Supernova 1987A: radiosphere resolved with VLBI five days after the neutrino burst

Jauncey, D. L.; Kemball, A. J.; Bartel, N.; Whitney, A. R.; Rogers, A. E. E.; Shapiro, I. I.; Preston, R. A.; Clark, T. A.; Harvey, Bruce; Jones, D. L.; Nicolson, G. D.; Nothnagel, A.; Phillips, R. B.; Reynolds, J. E.; Webber, J. C.

doi:10.1038/334412a0

Cited by 21 publications

(15 citation statements)

References 25 publications

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“…At these early epochs. Ha and radio VLBI observations both indicate that the shock velocity was « 19 000 -30 000 km s ^ ^ [8,9]. Dihgent radio monitoring over subsequent years was rewarded in mid-1990, when the MOST redetected radio emission from SN 1987A.…”

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confidence: 96%

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Fifteen Years of High-Resolution Radio Imaging of Supernova 1987A

Gaensler¹,

Manchester²,

Kesteven³

et al. 2007

AIP Conference Proceedings

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Supernova 1987A in the Large Magellanic Cloud provides a spectacularly detailed view of the aftermath of a core-collapse explosion. The supernova ejecta initially coasted outward at more than 10% of the speed of light, but in 1990 were observed to decelerate rapidly as they began to encounter dense circumstellar material expelled by the progenitor star. The resulting shock has subsequently produced steadily brightening radio synchrotron emission, which is resolved by the Australia Telescope Compact Array (ATCA) into an expanding limb-brightened shell. Here we present 15 years of ATCA imaging of Supernova 1987A, at an effective angular resolution of 0.4 arcsec. We find that the radio remnant has accelerated in its expansion over this period, from approx 3600 km/s in 1992 to approx 5200 km/s at the end of 2006. The published diameters of the evolving X-ray shell have been ~15% smaller than the corresponding radio values, but a simultaneous Fourier analysis of both radio and X-ray data eliminates this discrepancy, and yields a current diameter for the shell in both wave-bands of approx 1.7 arcsec. An asymmetric brightness distribution is seen in radio images at all ATCA epochs: the eastern and western rims have higher fluxes than the northern and southern regions, indicating that most of the radio emission comes from the equatorial plane of the system, where the progenitor star's circumstellar wind is thought to be densest. The eastern lobe is brighter than and further from the supernova site than the western lobe, suggesting an additional asymmetry in the initial distribution of supernova ejecta.Comment: 10 pages, including 7 b/w + 1 color embedded EPS figures; uses aipproc.cls . To appear in "Supernova 1987A: Twenty Years After: Supernovae and Gamma-Ray Bursters", edited by S. Immler, K. W. Weiler and R. McCray, American Institute of Physics, New York, 2007, in press. Updated figure

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confidence: 96%

“…9 GHz diffraction limited images of SN 1987A over 14 years of ATCA observations. Each panel is labeled with its corresponding epoch; the same linear greyscale range, between -0.2 and +30 mJy beam^\ is used in each panel.…”

mentioning

confidence: 99%

Fifteen Years of High-Resolution Radio Imaging of Supernova 1987A

Gaensler¹,

Manchester²,

Kesteven³

et al. 2007

AIP Conference Proceedings

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“…In contrast, the average expansion speed between 1987 and 1991 was about 35,000 km s −1 (cf. Jauncey et al 1988). Comparison of four images obtained between 1992 and 1995 showed that the brightness of the lobes increased relative to that of the spherical shell and that the asymmetry between the east and west lobes increased markedly over this period (Gaensler et al 1997).…”

Section: Introductionmentioning

confidence: 99%

Evolution of the Radio Remnant of SN 1987A: 1990-2001

Manchester

Gaensler

Wheaton

et al. 2002

Publ. – Astron. Soc. Aust

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The development of the radio remnant of SN 1987A has been followed using the Australia Telescope Compact Array since its first detection in 1990 August. The remnant has been observed at four frequencies, 1.4, 2.4, 4.8, and 8.6 GHz, at intervals of 4–6 weeks since the first detection. These data are combined with the 843 MHz data set of Ball et al. (2001) obtained at Molonglo Observatory to study the spectral and temporal variations of the emission. These observations show that the remnant continues to increase in brightness, with a larger rate of increase at recent times. They also show that the radio spectrum is becoming flatter, with the spectral index changing from −0.97 to −0.88 over the 11 years. In addition, at roughly yearly intervals since 1992, the remnant has been imaged at 9 GHz using super-resolution techniques to obtain an effective synthesised beamwidth of about 0″.5. The imaging observations confirm the shell morphology of the radio remnant and show that it continues to expand at ˜3000 km s−1. The bright regions of radio emission seen on the limb of the shell do not appear to be related to the optical hot spots which have subsequently appeared in surrounding circumstellar material.

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“…On 1987 February 25, Turtle et al (1987) Jauncey et al (1988) used VLBI techniques to resolve the expanding radiosphere. Continued observations saw the SN fade from its initial radio burst to almost undetectable levels within a few months (Turtle et al 1987).…”

Section: Introductionmentioning

confidence: 99%

HIGH RESOLUTION 36 GHz IMAGING OF THE SUPERNOVA REMNANT OF SN 1987A

Potter

Ball

et al. 2009

ApJ

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The aftermath of supernova (SN) 1987A continues to provide spectacular insights into the interaction between an SN blastwave and its circumstellar environment. We here present 36 GHz observations from the Australia Telescope Compact Array of the radio remnant of SN 1987A. These new images, taken in 2008 April and 2008 October, substantially extend the frequency range of an ongoing monitoring and imaging program conducted between 1.4 and 20 GHz. Our 36.2 GHz images have a diffraction-limited angular resolution of 0. 3-0. 4, which covers the gap between high resolution, low dynamic range VLBI images of the remnant and low resolution, high dynamic range images at frequencies between 1 and 20 GHz. The radio morphology of the remnant at 36 GHz is an elliptical ring with enhanced emission on the eastern and western sides, similar to that seen previously at lower frequencies. Model fits to the data in the Fourier domain show that the emitting region is consistent with a thick inclined torus of mean radius 0. 85, and a 2008 October flux density of 27 ± 6 mJy at 36.2 GHz. The spectral index for the remnant at this epoch, determined between 1.4 GHz and 36.2 GHz, is α = −0.83. There is tentative evidence for an unresolved central source with flatter spectral index.

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Supernova 1987A: radiosphere resolved with VLBI five days after the neutrino burst

Cited by 21 publications

References 25 publications

Fifteen Years of High-Resolution Radio Imaging of Supernova 1987A

Fifteen Years of High-Resolution Radio Imaging of Supernova 1987A

Evolution of the Radio Remnant of SN 1987A: 1990-2001

HIGH RESOLUTION 36 GHz IMAGING OF THE SUPERNOVA REMNANT OF SN 1987A

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