A semi-empirical simulation of the extragalactic radio continuum sky for next generation radio telescopes

Wilman, R. J.; Miller, L.; Jarvis, Matt J.; Mauch, T.; Levrier, F.; Abdalla, F. B.; Rawlings, Steve; Klöckner, H.-R.; Obreschkow, Danail; Olteanu, D.; Young, S.

doi:10.1111/j.1365-2966.2008.13486.x

Cited by 234 publications

(289 citation statements)

References 72 publications

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“…Right: redshift versus radio luminosity of the same galaxies, showing that the galaxies probed are in the bright tail of the radio luminosity function and have significant luminosity evolution. 0, applied to normal star forming galaxies in the SKADS S3 simulation of Wilman et al (2008). We expect to detect ∼5000 galaxies per square degree above 10σ .…”

Section: Emergence and Evolution Of Magnetic Fields In Galaxiesmentioning

confidence: 93%

SKA Deep Polarization and Cosmic Magnetism

Taylor¹,

Agudo²,

Akahori³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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Deep surveys with the SKA1-MID array offer for the first time the opportunity to systematically explore the polarization properties of the microJy source population. Our knowledge of the polarized sky approaching these levels is still very limited. In total intensity the population will be dominated by star-forming and normal galaxies to intermediate redshifts (z ∼ 1 − 2), and low-luminosity AGN to high redshift. The polarized emission from these objects is a powerful probe of their intrinsic magnetic fields and of their magnetic environments. For redshift of order 1 and above the broad bandwidth of the mid-bands span the Faraday thick and thin regimes allowing study of the intrinsic polarization properties of these objects as well as depolarization from embedded and foreground plasmas. The deep field polarization images will provide Rotation Measures data with very high solid angle density allowing a sensitive statistical analysis of the angular variation of RM on critical arc-minute scales from a magnetic component of Large Scale Structure of the Universe.Advancing Astrophysics with the Square Kilometre Array

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Section: Emergence and Evolution Of Magnetic Fields In Galaxiesmentioning

confidence: 93%

SKA Deep Polarization and Cosmic Magnetism

Taylor¹,

Agudo²,

Akahori³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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“…The foreground emission components that contaminate the 21 cm signals have been continuously discussed and simulated in detail in many works (e.g., Jelić et al 2008Jelić et al , 2010Gleser et al 2008;Bowman et al 2009). In our previous work (W2010), we fully took into account the effects of random variations of model parameters in the ranges allowed by the observations in Monte Carlo simulations to model the emissions from our Galaxy, galaxy clusters, and discrete sources (i.e., star-forming galaxies, radio-quiet AGNs, and radio-loud AGNs), and constructed the 50-200 MHz radio sky maps with a frequency resolution of 40 kHz, following the works of Snellen et al (2000), Giardino et al (2002), Finkbeiner (2003, Wilman et al (2008), and reference therein. All of the simulated sky maps are plotted in a circular field of view (FOV) with a radius of 5…”

Section: CM Signals Of Neutral Hydrogen From Eormentioning

confidence: 99%

“…In order to address the problems raised above, we attempt to re-examine and improve the polynomial fitting algorithm by applying a more complex foreground emission model that contains detailed emulations of both spatial and spectral features of the real sources (see Wang et al 2010 for details, which followed Snellen et al 2000, Giardino et al 2002, Finkbeiner 2003, and Wilman et al 2008 and references therein; W2010 hereafter), meanwhile employing a multi-narrow-frequency segment quadratic polynomial fitting technique to remove the foreground emission components in frequency space. We find that our new algorithm can reasonably correct the systematic bias introduced by the single-narrow-segment algorithm, which may lead to a reduction of the 21 cm signal power by about 75% for 6 h −1 Mpc scales and 34% for 1 h −1 Mpc scales, and therefore a significant underestimate of both the H ii bubble size and growth rate.…”

Section: Introductionmentioning

confidence: 99%

EXPLORING THE COSMIC REIONIZATION EPOCH IN FREQUENCY SPACE: AN IMPROVED APPROACH TO REMOVE THE FOREGROUND IN 21 cm TOMOGRAPHY

Wang

et al. 2013

ApJ

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With the intent of correctly restoring the redshifted 21 cm signals emitted by neutral hydrogen during the cosmic reionization processes, we re-examine the separation approaches based on the quadratic polynomial fitting technique in frequency space in order to investigate whether they work satisfactorily with complex foreground by quantitatively evaluating the quality of restored 21 cm signals in terms of sample statistics. We construct the foreground model to characterize both spatial and spectral substructures of the real sky, and use it to simulate the observed radio spectra. By comparing between different separation approaches through statistical analysis of restored 21 cm spectra and corresponding power spectra, as well as their constraints on the mean halo bias b and average ionization fraction x e of the reionization processes, at z = 8 and the noise level of 60 mK we find that although the complex foreground can be well approximated with quadratic polynomial expansion, a significant part of the Mpc-scale components of the 21 cm signals (75% for 6 h −1 Mpc scales and 34% for 1 h −1 Mpc scales) is lost because it tends to be misidentified as part of the foreground when the single-narrow-segment separation approach is applied. The best restoration of the 21 cm signals and the tightest determination of b and x e can be obtained with the three-narrow-segment fitting technique as proposed in this paper. Similar results can be obtained at other redshifts.

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“…Contribution of normal star forming galaxies to total intensity and polarized source counts at 1.4 GHz. Model total intensity source counts (black curve) adapted from [18]. Crosses: total intensity (top) and polarized (bottom) source sounts from the NVSS [19].…”

Section: B Modelsmentioning

confidence: 99%