Multi-frequency observations of SNR J0453–6829 in the LMC

Haberl, F.; Filipović, Miroslav; Bozzetto, L. M.; Crawford, E. J.; Points, Sean; Pietsch, W.; Horta, A. Y. De; Tothill, N.; Payne, Jeffrey L.; Sasaki, M.

doi:10.1051/0004-6361/201218971

Cited by 27 publications

(31 citation statements)

References 44 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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“…This depolarisation may also indicate somewhat older age of the remnant. The noticeably younger PWNe in the LMC such as N157B (Lazendic et al 2000), SNR J0453-6829 (Haberl et al 2012a), and 0540-69.3 (Brantseg et al 2014) all have strong polarisation.…”

Section: Radiomentioning

confidence: 99%

IKT 16: the first X-ray confirmed composite SNR in the SMC

Maitra

Ballet

Filipović

et al. 2015

A&A

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Aims. IKT 16 is an X-ray and radio-faint supernova remnant (SNR) in the Small Magellanic Cloud (SMC). A detailed X-ray study of this SNR with XMM-Newton confirmed the presence of a hard X-ray source near its centre, indicating the detection of the first composite SNR in the SMC. With a dedicated Chandra observation we aim to resolve the point source and confirm its nature. We also acquire new ATCA observations of the source at 2.1 GHz with improved flux density estimates and resolution. Methods. We perform detailed spatial and spectral analysis of the source. With the highest resolution X-ray and radio image of the centre of the SNR available today, we resolve the source and confirm its pulsar wind nebula (PWN) nature. Further, we constrain the geometrical parameters of the PWN and perform spectral analysis for the point source and the PWN separately. We also test for the radial variations of the PWN spectrum and its possible east west asymmetry. Results. The X-ray source at the centre of IKT 16 can be resolved into a symmetrical elongated feature centring a point source, the putative pulsar. Spatial modelling indicates an extent of 5.2 of the feature with its axis inclined at 82• east from north, aligned with a larger radio feature consisting of two lobes almost symmetrical about the X-ray source. The picture is consistent with a PWN which has not yet collided with the reverse shock. The point source is about three times brighter than the PWN and has a hard spectrum of spectral index 1.1 compared to a value 2.2 for the PWN. This points to the presence of a pulsar dominated by non-thermal emission. The expectedĖ is ∼10 37 erg s −1 and spin period <100 ms. However, the presence of a compact nebula unresolved by Chandra at the distance of the SMC cannot completely be ruled out.

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“…Ages for the first three type Ia SNRs are from light echo measurements (Rest et al 2005). ( have been found in MCSNR J0453−6829 (Gaensler et al 2003;Haberl et al 2012a) and in MCSNR J0535−6602 . In the latter, the case for a PWN is not as strong; however, analysis of the X-ray morphology using a power-ratio method (Lopez et al 2009) confirm the classification as CC-SNR.…”

Section: Appendix A: the Epic Backgroundmentioning

confidence: 99%

The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

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Aims. We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). Using primarily XMM-Newton observations, we conduct a systematic spectral analysis of LMC SNRs to gain new insight into their evolution and the interplay with their host galaxy. Methods. We combined all the archival XMM-Newton observations of the LMC with those of our Very Large Programme LMC survey. We produced X-ray images and spectra of 51 SNRs, out of a list of 59 objects compiled from the literature and augmented with newly found objects. Using a careful modelling of the background, we consistently analysed all the X-ray spectra and measure temperatures, luminosities, and chemical compositions. The locations of SNRs are compared to the distributions of stars, cold gas, and warm gas in the LMC, and we investigated the connection between the SNRs and their local environment, characterised by various star formation histories. We tentatively typed all LMC SNRs, in order to constrain the ratio of core-collapse to type Ia SN rates in the LMC. We also compared the column densities derived from X-ray spectra to H i maps, thus probing the three-dimensional structure of the LMC. Results. This work provides the first homogeneous catalogue of the X-ray spectral properties of SNRs in the LMC. It offers a complete census of LMC remnants whose X-ray emission exhibits Fe K lines (13% of the sample), or reveals the contribution from hot supernova ejecta (39%), which both give clues to the progenitor types. The abundances of O, Ne, Mg, Si, and Fe in the hot phase of the LMC interstellar medium are found to be between 0.2 and 0.5 times the solar values with a lower abundance ratio [α/Fe] than in the Milky Way. The current ratio of core-collapse to type Ia SN rates in the LMC is constrained to N CC /N Ia = 1.35( +0.11 −0.24 ), which is lower than in local SN surveys and galaxy clusters. Our comparison of the X-ray luminosity functions of SNRs in Local Group galaxies (LMC, SMC, M31, and M33) reveals an intriguing excess of bright objects in the LMC. Finally, we confirm that 30 Doradus and the LMC Bar are offset from the main disc of the LMC to the far and near sides, respectively.

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Multi-frequency observations of SNR J0453–6829 in the LMC

Cited by 27 publications

References 44 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

IKT 16: the first X-ray confirmed composite SNR in the SMC

The population of X-ray supernova remnants in the Large Magellanic Cloud

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