Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Abstract

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

Discovery of a very young high-mass X-ray binary associated with the supernova remnant MCSNR J0513-6724 in the LMC

“…We report here the discovery of a new HMXB at the geometrical centre of MCSNR J0513-6724 , which is confirmed as an SNR for the first time in this work. MCSNR J0513-6724 was previously a candidate SNR in the LMC (Bozzetto et al 2017). It was first reported by Haberl & Pietsch (1999) recording an extent of 17.5 albeit a 'hard' hardness-ratio.…”

Kinematics: A Clean Diagnostic for Separating Supernova Remnants from H ii Regions in Nearby Galaxies

“…J#: as listed by Bozzetto et al (2017); B04: Blair & Long (2004); S03: Soria & Wu (2003) X-ray source number; D83: de Vaucouleurs et al (1983); M06: Maddox et al (2006) radio source.c Object center position adopted from that ofBozzetto et al (2017) for scans; slit center position for long slits; object coordinates for M83 objects.…”

Supernova remnants in nearby galaxies

“…Figure (left, Bozzetto et al ) shows Venn diagrams of the number of SNRs detected in different wavelength bands. Typically, SNRs are bright radio and X‐ray sources due to their shocks.…”

“…The thin dotted lines show the power-law fit (N(> L X ) ∝ L X ) to the XLFs. Taken from Maggi et al (2016) Figure 5 (left, Bozzetto et al 2017) shows Venn diagrams of the number of SNRs detected in different wavelength bands. Typically, SNRs are bright radio and X-ray sources due to their shocks.…”