The Molonglo Southern 4 Jy Sample (MS4). I. Definition

Burgess, Ann M.; Hunstead, R. W.

doi:10.1086/498677

Cited by 45 publications

(73 citation statements)

References 155 publications

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“…The MS4 catalogue contains 228 bright sources with flux densities >4 Jy at 408 MHz between −85 • < δ < −30 • . Burgess & Hunstead (2006) have performed cross-matching with various archival and published data to calculate the flux density at intervals between 86 and 5000 MHz. The flux density error estimate given by Burgess & Hunstead (2006) for bright and compact sources is ∼10 per cent and this is factored into our method.…”

Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 99%

“…Burgess & Hunstead (2006) have performed cross-matching with various archival and published data to calculate the flux density at intervals between 86 and 5000 MHz. The flux density error estimate given by Burgess & Hunstead (2006) for bright and compact sources is ∼10 per cent and this is factored into our method. To minimize errors in the flux density calibration we apply the following selection criteria to MS4 sources.…”

Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 99%

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The First Murchison Widefield Array low-frequency radio observations of cluster scale non-thermal emission: the case of Abell 3667

Hindson¹,

Johnston‐Hollitt²,

Hurley‐Walker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present the first Murchison Widefield Array observations of the well-known cluster of galaxies Abell 3667 (A3667) between 105 and 241 MHz. A3667 is one of the best known examples of a galaxy cluster hosting a double radio relic and has been reported to contain a faint radio halo and bridge. The origin of radio haloes, relics and bridges is still unclear, however galaxy cluster merger seems to be an important factor. We clearly detect the north-west (NW) and south-east radio relics in A3667 and find an integrated flux density at 149 MHz of 28.1 ± 1.7 and 2.4 ± 0.1 Jy, respectively, with an average spectral index, between 120 and 1400 MHz, of −0.9 ± 0.1 for both relics. We find evidence of a spatial variation in the spectral index across the NW relic steepening towards the centre of the cluster, which indicates an ageing electron population. These properties are consistent with higher frequency observations. We detect emission that could be associated with a radio halo and bridge. However, due to the presence of poorly sampled large-scale Galactic emission and blended point sources we are unable to verify the exact nature of these features.

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Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 99%

Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 99%

The First Murchison Widefield Array low-frequency radio observations of cluster scale non-thermal emission: the case of Abell 3667

Hindson¹,

Johnston‐Hollitt²,

Hurley‐Walker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…The four sub-samples, MRC1 (McCarthy et al 1996), MS4 (Burgess & Hunstead 2006), BRL (Best et al 1999) and 3CRR (Laing et al 1983) are described in the paper of Yuan & Wang (2012). For comparison, the radio luminosity function (RLF) at 408 MHz estimated by the two methods are plotted together for all the redshift bins in Fig.…”

Section: Applying the Methods To Real Datamentioning

confidence: 99%

A graphical analysis of the systematic error of classical binned methods in constructing luminosity functions

Yuan

Wang

2013

Astrophys Space Sci

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The classical 1/V a and P C methods of constructing binned luminosity functions (LFs) are revisited and compared by graphical analysis. Using both theoretical analysis and illustration with an example, we show why the two methods give different results for the bins which are crossed by the flux limit curves L = L lim (z). Based on a combined sample simulated by a Monte Carlo method, the estimate φ of two methods are compared with the input model LFs. The two methods give identical and ideal estimate for the high luminosity points of each redshift interval. However, for the low luminosity bins of all the redshift intervals both methods give smaller estimate than the input model. We conclude that once the LF is evolving with redshift, the classical binned methods will unlikely give an ideal estimate over the total luminosity range. Page & Carrera (2000) noticed that for objects close to the flux limit φ 1/Va nearly always to be too small. We believe this is due to the arbitrary choosing of redshift and luminosity intervals. Because φ 1/Va is more sensitive to how the binning are chosen than φ P C . We suggest a new binning method, which can improve the LFs produced by the 1/V a method significantly, and also improve the LFs produced by the P C methods. Our simulations show that after adopting this new binning, both the 1/V a and P C methods have comparable results.

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“…The 4.8-GHz radio map of Burgess (1998) already showed evidence for embedded hotspots. PKS B1416−493 has other radio similarities to PKS B2152−699.…”

Section: Introductionmentioning

confidence: 98%

“…The MS4 catalog is the southern equivalent of 3CRR (Burgess 1998;Burgess & Hunstead 2006a,b). Our joint Chandra and ATCA programme concentrated first on the brightest FR I/II boundary source in the catalogue, the z = 0.0282 radio galaxy PKS B2152−699 (Worrall et al 2012).…”

Section: Introductionmentioning

confidence: 99%

A non cool-core 4.6-keV cluster around the bright nearby radio galaxy PKS B1416−493

Worrall¹,

Birkinshaw²

2017

Monthly Notices of the Royal Astronomical Society

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We present new X-ray (Chandra) and radio (ATCA) observations of the z = 0.09 radio galaxy PKS B1416−493, a member of the southern equivalent of the 3CRR sample. We find the source to be embedded in a previously unrecognized bright kT = 4.6-keV non cool-core cluster. The discovery of new clusters of such high temperature and luminosity within z = 0.1 is rare. The radio source was chosen for observation based on its intermediate FR I/II morphology. We identify a cavity coincident with the northeast lobe, and excess counts associated with the southwest lobe that we interpret as inverse Compton X-ray emission. The jet power, at 5.3 × 10 44 erg s −1 , when weighted by radio source density, supports suggestions that radio sources of intermediate morphology and radio power may dominate radio-galaxy heating in the local Universe.

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The Molonglo Southern 4 Jy Sample (MS4). I. Definition

Cited by 45 publications

References 155 publications

The First Murchison Widefield Array low-frequency radio observations of cluster scale non-thermal emission: the case of Abell 3667

The First Murchison Widefield Array low-frequency radio observations of cluster scale non-thermal emission: the case of Abell 3667

A graphical analysis of the systematic error of classical binned methods in constructing luminosity functions

A non cool-core 4.6-keV cluster around the bright nearby radio galaxy PKS B1416−493

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