Spectral Identification of an Ancient Supernova Using Light Echoes in the Large Magellanic Cloud

Rest, A.; Matheson, T.; Blondin, S.; Bergmann, Marcel; Welch, D. L.; Suntzeff, Nicholas B.; Smith, R. C.; Olsen, Knut; Prieto, J. L.; Garg, Arti; Challis, Peter; Stubbs, C. W.; Hicken, M.; Modjaz, M.; Wood‐Vasey, W. M.; Zenteno, A.; Damke, G.; Newman, Andrew B.; Huber, M. E.; Cook, K. H.; Nikolaev, Sergei; Becker, A. C.; Miceli, Antonino; Covarrubias, R.; Morelli, L.; Pignata, G.; Clocchiatti, A.; Minniti, D.; Foley, R. J.

doi:10.1086/587158

Cited by 112 publications

(97 citation statements)

References 61 publications

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“…This is unlike the youngest known type Ia SNR in the LMC, 0509-67.5, which was according to the light echo spectrum of the supernova an exceptionally bright type Ia (Rest et al 2008), similar to SN 1991T.…”

Section: The Chemical Composition Of Snr 0519-690mentioning

confidence: 62%

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

Kosenko

Helder

Vink

2010

A&A

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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.

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Section: The Chemical Composition Of Snr 0519-690mentioning

confidence: 62%

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

Kosenko

Helder

Vink

2010

A&A

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“…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

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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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“…The identification of GCD explosions with SNe 91T is challenged from observations of the supernova remnant SNR 0509-67.5 in the LMC. First, based on light echo spectra, Rest et al (2008) demonstrated clearly that this SN was a 1991T-like explosion. Second, Schaefer & Pagnotta (2012) ruled out the existence of a companion star in this SNR to very deep limits and thereby argued for a double-degenerate progenitor, which would exclude the canonical single-degenerate formation channel as a path to the GCD model.…”

Section: Introductionmentioning

confidence: 98%

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

Seitenzahl

Kromer

Ohlmann

et al. 2016

A&A

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The gravitationally confined detonation (GCD) model has been proposed as a possible explosion mechanism for Type Ia supernovae in the single-degenerate evolution channel. It starts with ignition of a deflagration in a single off-centre bubble in a near-Chandrasekharmass white dwarf. Driven by buoyancy, the deflagration flame rises in a narrow cone towards the surface. For the most part, the main component of the flow of the expanding ashes remains radial, but upon reaching the outer, low-pressure layers of the white dwarf, an additional lateral component develops. This causes the deflagration ashes to converge again at the opposite side, where the compression heats fuel and a detonation may be launched. We first performed five three-dimensional hydrodynamic simulations of the deflagration phase in 1.4 M carbon/oxygen white dwarfs at intermediate-resolution (256 3 computational zones). We confirm that the closer the initial deflagration is ignited to the centre, the slower the buoyant rise and the longer the deflagration ashes takes to break out and close in on the opposite pole to collide. To test the GCD explosion model, we then performed a high-resolution (512 3 computational zones) simulation for a model with an ignition spot offset near the upper limit of what is still justifiable, 200 km. This high-resolution simulation met our deliberately optimistic detonation criteria, and we initiated a detonation. The detonation burned through the white dwarf and led to its complete disruption. For this model, we determined detailed nucleosynthetic yields by post-processing 10 6 tracer particles with a 384 nuclide reaction network, and we present multi-band light curves and time-dependent optical spectra. We find that our synthetic observables show a prominent viewing-angle sensitivity in ultraviolet and blue wavelength bands, which contradicts observed SNe Ia. The strong dependence on the viewing angle is caused by the asymmetric distribution of the deflagration ashes in the outer ejecta layers. Finally, we compared our model to SN 1991T. The overall flux level of the model is slightly too low, and the model predicts pre-maximum light spectral features due to Ca, S, and Si that are too strong. Furthermore, the model chemical abundance stratification qualitatively disagrees with recent abundance tomography results in two key areas: our model lacks low-velocity stable Fe and instead has copious amounts of high-velocity 56 Ni and stable Fe. We therefore do not find good agreement of the model with SN 1991T.

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Spectral Identification of an Ancient Supernova Using Light Echoes in the Large Magellanic Cloud

Cited by 112 publications

References 61 publications

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

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

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

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

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