Supernova Remnants in the Magellanic Clouds

Bozzetto, L. M.; Filipović, Miroslav; Haberl, F.; Sasaki, M.; Kavanagh, Patrick; Maggi, Pierre; Urošević, D.; Sturm, R.

doi:10.5303/pkas.2015.30.2.149

Cited by 4 publications

(2 citation statements)

References 25 publications

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“…Some recent studies include: Bojičić et al (2007), Cajko et al (2009), Crawford et al (2008Crawford et al ( , 2010Crawford et al ( , 2014, Bozzetto et al (2010), Grondin et al (2012), Bozzetto et al (2012d,b,a,c), de Horta et al (2012);De Horta et al (2014), Kavanagh et al (2013), Bozzetto et al (2013), Brantseg et al (2014), Bozzetto et al (2014b,a); Bozzetto & Filipović (2014), Warth et al (2014), Maggi et al (2014), Reid et al (2015), Kavanagh et al (2015a,b,c), Bozzetto et al (2015) and Kavanagh et al (2016).…”

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Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Bozzetto

Filipović

Vukotić

et al. 2017

ApJS

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We construct the most complete sample of supernova remnants (SNRs) in any galaxy -the Large Magellanic Cloud (LMC) SNR sample. We study their various properties such as spectral index (α), size and surface-brightness. We suggest an association between the spatial distribution, environment density of LMC SNRs and their tendency to be located around supergiant shells. We find evidence that the 16 known type Ia LMC SNRs are expanding in a lower density environment compared to the Core-Collapse (CC) type. The mean diameter of our entire population (74) is 41 pc, which is comparable to nearby galaxies. We didn't find any correlation between the type of SN explosion, ovality or age. The N (< D) relationship of a = 0.96 implies that the randomised diameters are readily mimicking such an exponent. The rate of SNe occurring in the LMC is estimated to be ∼1 per 200 yr. The mean α of the entire LMC SNR population is α=-0.52, which is typical of most SNRs. However, our estimates show a clear flattening of the synchrotron α as the remnants age. As predicted, our CC SNRs sample are significantly brighter radio emitters than the type Ia remnants. We also estimate the Σ − D relation for the LMC to have a slope ∼3.8 which is comparable with other nearby galaxies. We also find the residency time of electrons in the galaxy

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confidence: 99%

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Bozzetto

Filipović

Vukotić

et al. 2017

ApJS

Self Cite

111

158

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“…Apart from the above mentioned LMC SNR survey papers, there are a number of studies focusing on particular LMC SNRs, such as N 103B and N 132D. Some recent studies include: Bojičić et al (2007); Cajko et al (2009); Crawford et al (2008Crawford et al ( , 2010; Crawford et al (2014a); Bozzetto et al (2010); Grondin et al (2012); Bozzetto et al (2017); de Horta et al (2012); De Horta et al (2014); Kavanagh et al (2013); Brantseg et al (2014); Kavanagh et al (2016Kavanagh et al ( , 2015c; Reid et al (2015); Maggi et al (2014); Warth et al (2014); ; Bozzetto et al (2015Bozzetto et al ( , 2013Bozzetto et al ( , 2014a; ; Bozzetto et al (2014bBozzetto et al ( , 2012a; Leahy (2017); Ghavamian et al (2017); Dopita et al (2018); Maitra et al (2019); Alsaberi et al (2019a); Seitenzahl et al (2019); Leahy et al (2019); Pennock et al (2020).…”

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New Optically Identified Supernova Remnants in the Large Magellanic Cloud

Yew,

Filipović,

Stupar

et al. 2020

Preprint

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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 H𝛼, [S ] and [O ] 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 ]/H𝛼 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.

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Radio emission from interstellar shocks: Young type Ia supernova remnants and the case of N 103B in the Large Magellanic Cloud

Alsaberi

Barnes

Filipović

et al. 2019

Astrophys Space Sci

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We investigate young type Ia supernova remnants (SNRs) in our Galaxy and neighbouring galaxies in order to understand their properties and early stage of their evolution. Here we present a radio continuum study based on new and archival data from the Australia Telescope Compact Array (ATCA) towards N 103B, a young (≤1000 yrs) spectro-This article belongs to the Topical Collection: Plasma, Particles, and Photons: ISM Physics Revisited.

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Supernova Remnants in the Magellanic Clouds

Cited by 4 publications

References 25 publications

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

New Optically Identified Supernova Remnants in the Large Magellanic Cloud

Radio emission from interstellar shocks: Young type Ia supernova remnants and the case of N 103B in the Large Magellanic Cloud

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