scholarly journals Australia Telescope observations of the supernova remnant N49 in the LMC

1991 ◽  
Vol 148 ◽  
pp. 347-348
Author(s):  
Norbert Junkes
Keyword(s):  
High Resolution ◽  
Shell Structure ◽  
Supernova Remnant ◽  
Radio Image ◽  
Southeastern Part ◽  
X Ray ◽  
Northern Edge

We present the first high-resolution radio image of the supernova remnant N49 near the northern edge of the LMC. These observations with the Australia Telescope at 6cm wavelength (4 arcsec resolution) show a distinct radio shell. The shell structure of N49 is similar in radio and X-ray emission, with the maximum of the emission found in the southeastern part of the SNR.

scholarly journals N49: The Site of a Gamma-ray Burst. Preliminary Results from X-ray Observations

1983 ◽  
Vol 101 ◽  
pp. 573-577
Author(s):  
G. Pizzichini ◽  
T. L. Cline ◽  
U. D. Desai ◽  
B. J. Teegarden ◽  
W. D. Evans ◽  
...  
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
Gamma Ray ◽  
Large Magellanic Cloud ◽  
X Rays ◽  
Radio Image ◽  
Gamma Ray Burst ◽  
X Ray ◽  
Preliminary Results ◽  
Einstein Observatory

The error box of the unusual Gamma-Ray Burst of March 5, 1979 falls completely inside the optical and radio image of the Supernova Remnant N49 in the Large Magellanic Cloud. This region was observed twice in x-rays with the High Resolution Imager of the Einstein Observatory, six weeks and nearly two years after the Gamma-Ray Burst. We show the comparison between the two observations.

scholarly journals Radio imaging of the supernova remnant N132D in the Large Magellanic Cloud

1991 ◽  
Vol 148 ◽  
pp. 349-350
Author(s):  
John R. Dickel ◽  
D. K. Milne
Keyword(s):  
High Resolution ◽  
Shell Structure ◽  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Radio Image ◽  
Radio Imaging

The first high resolution radio image of the supernova remnant N132D shows a complex shell structure.

scholarly journals Detailed X-ray Observations of the Cygnus Loop

1983 ◽  
Vol 101 ◽  
pp. 253-260
Author(s):  
W. H.-M. Ku ◽  
K. Long ◽  
R. Pisarski ◽  
M. Vartanian
Keyword(s):  
High Resolution ◽  
Proportional Counter ◽  
Supernova Remnant ◽  
Sounding Rocket ◽  
Loop Structure ◽  
High Quality ◽  
Radio Structure ◽  
X Ray ◽  
Cygnus Loop ◽  
Spatially Resolved

High quality X-ray spectral and imaging observations of the Cygnus Loop have been obtained with three different instruments. The High Resolution Imager (HRI) on the Einstein Observatory was used to obtain arcsecond resolution images of select bright regions in the Cygnus Loop which permit detailed comparisons between the X-ray, optical, and radio structure of the Loop. The Imaging Proportional Counter (IPC) on the Einstein Observatory was used to obtain an arcminute resolution map of essentially the full Loop structure. Finally, an Imaging Gas Scintillation Proportional Counter (IGSPC), carried aloft by a sounding rocket last fall, obtained modest resolution, spatially resolved spectrophotometry of the Cygnus Loop. An X-ray map of the Loop in the energy of the 0 VIII line was obtained. These data combine to yield a very powerful probe of the abundance, temperature, and density distribution of material in the supernova remnant, and in the interstellar medium.

scholarly journals Non-Equilibrium Ionization in Puppis A

1983 ◽  
Vol 101 ◽  
pp. 245-252
Author(s):  
P. F. Winkler ◽  
C. R. Canizares ◽  
B. C. Bromley
Keyword(s):  
High Resolution ◽  
Spectroscopic Data ◽  
Supernova Remnant ◽  
Optical Data ◽  
Equilibrium Conditions ◽  
X Ray ◽  
Flux Measurements ◽  
Far From Equilibrium ◽  
Einstein Observatory ◽  
Non Equilibrium

High resolution X-ray spectroscopy of the brightest knot of emission in the Puppis A supernova remnant shows that it is made up of ionizing plasma, far from equilibrium. Flux measurements in several X-ray lines enable us to determine the non-equilibrium conditions: electron temperature, ion populations, and time since the knot was heated by the supernova shock. Imaging and spectroscopic data from the Einstein Observatory together suggest that this knot is a cloud of density about 10 cm−3 which has recently been shocked to a temperature 7 × 106 K. Radio and optical data on the region appear consistent with this picture.

