Simulation of the Polarized Sky at 1.4 GHz

O’Sullivan, Shane; Stil, J. M.; Taylor, A. Russ; Ricci, R.; Grant, J. K.

doi:10.22323/1.072.0107

Cited by 3 publications

(2 citation statements)

References 3 publications

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“…Further, more detailed investigations may be required in order to refine this conclusion and assess the full range of effects that may potentially affect the dynamic range and structural sensitivity derived from images obtained with different uvcoverages and different values of ∆u/u. One possibility would be to use more elaborate and more realistic sky models coming from source simulations (e.g., O'Sullivan et al 2009).…”

Section: Numerical Simulationsmentioning

confidence: 99%

SKADS Array Configuration Study

Lobanov¹,

Lal²,

Monferrer³

2011

Proceedings of Wide Field Astronomy &Amp; Technology for the Square Kilometre Array — PoS(SKADS 2009)

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Results from SKADS array configuration study are presented, focusing on a quantitative assessment of the effect of the array configuration on imaging performance of the SKA. The spatial dynamic range (SDR) and a measure of incompleteness of the Fourier domain coverage (∆u/u) are employed as prime figures of merit (FoM). We conclude that ∆u/u ≤ 0.03 provides a benchmark at which the Fourier domain coverage will not be a dominant factor limiting imaging capabilities of the SKA. An algorithm for calculating the distribution of ∆u/u from interferometric data is described, and a set of FoM for evaluating array configurations is proposed.

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Section: Numerical Simulationsmentioning

confidence: 99%

SKADS Array Configuration Study

Lobanov¹,

Lal²,

Monferrer³

2011

Proceedings of Wide Field Astronomy &Amp; Technology for the Square Kilometre Array — PoS(SKADS 2009)

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“…Future deep polarization surveys with the SKA prompted the extrapolation of polarized radio source counts to predict the density of a "RM grid" made with a survey of given sensitivity [8]. Later extrapolations were based on a power law extrapolation [9] of faint polarized radio source counts by [10], and by fitting polarized radio source counts with models of radio source populations that include polarization [11,12]. These extrapolations are are made over as much as 4 orders of magnitude in polarized flux density (from ∼ 1 mJy to ∼ 0.1 µJy), with a high level of uncertainty.…”

Section: The Rm Gridmentioning

confidence: 99%

Evolution of magnetic fields in galaxies

Stil¹

2010

Proceedings of Panoramic Radio Astronomy: Wide-Field 1-2 GHz Research on Galaxy Evolution — PoS(PRA2009)

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Faraday rotation of polarized radio sources is one of the most effective observational tools to study cosmic magnetic fields. A densely-sampled grid of Faraday rotation measures that covers the complete sky (the Rotation Measure Grid) will allow us to probe the magnetic field in the Milky Way Galaxy as well as in other nearby galaxies. First results from a new database of 37543 rotation measures that covers over 80% of the sky show the potential of an all-sky polarization survey with SKA path finders and the SKA. Structures in RM on angular scales of tens of degrees and systematic variation in the amplitude and slope of rotation measure structure functions across the sky are presented. A future all-sky RM grid of ∼ 5000 per square degree will allow detailed mapping of the magneto-ionic medium, and also probe ∼ 1000 nearby galaxies with at least 20 rotation measures per galaxy. Observations of magnetic field structure in more distant galaxies will rely on the detection of polarized synchrotron emission for which a deep field would have the necessary sensitivity. At high redshift, imaging the polarized structure of normal galaxies at a resolution of ∼0.1 ′′ or better requires sensitivity beyond the design specifications of the SKA. However, the polarization of unresolved disk galaxies as a function of redshift provides a way to probe the evolution of magnetic fields in disk galaxies over time.

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THE DRAO PLANCK DEEP FIELDS: THE POLARIZATION PROPERTIES OF RADIO GALAXIES AT 1.4 GHz

Grant

Taylor

Stil

et al. 2010

ApJ

107

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We present results of deep polarization imaging at 1.4 GHz with the Dominion Radio Astrophysical Observatory as part of the DRAO Planck Deep Fields project. This deep extragalactic field covers 15.16 deg 2 centered at α 2000 = 16 h 14 m and δ 2000 = 54 • 56 ′ , has an angular resolution of 42 ′′ × 62 ′′ at the field center, and reaches a sensitivity of 55 µJy beam −1 in Stokes I and 45 µJy beam −1 in Stokes Q and U. We detect 958 radio sources in Stokes I of which 136 are detected in polarization. We present the Euclidean-normalized polarized differential source counts down to 400 µJy. These counts indicate that sources have a higher degree of fractional polarization at fainter Stokes I flux density levels than for brighter sources, confirming an earlier result. We find that the majority of our polarized sources are steep-spectrum objects with a mean spectral index of −0.77, and there is no correlation between fractional polarization and spectral index. We also matched deep field sources to counterparts in the Faint Images of the Radio Sky at Twenty Centimeters catalogue. Of the polarized sources, 77% show structure at the arc-second scale whereas only 38% of the sources with no detectable polarization show such structure. The median fractional polarization is for resolved sources is 6.8%, while it is 4.4% for compact objects. The polarized radio sources in our deep field are predominantly those sources which are resolved and show the highest degrees of fractional polarization, indicating that the lobe dominated structure may be the source of the highly polarized sources. These resolved radio galaxies dominate the polarized source counts at P 0 = Q 2 + U 2 < 3 mJy.

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Simulation of the Polarized Sky at 1.4 GHz

Cited by 3 publications

References 3 publications

SKADS Array Configuration Study

SKADS Array Configuration Study

Evolution of magnetic fields in galaxies

THE DRAO PLANCK DEEP FIELDS: THE POLARIZATION PROPERTIES OF RADIO GALAXIES AT 1.4 GHz

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