Multifrequency study of a new Fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508−6902

Bozzetto, L. M.; Kavanagh, Patrick; Maggi, Pierre; Filipović, Miroslav; Stupar, M.; Parker, Quentin A.; Reid, Warren A.; Sasaki, M.; Haberl, F.; Urošević, D.; Dickel, John R.; Sturm, R.; Williams, Robert J.; Ehle, M.; Gruendl, R. A.; Chu, You‐Hua; Points, Sean; Crawford, E. J.

doi:10.1093/mnras/stu051

Cited by 21 publications

(41 citation statements)

References 100 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Green symbols represent confirmed remnants, while blue symbols show the position of candidate remnants. Bozzetto et al (2014b, Figure 2), where the radio (5500 MHz) and optical (Hα) emission form the 'ring' of emission inside which the X-ray (0.7−1.1 keV) emission resides. The major and minor axes, in addition to the position angle of these measurements, are listed in Tables 1 and 2.…”

Section: Differential Size Distributionmentioning

confidence: 99%

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Bozzetto

Filipović

Vukotić

et al. 2017

ApJS

116

158

View full text Add to dashboard Cite

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

show abstract

Section: Differential Size Distributionmentioning

confidence: 99%

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Bozzetto

Filipović

Vukotić

et al. 2017

ApJS

116

158

View full text Add to dashboard Cite

show abstract

“…The shell A of DEM L316 (MCSNR J0547−6941) has striking spectral differences to the very close neighbour MCSNR J0547−6943 (DEM L316B): the former is also mostly exhibiting Fe L-shell emission, which leads to the interpretation that it is another type Ia remnant (Nishiuchi et al 2001;. Then come three more evolved (age 15 kyr) iron-rich SNRs that were presented in Maggi et al (2014) and Bozzetto et al (2014). Finally, since these publications, we obtained XMM-Newton follow-up observations of two remnants, which we classified as type Ia: i) MCSNR J0506−7026 was a ROSATselected candidate ([HP99] 1139), which revealed a remnant similar to DEM L238 and L249, about 17−21 kyr old and holding about 0.9 M −1 M in the central region (Kavanagh et al, in prep., Table E.1); ii) MCSNR J0527−7104 was confirmed by our group in a multi-wavelength study (Kavanagh et al 2013).…”

Section: B1 Type Ia Snrsmentioning

confidence: 99%

“…For instance, the SNR N132D is used as a calibration source and regularly observed; also SN 1987A is frequently monitored (Heng et al 2008;Maggi et al 2012b). In these two regions, the combined exposure reaches 10 6 s. We have also carried out dedicated XMM-Newton observations of SNR candidates found in ROSAT, radio, and optical data (Grondin et al 2012;Bozzetto et al 2014;Kavanagh et al 2015b). …”

Section: Introductionmentioning

confidence: 99%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

Self Cite

156

205

View full text Add to dashboard Cite

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.

show abstract

“…Detailed descriptions of the X-ray background constituents and spectral modelling can be found in Bozzetto et al (2014) and Maggi et al (2014). Here we briefly summarise the treatment of the X-ray background in the case of MCSNR J0512−6707.…”

Section: X-ray Backgroundmentioning

confidence: 99%

Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512−6707 in the Large Magellanic Cloud

Kavanagh

Sasaki

Bozzetto

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We present a multi-frequency study of the supernova remnant MCSNR J0512−6707 in the Large Magellanic Cloud. Methods. We used new data from XMM-Newton to characterise the X-ray emission and data from the Australian Telescope Compact Array, the Magellanic Cloud Emission Line Survey, and Spitzer to gain a picture of the environment into which the remnant is expanding. We performed a morphological study, determined radio polarisation and magnetic field orientation, and performed an X-ray spectral analysis. Results. We estimated the remnant's size to be 24.9 (±1.5) × 21.9 (±1.5) pc, with the major axis rotated ∼29 • east of north. Radio polarisation images at 3 cm and 6 cm indicate a higher degree of polarisation in the northwest and southeast tangentially oriented to the SNR shock front, indicative of an SNR compressing the magnetic field threading the interstellar medium. The X-ray spectrum is unusual as it requires a soft (∼0.2 keV) collisional ionisation equilibrium thermal plasma of interstellar medium abundance, in addition to a harder component. Using our fit results and the Sedov dynamical model, we showed that the thermal emission is not consistent with a Sedov remnant. We suggested that the thermal X-rays can be explained by MCSNR J0512−6707 having initially evolved into a wind-blown cavity and is now interacting with the surrounding dense shell. The origin of the hard component remains unclear. We could not determine the supernova type from the X-ray spectrum. Indirect evidence for the type is found in the study of the local stellar population and star formation history in the literature, which suggests a core-collapse origin. Conclusions. MCSNR J0512−6707 likely resulted from the core-collapse of high mass progenitor which carved a low density cavity into its surrounding medium, with the soft X-rays resulting from the impact of the blast wave with the surrounding shell. The unusual hard X-ray component requires deeper and higher spatial resolution radio and X-ray observations to confirm its origin.

show abstract

Multifrequency study of a new Fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508−6902

Cited by 21 publications

References 100 publications

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

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

Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512−6707 in the Large Magellanic Cloud

Contact Info

Product

Resources

About