. In this paper, we outline an ambitious science program for ASKAP, examining key science such as understanding the evolution, formation and population of galaxies including our own, understanding the magnetic Universe, revealing the transient radio sky and searching for gravitational waves.

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“…Total intensity counts from the NVSS are shown as diamonds and polarized counts are shown as crosses. The 10-field DRAO ELAIS N1 polarized source counts [3] are shown as triangles.…”

Section: Simulation Resultsmentioning

confidence: 99%

Simulation of the Polarized Sky at 1.4 GHz

O’Sullivan¹,

Stil²,

Taylor³

et al. 2009

Proceedings of the 9th European VLBI Network Symposium on the Role of VLBI in the Golden Age for Radio Astronomy and EVN Users

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We present results from simulations of the extragalactic polarized sky at 1.4 GHz. As the basis for our polarization models, we use a semi-empirical simulation of the extragalactic total intensity (Stokes I) continuum sky developed at the University of Oxford (http://scubed.physics.ox.ac.uk) under the European SKA Design Study (SKADS) initiative, and polarization distributions derived from analysis of polarization observations. By considering a luminosity dependence for the polarization of AGN, we are able to fit the 1.4 GHz polarized source counts derived from the NVSS and the DRAO ELAIS N1 deep field survey down to approximately 1 mJy. This trend is confirmed by analysis of the polarization of a complete sample of bright AGN. We are unable to fit the additional flattening of the polarized source counts from the deepest observations of the ELAIS N1 survey, which go down to ∼ 0.5 mJy. Below 1 mJy in Stokes I at 1.4 GHz, starforming galaxies become an increasingly important fraction of all radio sources. We use a spiral galaxy integrated polarization model to make realistic predictions of the number of polarized sources at µJy levels in polarized flux density and hence, realistic predictions of what the next generation radio telescopes such as ASKAP, other SKA pathfinders and the SKA itself will see.

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Radio Polarimetry of the ELAIS N1 Field: Polarized Compact Sources

Cited by 65 publications

References 25 publications

DRAO deep polarization study at 1.4 GHz

DRAO deep polarization study at 1.4 GHz

Science with the Australian Square Kilometre Array Pathfinder

Simulation of the Polarized Sky at 1.4 GHz

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