Radio-continuum study of MCSNR J0536–7038 (DEM L249)

Bozzetto, L. M.; Filipović, Miroslav

doi:10.1007/s10509-014-1825-y

Cited by 5 publications

(4 citation statements)

References 30 publications

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“…Our estimated peak fractional polarisation value is P = 5 ± 1 percent, while average polarisation is about ∼3 percent. This is unusually weak for a young SNR and very similar to earlier Dickel et al (1993) results, especially when compared to the range of other LMC SNRs that we observed over the past decades with ATCA (Bojičić et al 2007;Crawford et al 2008a,b;Cajko et al 2009;Crawford et al 2010;Bozzetto et al 2010Bozzetto et al , 2012aHaberl et al 2012;Bozzetto et al 2012dBozzetto et al , 2013Brantseg et al 2014;Bozzetto et al 2014a;Bozzetto & Filipović 2014;Bozzetto et al 2014b;Kavanagh et al 2015). Perhaps, significant depolarization within the 2 GHz bandwidth is present.…”

Section: Radio Continuumsupporting

confidence: 90%

ALMA CO Observations of Supernova Remnant N63A in the Large Magellanic Cloud: Discovery of Dense Molecular Clouds Embedded within Shock-ionized and Photoionized Nebulae

Sano

Matsumura

Nagaya

et al. 2019

ApJ

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We carried out new 12 CO(J = 1-0, 3-2) observations of a N63A supernova remnant (SNR) from the LMC using ALMA and ASTE. We find three giant molecular clouds toward the northeast, east, and near the center of the SNR. Using the ALMA data, we spatially resolved clumpy molecular clouds embedded within the optical nebulae in both the shock-ionized and photoionized lobes discovered by previous Hα and [S ii] observations. The total mass of the molecular clouds is ∼800 M ⊙ for the shockionized region and ∼1700 M ⊙ for the photoionized region. Spatially resolved X-ray spectroscopy reveals that the absorbing column densities toward the molecular clouds are ∼1.5-6.0 × 10 21 cm −2 , which are ∼1.5-15 times less than the averaged interstellar proton column densities for each region. This means that the X-rays are produced not only behind the molecular clouds, but also in front of them. We conclude that the dense molecular clouds have been completely engulfed by the shock waves, but have still survived erosion owing to their high-density and short interacting time. The X-ray spectrum toward the gas clumps is well explained by an absorbed power-law or high-temperature plasma models in addition to the thermal plasma components, implying that the shock-cloud interaction is efficiently working for both the cases through the shock ionization and magnetic field amplification. If the hadronic gamma-ray is dominant in the GeV band, the total energy of cosmic-ray protons is calculated to be ∼0.3-1.4 × 10 49 erg with the estimated ISM proton density of ∼190 ± 90 cm −3 , containing both the shock-ionized gas and neutral atomic hydrogen.

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Section: Radio Continuumsupporting

confidence: 90%

ALMA CO Observations of Supernova Remnant N63A in the Large Magellanic Cloud: Discovery of Dense Molecular Clouds Embedded within Shock-ionized and Photoionized Nebulae

Sano

Matsumura

Nagaya

et al. 2019

ApJ

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“…In comparison to other LMC SNRs arising from a Type Ia SNe, MCSNR J0506−7025 shows similar mean levels of fractional polarisation: MCSNR J0509-6731 with 26 ± 13% at 6 cm (Bozzetto et al 2014a); MCSNR J0533-7202 with 12 ± 7% (Bozzetto et al 2013); MCSNR J0536-7038 with 35 ± 8% (Bozzetto & Filipović 2014); while MCSNR J0519-6902 exhibited a much lower mean fractional polarisation at a level of 2.2 and 3.2% at 6 and 3 cm, respectively (Bozzetto et al 2012). …”

Section: Magnetic Fieldmentioning

confidence: 76%

Two evolved supernova remnants with newly identified Fe-rich cores in the Large Magellanic Cloud

Kavanagh

Sasaki

Bozzetto

et al. 2016

A&A

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Aims. We present a multi-wavelength analysis of the evolved supernova remnants MCSNR J0506−7025 and MCSNR J0527−7104 in the Large Magellanic Cloud. Methods. We used observational data from XMM-Newton, the Australian Telescope Compact Array, and the Magellanic Cloud Emission Line Survey to study their broad-band emission and used Spitzer and H  data to gain a picture of the environment into which the remnants are expanding. We performed a multi-wavelength morphological study and detailed radio and X-ray spectral analyses to determine their physical characteristics. Results. Both remnants were found to have bright X-ray cores, dominated by Fe L-shell emission, which is consistent with reverse shock-heated ejecta with determined Fe masses in agreement with Type Ia explosion yields. A soft X-ray shell, which is consistent with swept-up interstellar medium, was observed in MCSNR J0506−7025, suggestive of a remnant in the Sedov phase. Using the spectral fit results and the Sedov self-similar solution, we estimated the age of MCSNR J0506−7025 to be ∼16−28 kyr, with an initial explosion energy of (0.07−0.84) × 10 51 erg. A soft shell was absent in MCSNR J0527−7104, with only ejecta emission visible in an extremely elongated morphology that extends beyond the optical shell. We suggest that the blast wave has broken out into a low density cavity, allowing the shock heated ejecta to escape. We find that the radio spectral index of MCSNR J0506−7025 is consistent with the standard −0.5 for supernova remnants. Radio polarisation at 6 cm indicates a higher degree of polarisation along the western front and at the eastern knot with a mean fractional polarisation across the remnant of P (20 ± 6)%. Conclusions. The detection of Fe-rich ejecta in the remnants suggests that both resulted from Type Ia explosions. The newly identified Fe-rich cores in MCSNR J0506−7025 and MCSNR J0527−7104 make them members of the expanding class of evolved Fe-rich remnants in the Magellanic Clouds.

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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).…”

mentioning

confidence: 99%

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Bozzetto

Filipović

Vukotić

et al. 2017

ApJS

115

158

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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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Radio-continuum study of MCSNR J0536–7038 (DEM L249)

Cited by 5 publications

References 30 publications

ALMA CO Observations of Supernova Remnant N63A in the Large Magellanic Cloud: Discovery of Dense Molecular Clouds Embedded within Shock-ionized and Photoionized Nebulae

ALMA CO Observations of Supernova Remnant N63A in the Large Magellanic Cloud: Discovery of Dense Molecular Clouds Embedded within Shock-ionized and Photoionized Nebulae

Two evolved supernova remnants with newly identified Fe-rich cores in the Large Magellanic Cloud

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

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