High-resolution radio observations of five supernova remnants

Caswell, J. L.; Milne, D. K.; Wellington, K. J.

doi:10.1093/mnras/195.1.89

Cited by 52 publications

(31 citation statements)

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“…Polarisation of up to 15% was detected at 8.55 GHz, while flux densities of S 4.5 = 30 ± 2 Jy and S 8.55 = 17 ± 4 Jy were measured. In conjunction with the flux densities determined by Caswell & Barnes (1985) • 27 40 is non-thermal, has a steep spectral index, and may be extragalactic (Caswell et al 1981). The MOST observations show that the small-diameter source (G315.31−0.27) situated within the extended emission at R.A. (J2000) = 14 h 35 m 06 s , Dec. (J2000) = −60…”

Section: Msca Sourcesmentioning

confidence: 71%

“…Using the Fleurs synthesis radio telescope at 1.415 GHz, Caswell et al (1981) found evidence of shell-like structure in the brighter component, supported by the MOST contour map, although they note that if G308.7+0.0 is a shell SNR, then its appearance is peculiar because it does not have the characteristic sharply-defined outer perimeter. In addition, the emission is significantly more elongated than for a typical shell remnant.…”

Section: Msca Sourcesmentioning

confidence: 96%

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The MOST supernova remnant catalogue (MSC)

Whiteoak

Green

1996

Astron. Astrophys. Suppl. Ser.

292

441

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Abstract. -A catalogue of supernova remnants in the southern Galaxy within the area 245• ≤ l ≤ 355• , |b| ∼ < 1.5• has been produced from observations made at 0.843 GHz with a resolution of 43 using the Molonglo Observatory Synthesis Telescope (MOST). The catalogue, presented here, provides greyscale images and contour maps of known and newly-discovered remnants. The increased resolution and sensitivity of these observations has resulted in better statistics for southern remnants.

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Section: Msca Sourcesmentioning

confidence: 71%

Section: Msca Sourcesmentioning

confidence: 96%

The MOST supernova remnant catalogue (MSC)

Whiteoak

Green

1996

Astron. Astrophys. Suppl. Ser.

292

441

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“…It is a rough circular SNR with a diameter of ∼30 from the radio observations (Caswell et al 1981), and a PWN powered by an energetic pulsar PSR B1509-58 (e.g., Gaensler et al 2002) was discovered in the remnant. Livingstone et al (2005) presented an updated timing solution for the young energetic pulsar PSR B1509-58 based on the 21.3 yr of radio data and the 7.6 yr of X-ray timing data.…”

Section: Msh 15-52mentioning

confidence: 99%

“…MSH 15-52 is a complex SNR with a ragged shell in the radio observations (Caswell et al 1981). An elongated PWN powered by an energetic pulsar was found in the remnant in the X-ray observations with ROSAT (Trussoni et al 1996), BeppoSAX (Mineo et al 2001) and Chandra .…”

Section: Introductionmentioning

confidence: 99%

Multiband emission from pulsar wind nebulae: a possible injection spectrum

Fang¹,

Zhang²

2010

A&A

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Aims. Recent research shows that particles with a spectrum of a relativistic Maxwellian plus a high-energy tail can be accelerated by relativistic collisionless shocks. We investigate the possibility of the high-energy particles with this new spectrum injected into pulsar wind nebulae (PWNe) from the terminate shock based on the study of multiwavelength emission from PWNe. Methods. The dynamics of a supernova remnant (SNR) and multiband nonthermal emission from the PWN inside the remnant are investigated using a dynamical model with electrons/positrons injected with the new spectrum. In this model, the dynamical and radiative evolution of a pulsar wind nebula in a nonradiative supernova remnant can be described self-consistently. Results. This model is applied to the three composite SNRs, G0.9+0.1, MSH 15-52, G338.3-0.0, and the multiband observed emission from the three PWNe is reproduced. Conclusions. Our studies on the three remnants provide evidence of a new spectrum of the particles, which are accelerated by the terminate shock and injected into a PWN.

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“…The composite supernova remnant MSH 15−52 (SNR G320.4−1.2 [14]) is usually associated to the radio pulsar PSR B1509−58. Einstein X-ray observations of MSH 15−52 revealed the existence of an elongated non-thermal PWN centered on the pulsar [24].…”

Section: The Pwn In Msh 15-52mentioning

confidence: 99%

Recent detections of TeV Pulsar Wind Nebulae with the Fermi-Large Area Telescope

Grondin¹,

Lemoine‐Goumard²

2011

Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)

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Prior to the Fermi Gamma-ray Space Telescope, only six pulsars and one associated Pulsar Wind Nebula (PWN), the Crab Nebula, had been detected in γ-rays by the CGRO-EGRET experiment. Since then, the Large Area Telescope (LAT) aboard Fermi has significantly increased the number of detected pulsars in the 100 MeV to 300 GeV energy range. A large fraction of these pulsars, characterized by high energy loss rates (Ė from ∼ 3 × 10 33 to ∼ 5 × 10 38 erg/s), is associated to PWNe or candidates observed in the TeV energy range and are likely to power a PWN detectable in the Fermi-LAT energy range, as done for the Crab. Here, we will review the recent results obtained with the Fermi-LAT on TeV Pulsar Wind Nebulae, including the Crab Nebula, Vela-X and MSH 15-52, HESS J1825-137, and give a general overview of the constraints provided by Fermi-LAT non-detections.

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High-resolution radio observations of five supernova remnants

Cited by 52 publications

References 0 publications

The MOST supernova remnant catalogue (MSC)

The MOST supernova remnant catalogue (MSC)

Multiband emission from pulsar wind nebulae: a possible injection spectrum

Recent detections of TeV Pulsar Wind Nebulae with the Fermi-Large Area Telescope

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