The mass of Tycho's supernova remnant as determined from a high-resolution X-ray map

1983 ◽  
Vol 266 ◽  
pp. 287 ◽  
Author(s):  
F. Seward ◽  
P. Gorenstein ◽  
W. Tucker
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
X Ray

scholarly journals HESS J1858+020: A GeV-TeV source possibly powered by cosmic rays from SNR G35.6-0.4

2021 ◽  
Vol 646 ◽  
pp. A114
Author(s):  
Y. Cui ◽  
Y. Xin ◽  
S. Liu ◽  
P. H. T. Tam ◽  
G. Pühlhofer ◽  
...  
Keyword(s):  
Diffusion Coefficient ◽  
Cosmic Rays ◽  
Power Law ◽  
Supernova Remnant ◽  
Observational Evidence ◽  
X Ray ◽  
Multi Wavelength ◽  
Northern Edge ◽  
Cloud Complex ◽  
Hadronic Model

Context. The supernova remnant (SNR) G35.6−0.4 shows a non-thermal radio shell, however, no γ-ray or X-ray counterparts have been found for it thus far. One TeV source, HESS J1858+020, was found near the SNR and this source is spatially associated with some clouds at 3.6 kpc. Aims. To attain a better understanding of the origin of HESS J1858+020, we further investigate the association between SNR cosmic rays (CRs) and the clouds through the Fermi-LAT analysis and hadronic modeling. Methods. We performed the Fermi-LAT analysis to explore the GeV emission in and around the SNR. We explored the SNR physics with previously observed multi-wavelength data. We built a hadronic model using runaway CRs of the SNR to explain the GeV-TeV observation. Results. We found a hard GeV source (SrcX2) that is spatially coincident with both HESS J1858+020 and a molecular cloud complex at 3.6 kpc. In addition, a soft GeV source (SrcX1) was found at the northern edge of the SNR. The GeV spectrum of SrcX2 connects well with the TeV spectrum of HESS J1858+020. The entire γ-ray spectrum ranges from several GeV up to tens of TeV and it follows a power-law with an index of ~2.15. We discuss several pieces of observational evidence to support the middle-aged SNR argument. Using runaway CRs from the SNR, our hadronic model explains the GeV-TeV emission at HESS J1858+020, with a diffusion coefficient that is much lower than the Galactic value.

High-resolution radio and X-ray observations of the supernova remnant W28

1983 ◽  
Vol 266 ◽  
pp. 684 ◽  
Author(s):  
M. D. Andrews ◽  
J. P. Basart ◽  
R. C. Lamb ◽  
R. H. Becker
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
X Ray

scholarly journals X-ray Observations of SNR E0102.2-72.2 in the SMC

1988 ◽  
Vol 101 ◽  
pp. 125-128
Author(s):  
John P. Hughes
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Spectral Data ◽  
Proportional Counter ◽  
High Velocity ◽  
Supernova Remnant ◽  
Optical Emission ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
Best Fit

AbstractThe supernova remnant (SNR) E0102.2-72.2 is the brightest in the Small Magellanic Cloud (SMC) at X-ray wavelengths. This object, which is remarkable because of its high velocity (∼4000 km s−1) oxygen-rich optical emission, appears to be similarly remarkable at X-ray wavelengths. The high resolution imager (HRI) data can be quite well described by a thick ring with a radius of ∼19" (6 pc at a distance of 63 kpc). The imaging proportional counter (IPC) X-ray spectral data can be best fit by a single emission line of energy ∼0.9 keV. It seems likely that this is the emission from a plasma of almost pure neon.

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