A Catalogue of Radio Sources Between Declinations ?50° and ?80°

Mills, Sean R.; Slee, O. B.; Hill, E. R.

doi:10.1071/ph610497

Cited by 62 publications

(48 citation statements)

References 4 publications

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“…With its first detection at radio wavelengths, the SNR MSH 15-56 (G326.3−1.8) became the prototype for the composite class of SNRs (Mills et al 1961;Milne et al 1979). A lower limit on its distance of 3.1 kpc has been established by the H i absorption profile of Goss et al (1972), while Rosado et al (1996) found a distance of 4.1 kpc through Hα velocity measurements, the distance we adopt in this paper.…”

Section: Introductionmentioning

confidence: 99%

HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56

Temim

Slane

Castro

et al. 2013

ApJ

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MSH 15-56 (G326.3−1.8) is a composite supernova remnant (SNR) that consists of an SNR shell and a displaced pulsar wind nebula (PWN) in the radio. We present XMM-Newton and Chandra X-ray observations of the remnant that reveal a compact source at the tip of the radio PWN and complex structures that provide evidence for mixing of the supernova (SN) ejecta with PWN material following a reverse shock interaction. The X-ray spectra are well fitted by a non-thermal power-law model whose photon index steepens with distance from the presumed pulsar, and a thermal component with an average temperature of 0.55 keV. The enhanced abundances of silicon and sulfur in some regions, and the similar temperature and ionization timescale, suggest that much of the X-ray emission can be attributed to SN ejecta that have either been heated by the reverse shock or swept up by the PWN. We find one region with a lower temperature of 0.3 keV that appears to be in ionization equilibrium. Assuming the Sedov model, we derive a number of SNR properties, including an age of 16,500 yr. Modeling of the γ -ray emission detected by Fermi shows that the emission may originate from the reverse shock-crushed PWN.

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Section: Introductionmentioning

confidence: 99%

HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56

Temim

Slane

Castro

et al. 2013

ApJ

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“…MSH 15−52 (G320.4−1.2) is a complex supernova remnant (SNR) that was discovered in radio wavelengths by Mills et al (1961). Its radio appearance is dominated by two spots, a brighter one to the northwest and a fainter one to the southeast.…”

Section: Introductionmentioning

confidence: 99%

Spatially resolved XMM-Newton analysis and a model of the nonthermal emission of MSH 15–52

Schöck¹,

Büsching²,

Jager³

et al. 2010

A&A

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We present an X-ray analysis and a model of the nonthermal emission of the pulsar wind nebula (PWN) MSH 15−52. We analyzed XMM-Newton data to obtain the spatially resolved spectral parameters around the pulsar PSR B1509−58. A steepening of the fitted power-law spectra and decrease in the surface brightness is observed with increasing distance from the pulsar. In the second part of this paper, we introduce a model for the nonthermal emission, based on assuming the ideal magnetohydrodynamic limit. This model is used to constrain the parameters of the termination shock and the bulk velocity of the leptons in the PWN. Our model is able to reproduce the spatial variation of the X-ray spectra. The parameter ranges that we found agree well with the parameter estimates found by other authors with different approaches. In the last part of this paper, we calculate the inverse Compton emission from our model and compare it to the emission detected with the HESS telescope system. Our model is able to reproduce the flux level observed with HESS, but not the spectral shape of the observed TeV γ-ray emission.

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“…Numerous radio observations of A3667 (e.g. Mills, Slee & Hill 1961;Ekers 1969;Schilizzi 1975;Goss et al 1982;Rottgering et al 1997) have noted the bright extended structures in A3667 but failed to image the entire extent of both relics. The first study of the entire region at high resolution (∼ 6 arcsec), including both the NW and SE relics, was carried out by Johnston-Hollitt (2003) at 1.4 GHz.…”

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confidence: 99%

“…The presence of a faint radio halo in the centre of the cluster has also been reported (Johnston-Hollitt 2004;Carretti et al 2013). The only study of A3667 below 300 MHz was performed more than five decades ago by Mills et al (1961) at 86 MHz using the Mills Cross Telescope with a resolution of 50 arcmin. The large angular extent and high surface brightness of the relics and the detection of a faint radio halo and bridge (at frequencies of 1.4-3.3 GHz) in A3667 make it an excellent laboratory in which to carry out low-frequency observations to study the ICM.…”

mentioning

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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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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A Catalogue of Radio Sources Between Declinations ?50° and ?80°

Cited by 62 publications

References 4 publications

HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56

HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56

Spatially resolved XMM-Newton analysis and a model of the nonthermal emission of MSH 15–52

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

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