Smoothed particle inference analysis and abundance calculations of DEM L71, and comparison to SN explosion models

Siegel, Jared; Dwarkadas, Vikram V.; Frank, Kari A.; Burrows, D. N.; Panfichi, Aldo

doi:10.1002/asna.202023773

Cited by 8 publications

(5 citation statements)

References 16 publications

(29 reference statements)

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“…Our tentative Fe Kα detection in DEM L71 falls comfortably within the Type Ia parameter space reported by Y14. This classification is consistent with several previous studies of DEM L71, which identified Fe enhancements and pure-ejecta emission (Ghavamian et al 2003;Hughes et al 2003;Frank et al 2019;Siegel et al 2020a).…”

Section: Discussionsupporting

confidence: 93%

Can the Fe K-alpha Line Reliably Predict Supernova Remnant Progenitors?

Siegel,

Dwarkadas,

Frank

et al. 2021

Preprint

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The centroid energy of the Fe Kα line has been used to identify the progenitors of supernova remnants (SNRs). These investigations generally considered the energy of the centroid derived from the spectrum of the entire remnant. Here we use XMM-Newton data to investigate the Fe Kα centroid in 6 SNRs: 3C 397, N132D, W49B, DEM L71, 1E 0102.2-7219, and Kes 73. In Kes 73 and 1E 0102.2-7219, we fail to detect any Fe Kα emission. We report a tentative first detection of Fe Kα emission in SNR DEM L71, with a centroid energy consistent with its Type Ia designation. In the remaining remnants, the spatial and spectral sensitivity is sufficient to investigate spatial variations of the Fe Kα centroid. We find in N132D and W49B that the centroids in different regions are consistent with that derived from the overall spectrum, although not necessarily with the remnant type identified via other means. However, in SNR 3C 397, we find statistically significant variation in the centroid of up to 100 eV, aligning with the variation in the density structure around the remnant. These variations span the intermediate space between centroid energies signifying core-collapse and Type Ia remnants. Shifting the dividing line downwards by 50 eV can place all the centroids in the CC region, but contradicts the remnant type obtained via other means. Our results show that caution must be used when employing the Fe Kα centroid of the entire remnant as the sole diagnostic for typing a remnant.

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Section: Discussionsupporting

confidence: 93%

Can the Fe K-alpha Line Reliably Predict Supernova Remnant Progenitors?

Siegel,

Dwarkadas,

Frank

et al. 2021

Preprint

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“…The total swept-up mass, 𝑀 SW = 𝑛 0 𝑚 p 𝑉 is also estimated to be 𝑀 SW ∼ 145 +30 −25 𝑓 1/2 𝑀 , assuming that the average SNR radius of ∼ 9.7 pc. This calculated mass conforms with the swept-up ISM value given by Siegel et al (2020) within uncertainties. Our estimated explosion energy suggest that DEM L71 originates from a canonical SD or DD progenitor system.…”

Section: Snr Dynamicssupporting

confidence: 86%

“…Optical observations of the Balmer-dominated shock velocities by Ghavamian et al (2003) yield an age estimate of 4, 360 ± 90 yr. Pagnotta & Schaefer (2015) utilized optical images (𝑔 , 𝑟 , 𝑖 , and H 𝛼 ) to identify a great number of possible candidates for the SNs surviving companion; but it has not been detected. Recently, Siegel et al (2020) analyzed the XMM-Newton data of the DEM L71 and estimated the total mass of the swept-up interstellar medium (ISM) as 228 ± 23𝑀 .…”

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confidence: 99%

Spatially Resolved Chandra Spectroscopy of Supernova Remnant DEM L71 in the Large Magellanic Cloud

Alan,

Bilir

2022

Preprint

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We present a detailed X-ray spectroscopic study of the supernova remnant DEM L71 in the Large Magellanic Cloud.Based on deep ∼ 103 ks archival Chandra data, we perform a detailed spatially resolved spectral analysis of DEM L71. We analyze regional spectra extracted from thin-sliced regions along several different azimuthal directions of the SNR to construct radial profiles of elemental abundances for O, Ne, Mg, Si, and Fe. Our elemental abundance measurements reveal an asymmetrical spatial distribution of metal-rich ejecta gas. Especially the asymmetry on the western part of the central Fe distribution is remarkable. While the location of the contact discontinuity is generally at ∼ 5 pc from the geometric center of the X-ray emission of DEM L71, it is uncertain in western part of the remnant. Fe is enhanced in the ejecta while O and Ne abundances are generally negligible. This finding confirms the Type Ia origin of DEM L71.We estimate an upper limit on the Sedov age of ∼ 6, 660 ± 770 yr and explosion energy of ∼ 1.74 ± 0.35 × 10 51 erg for the remnant. This explosion energy estimate is consistent with a canonical explosion of a Type Ia supernova remnant.

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“…This method allows us to model the entire remnant and provides significant flexibility while analyzing the emission. Details of the SPI process, combined with a first demonstration of its unique capabilities, were provided in two earlier papers, where it was used to study the SNR DEM L71 (Frank et al 2019;Siegel et al 2020).…”

Section: Application Of Spi To W49bmentioning

confidence: 99%

“…Using the blob volume in the equation for EM above, we derive the combination of n e n H ; we further need a relation between n e and n H to extricate the individual quantities. This process was discussed in Siegel et al (2020). Here we consider two different approaches.…”

Section: Mass and Densitymentioning

confidence: 99%

Analysis of XMM-Newton Observations of Supernova Remnant W49B and Clues to the Progenitor

Siegel,

Dwarkadas,

Frank

et al. 2020

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W49B is a supernova remnant (SNR) discovered over 60 years ago in early radio surveys. It has since been observed over the entire wavelength range, with the X-ray morphology resembling a centrallyfilled SNR. The nature of its progenitor star is still debated. Applying Smoothed Particle Inference techniques to analyze the X-Ray emission from W49B, we characterize the morphology and abundance distribution over the entire remnant. We also infer the density structure and derive the mass of individual elements present in the plasma. The morphology is consistent with an interaction between the remnant and a dense medium along the eastern edge, and some obstruction towards the west. We find a total mass of 130 (±16) M and an estimated ejecta mass of 1.2 (±0.2) M . Comparison of the inferred abundance values and individual element masses with a wide selection of SN models suggests that deflagration-to-detonation (DDT) Type Ia models are the most compatible, with Fe abundance being the major discriminating factor. The general agreement between our abundance measurements and those from previous studies suggests that disagreement between various authors is more likely due to the choice of models used for comparison, rather than the abundance values themselves. While our abundance results lean toward a Type Ia origin, ambiguities in the interpretation of various morphological and spectral characteristics of W49B do not allow us to provide a definitive classification.

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Smoothed particle inference analysis and abundance calculations of DEM L71, and comparison to SN explosion models

Cited by 8 publications

References 16 publications

Can the Fe K-alpha Line Reliably Predict Supernova Remnant Progenitors?

Can the Fe K-alpha Line Reliably Predict Supernova Remnant Progenitors?

Spatially Resolved Chandra Spectroscopy of Supernova Remnant DEM L71 in the Large Magellanic Cloud

Analysis of XMM-Newton Observations of Supernova Remnant W49B and Clues to the Progenitor

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