Light echoes from ancient supernovae in the Large Magellanic Cloud

Rest, A.; Suntzeff, Nicholas B.; Olsen, Knut; Prieto, J. L.; Smith, R. C.; Welch, D. L.; Becker, A. C.; Bergmann, Marcel; Clocchiatti, A.; Cook, K. H.; Garg, Arti; Huber, M. E.; Miknaitis, G.; Minniti, D.; Nikolaev, Sergei; Stubbs, C. W.

doi:10.1038/nature04365

Cited by 158 publications

(204 citation statements)

References 24 publications

Supporting

Mentioning

192

Contrasting

Order By: Relevance

“…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 .…”

Section: Appendix A: the Epic Backgroundmentioning

confidence: 99%

See 1 more Smart Citation

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

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

Section: Appendix A: the Epic Backgroundmentioning

confidence: 99%

“…The most secured typing methods are the study of SN optical light echoes (Rest et al 2005(Rest et al , 2008; infrared light echoes can be used to probe the ISM dust, see e.g. Vogt et al 2012), the measurement of the nucleosynthesis products in the ejecta (e.g.…”

Section: The Typing Of Snrs In Generalmentioning

confidence: 99%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

156

205

View full text Add to dashboard Cite

show abstract

“…All those conditions are not usually met. In fact, light echoes are impressive and very rare phenomena that have been witnessed in only a handful of events (Couderc 1939;Suntzeff et al 1988;Bode & Evans 1985;Rest et al 2005;Krause et al 2005;Bond et al 2003;Sugerman 2005;Quinn et al 2006;Sugerman 2003;Crotts & Yourdon 2008;Liu et al 2003;Rest et al 2008a,b;Cappellaro et al 2001;Sparks et al 1999Sparks et al , 2008Bond & Sparks 2009, and references therein). Such events are mostly explosive or nearly explosive (supernovae, novae, novae-like, a Cepheid variable, and a planetary nebula) from stellar objects in their latest stages of evolution.…”

Section: Introductionmentioning

confidence: 99%

Observation of light echoes around very young stars

Ortiz¹,

Sugerman

Cueva³

et al. 2010

A&A

View full text Add to dashboard Cite

Aims. The goal of the paper is to present new results on light echoes from young stellar objects. Methods. Broad band CCD images were obtained over three months at one-to-two week intervals for the field of NGC 6726, using the large field-of-view remotely-operated telescope on top of Cerro Burek. Results. We detected scattered light echoes around two young, low-amplitude, irregular variable stars. Observations revealed not just one, but multiple light echoes from brightness pulses of the T Tauri star S CrA and the Herbig Ae/Be star R CrA. Analysis of S CrA's recurring echoes suggests that the star is located 138 ± 16 pc from Earth, making these the closest echoes ever detected. The environment that scatters the stellar light from S CrA is compatible with an incomplete dust shell or an inclined torus some 10 000 AU in radius and containing ∼2 × 10 −3 M of dust. The cause of such concentration at ∼10 000 AU from the star is unknown. It could be the remnant of the envelope from which the star formed, but the distance of the cloud is remarkably similar to the nominal distance of the Oort cloud to the Sun, leading us to also speculate that the dust (or ice) seen around S CrA might have the same origin as the Solar System Oort cloud.

show abstract

“…It is also one of several LMC SNRs for which a light-echo has been identified, from which an age of 600 ± 200 years can be deduced (Rest et al 2005).…”

Section: Introductionmentioning

confidence: 99%

The kinematics and chemical stratification of the type Ia supernova remnant 0519-69.0

Kosenko

Helder

Vink

2010

A&A

View full text Add to dashboard Cite

We present a detailed analysis of the XMM-Newton and Chandra X-ray data of the young type Ia supernova remnant SNR 0519-69.0, which is situated in the Large Magellanic Cloud. We used data from both the Chandra ACIS and XMM-Newton EPIC MOS instruments, and high resolution X-ray spectra obtained with the XMM-Newton reflection grating spectrometer (RGS). Our analysis of the spatial distribution of X-ray line emission using the Chandra data shows that there is a radial stratification of oxygen, intermediate mass elements (IME) and iron, with the emission from more massive elements peaking more toward the center. Using a deprojection technique we measure a forward shock radius of 4.0 ± 0.3 pc and a reverse shock radius of 2.7 ± 0.4 pc. We took the observed stratification of the shocked ejecta into account in the modeling of the X-ray spectra, for which we used multicomponent non-equilibrium ionization models, with the components corresponding to layers dominated by one or two elements. An additional component was added in order to represent the shocked interstellar medium, which mostly contributed to the continuum emission. This multicomponent model fits the data adequately, and was also employed to characterize the spectra of distinct regions extracted from the Chandra data. From our spectral analysis we find that the approximate fractional masses of shocked ejecta for the most abundant elements are: M O ≈ 32%, M Si/S ≈ 7%/5%, M Ar+Ca ≈ 1% and M Fe ≈ 55%. From the continuum component we derive a circumstellar density of n H = 2.4 ± 0.2 cm −3 . This density, together with the measurements of the forward and reverse shock radii suggest an age of 0519-69.0 of 450 ± 200 yr, somewhat lower than, but consistent with the age estimate based on the extent of the light echo (600 ± 200 yr). Finally, from the high resolution RGS spectra we measured a Doppler broadening of σ = 1873 ± 50 km s −1 , from which we derive a forward shock velocity of v FS = 2770 ± 500 km s −1 . We discuss our results in the context of single degenerate explosion models, using semi-analytical and numerical modeling, and compare the characteristics of 0519-69.0 with those of other type Ia supernova remnants.

show abstract

Light echoes from ancient supernovae in the Large Magellanic Cloud

Cited by 158 publications

References 24 publications

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

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

Observation of light echoes around very young stars

The kinematics and chemical stratification of the type Ia supernova remnant 0519-69.0

Contact Info

Product

Resources

About