A new oxygen-rich supernova remnant in the Large Magellanic Cloud

1980 ◽  
Vol 242 ◽  
pp. L73 ◽  
Author(s):  
D. S. Mathewson ◽  
M. A. Dopita ◽  
I. R. Tuohy ◽  
V. L. Ford
Keyword(s):  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals New optically identified supernova remnants in the Large Magellanic Cloud

2020 ◽  
Vol 500 (2) ◽  
pp. 2336-2358
Author(s):  
Miranda Yew ◽  
Miroslav D Filipović ◽  
Milorad Stupar ◽  
Sean D Points ◽  
Manami Sasaki ◽  
...  
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Narrow Band Imaging ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Main Body ◽  
Found Objects ◽  
Type Ia ◽  
Optical Sample

ABSTRACT We present a new optical sample of three Supernova Remnants (SNRs) and 16 Supernova Remnant (SNR) candidates in the Large Magellanic Cloud (LMC). These objects were originally selected using deep H α, [S ii], and [O iii] narrow-band imaging. Most of the newly found objects are located in less dense regions, near or around the edges of the LMC’s main body. Together with previously suggested MCSNR J0541–6659, we confirm the SNR nature for two additional new objects: MCSNR J0522–6740 and MCSNR J0542–7104. Spectroscopic follow-up observations for 12 of the LMC objects confirm high [S ii]/H α emission-line ratios ranging from 0.5 to 1.1. We consider the candidate J0509–6402 to be a special example of the remnant of a possible type Ia Supernova (SN) which is situated some 2° (∼1.75 kpc) north from the main body of the LMC. We also find that the SNR candidates in our sample are significantly larger in size than the currently known LMC SNRs by a factor of ∼2. This could potentially imply that we are discovering a previously unknown but predicted, older class of large LMC SNRs that are only visible optically. Finally, we suggest that most of these LMC SNRs are residing in a very rarefied environment towards the end of their evolutionary span where they become less visible to radio and X-ray telescopes.

scholarly journals FORBIDDEN IRON LINES AND DUST DESTRUCTION IN SUPERNOVA REMNANT SHOCKS: THE CASE OF N49 IN THE LARGE MAGELLANIC CLOUD

2016 ◽  
Vol 826 (2) ◽  
pp. 150 ◽  
Author(s):  
Michael A. Dopita ◽  
Ivo R. Seitenzahl ◽  
Ralph S. Sutherland ◽  
Frédéric P. A. Vogt ◽  
P. Frank Winkler ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Dust Destruction

scholarly journals Multiwavelength study of the newly confirmed supernova remnant MCSNR J0527−7104 in the Large Magellanic Cloud

2013 ◽  
Vol 549 ◽  
pp. A99 ◽  
Author(s):  
P. J. Kavanagh ◽  
M. Sasaki ◽  
S. D. Points ◽  
M. D. Filipović ◽  
P. Maggi ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals Multifrequency radio observations of a SNR in the LMC: The case of SNR J0527-6549 (DEM l204)

2010 ◽  
pp. 43-49 ◽  
Author(s):  
L.M. Bozzetto ◽  
M.D. Filipovic ◽  
E.J. Crawford ◽  
I.S. Bojicic ◽  
J.L. Payne ◽  
...  
Keyword(s):  
Spectral Index ◽  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
High Order ◽  
Older Age ◽  
Radio Observations ◽  
Large Size ◽  
Peak Value ◽  
Compact Array

We present a detailed study and results of new Australia Telescope Compact Array (ATCA) observations of supernova remnant SNR J0527-6549. This Large Magellanic Cloud (LMC) object follows a typical supernova remnant (SNR) horseshoe morphology with a diameter of D=(66?58)?1 pc which is among the largest SNRs in the LMC. Its relatively large size indicates older age while a steeper than expected radio spectral index of ?=-0.92?0.11 is more typical of younger and energetic SNRs. Also, we report detections of regions with a high order of polarization at a peak value of ~54%?17% at 6 cm.

scholarly journals Multifrequency study of the Large Magellanic Cloud supernova remnant J0529−6653 near pulsar B0529-66

2012 ◽  
Vol 420 (3) ◽  
pp. 2588-2595 ◽  
Author(s):  
L. M. Bozzetto ◽  
M. D. Filipović ◽  
E. J. Crawford ◽  
F. Haberl ◽  
M. Sasaki ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals A DEEPCHANDRAOBSERVATION OF THE OXYGEN-RICH SUPERNOVA REMNANT 0540-69.3 IN THE LARGE MAGELLANIC CLOUD

2010 ◽  
Vol 710 (2) ◽  
pp. 948-957 ◽  
Author(s):  
Sangwook Park ◽  
John P. Hughes ◽  
Patrick O. Slane ◽  
Koji Mori ◽  
David N. Burrows
Keyword(s):  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals Multifrequency study of the Large Magellanic Cloud supernova remnant (SNR) B0513−692 and new SNR candidate J051327−6911

2007 ◽  
Vol 378 (4) ◽  
pp. 1237-1247 ◽  
Author(s):  
I. S. Bojičić ◽  
M. D. Filipović ◽  
Q. A. Parker ◽  
J. L. Payne ◽  
P. A. Jones ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals [ITAL]Far Ultraviolet Spectroscopic Explorer[/ITAL] Observations of the Supernova Remnant N49 in the Large Magellanic Cloud

2000 ◽  
Vol 538 (1) ◽  
pp. L61-L64 ◽  
Author(s):  
William P. Blair ◽  
Ravi Sankrit ◽  
Robin Shelton ◽  
Kenneth R. Sembach ◽  
H. Warren Moos ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Far Ultraviolet

scholarly journals The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud

2021 ◽  
Vol 163 (1) ◽  
pp. 30
Author(s):  
Chuan-Jui Li ◽  
You-Hua Chu ◽  
Chen-Yu Chuang ◽  
Guan-Hong Li
Keyword(s):  
Large Scale ◽  
Supernova Remnant ◽  
Ambient Medium ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Low Density ◽  
Energy Feedback ◽  
Stellar Ages ◽  
Nonthermal Radio Emission ◽  
Stellar Masses

Abstract The supernova remnant (SNR) B0532−67.5 in the Large Magellanic Cloud (LMC) was first diagnosed by its nonthermal radio emission, and its SNR nature was confirmed by the observation of diffuse X-ray emission; however, no optical SNR shell is detected. The OB association LH75, or NGC 2011, is projected within the boundary of this SNR. We have analyzed the massive star population in and around SNR B0532−67.5 using optical photometric data to construct color–magnitude diagrams, using stellar evolutionary tracks to estimate stellar masses, and using isochrones to assess the stellar ages. From these analyses, we find a 20–25 Myr population in LH75 and a younger population less than 10 Myr old to the southwest of LH75. The center of SNR B0532−67.5 is located closer to the core of LH75 than to the massive stars to its southwest. We conclude that the supernova progenitor was probably a member of LH75 with an initial mass of ∼15 M ⊙. The supernova exploded in an H i cavity excavated by the energy feedback of LH75. The low density of the ambient medium prohibits the formation of a visible nebular shell. Despite the low density in the ambient medium, physical properties of the hot gas within the SNR interior do not differ from SNRs with a visible shell by more than a factor of 2–3. The large-scale H i map shows that SNR B0532−67.5 is projected in a cavity that appears to be connected with the much larger cavity of the supergiant shell LMC-4.

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