Abundances of the heavy elements in the Magellanic Clouds. III - Interpretation of results

Russell, Stephen C.; Dopita, Michael A.

doi:10.1086/170893

Cited by 569 publications

(698 citation statements)

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“…First, a one-component collisional ionisation equilibrium (CIE) model (vapec in XSPEC) is tried. The elemental abundances are initially set to the values measured by Russell & Dopita (1992). Their abundance of silicon is highly uncertain, however, and therefore we use an initial value of half solar for Si.…”

Section: Spectral Modelsmentioning

confidence: 99%

“…To identify SNRs with detected ejecta and the origin thereof, we computed abundance ratios X/Fe, where X is O, Ne, Mg, or Si. The ratios are normalised with respect to (X/Fe) LMC , the corresponding ratios with the LMC abundances (from Russell & Dopita 1992). As CC-SNRs produce large amounts of light-Z elements and little iron, high (X/Fe)/(X/Fe) LMC ratios (in excess of one) indicate a massive star progenitor.…”

Section: Detection Of Sn Ejectamentioning

confidence: 99%

“…Therefore, the fitted abundances in these cases provide us with measurements of the chemical composition of the gas phase of the LMC ISM. Russell & Dopita (1992) and Hughes et al (1998) have used samples of SNRs to obtain the abundance of some elements (using optical and X-ray observations, respectively), but the smaller sample of known SNRs and sensitivity of the X-ray instrument used (ASCA) at the time limited the number of SNRs eligible to measure LMC abundances. We first selected all 1T/2T SNRs with fitted abundances but no high or low abundance ratios.…”

Section: Metal Abundances Of the Lmc Ismmentioning

confidence: 99%

“…The results are listed in Table 5. The absolute abundances, in the form 12 + log(X/H) (by number), are given, in comparison with results from Russell & Dopita (1992) Wilms et al (2000), measured in a sample of 16 X-ray SNRs. The selection of the sample and the measurements of abundance are described in Sect.…”

Section: Metal Abundances Of the Lmc Ismmentioning

confidence: 99%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

149

205

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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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Section: Spectral Modelsmentioning

confidence: 99%

Section: Detection Of Sn Ejectamentioning

confidence: 99%

Section: Metal Abundances Of the Lmc Ismmentioning

confidence: 99%

Section: Metal Abundances Of the Lmc Ismmentioning

confidence: 99%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

149

205

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“…We will need upcoming Chandra observations in order to determine whether the latest temperature variation means a truly stable phase or only a temporary state in the course of further, continuous softening of the overall X-ray spectrum. Russell & Dopita 1992 Although the overall X-ray spectrum of SNR 1987A can be described by a single temperature plane-shock in non-equilibrium ionization (NEI), the physical model of the shock-inner ring interaction indicates that X-ray emission most likely originates from multiple velocity components of the shock in various ionization states. Considering such a multi-component shock, a two-temperature shock model was implemented in order to fit the observed X-ray spectrum (Michael et al, 2002;Park et al, 2004).…”

Section: X-ray Spectrummentioning

confidence: 99%

Supernova remnant 1987A: The latest report from the Chandra X-ray Observatory

Park

Zhekov

Burrows

et al. 2005

Advances in Space Research

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We continue monitoring supernova remnant (SNR) 1987A with the Chandra Xray Observatory. As of 2004 January, bright X-ray spots in the northwest and the southwest are now evident in addition to the bright eastern ring. The overall Xray spectrum, Since 2002 December, can be described by a planar shock with an electron temperature of ∼2.1 keV. The soft X-ray flux is now 8 × 10 −13 ergs cm −2 s −1 , which is about five times higher than four years ago. This flux increase rate is consistent with our prediction based on an exponential density distribution along the radius of the SNR between the HII region and the inner ring. We still have no direct evidence of a central point source, and place an upper limit of L X = 1.3 × 10 34 ergs s −1 on the 3−10 keV band X-ray luminosity.

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

et al. 2020

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We analyze the X‐ray emission from the supernova remnant DEM L71 using the smoothed particle inference (SPI) technique. The high Fe abundance found appears to confirm the Type Ia origin. Our method allows the separation of the material ejected in the supernova explosion from the material swept up by the supernova shock wave. We are able to calculate the total mass of this swept‐up material to be about 228 ± 23 M⊙. We plot the posterior distribution for the number density parameter, and create a map of the density structure within the remnant. While the observed density shows substantial variations, we find our results are generally consistent with a two‐dimensional hydrodynamical model of the remnant that we have run. Assuming the ejected material arises from a Type Ia explosion, with no hydrogen present, we use the predicted yields from Type Ia models available in the literature to characterize the emitting gas. We find that the abundance of various elements match those predicted by deflagration‐to‐detonation transition (DDT) models. Our results, compatible with the Type Ia scenario, highlight the complexity of the remnant and the nature of the surrounding medium.

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Abundances of the heavy elements in the Magellanic Clouds. III - Interpretation of results

Cited by 569 publications

References 0 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

Supernova remnant 1987A: The latest report from the Chandra X-ray Observatory

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

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