Calibrating Interstellar Abundances Using Supernova Remnant Radiative Shocks

Dopita, Michael A.; Seitenzahl, Ivo R.; Sutherland, Ralph S.; Nicholls, David C.; Vogt, F.; Ghavamian, Parviz; Ruiter, Ashley J.

doi:10.3847/1538-3881/aaf235

Cited by 42 publications

(34 citation statements)

References 77 publications

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“…Our MCSNR candidates have values of 0.47 and 0.46 (see also Table 2) so we can classify them as SNRs. Also, the ratio between the individual [S ii] lines (6717 Å/ 6731 Å) of 1.32 and 1.56 is fully in line with optical 1979) it is well known that [N ii] lines are very weak due to an abundance effect: nitrogen, particularly in the SMC, is even more underabundant (by 0.3 -0.5 dex) than other elements (Russell & Dopita 1992;Dopita et al 2019). So, if we exclude the value and comparison of nitrogen lines with Hα, all other spectral characteristics of these two candidates match SNRs.…”

Section: Optical Spectroscopysupporting

confidence: 52%

“…ii) Photoionisation modelling of H ii nebular spectra (Kurt et al 1999;Peimbert et al 2000;Testor 2001;Relaño et al 2002;Peña-Guerrero et al 2012;Carlos Reyes et al 2015) remains affected by uncertainties of available atomic data, escape fraction, and incident spectra. iii) Spectral modelling of radiative shocks in dense ISM clouds, as found within some SNRs (Russell & Dopita 1990;Dopita et al 2019). Finally, in cases where the X-ray emission of SNRs is solely comprised of, or dominated by swept-up ISM, we can use the fitted abundances as measurements of the chemical composition of the ISM gas phase.…”

Section: Abundances Of the Smc Ismmentioning

confidence: 99%

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The supernova remnant population of the Small Magellanic Cloud

Maggi

Filipović

Vukotić

et al. 2019

A&A

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Aims. We present a comprehensive study of the supernova remnant (SNR) population of the Small Magellanic Cloud (SMC). We measure multiwavelength properties of the SMC SNRs and compare them to those of the Large Magellanic Cloud (LMC) population.Methods. This study combines the large dataset of XMM-Newton observations of the SMC, archival and recent radio continuum observations, an optical line emission survey, and new optical spectroscopic observations. We can thus build a complete and clean sample of 19 confirmed and 4 candidate SNRs. The homogeneous X-ray spectral analysis allows to search for SN ejecta and Fe K line emission, and to measure interstellar medium (ISM) abundances. We estimate the ratio of core-collapse to type Ia supernova rates of the SMC based on the X-ray properties and the local stellar environment of each SNR. Results. After the removal of unconfirmed or misclassified objects, and the addition of two newly confirmed SNRs based on multiwavelength features, we present a final list of 21 confirmed SNRs and 2 candidates. While no Fe K line is detected even for the brightest and youngest SNR, we find X-ray evidence of SN ejecta in 11 SNRs. We estimate a ratio of 4.7 +0.6 −1.9 core-collapse supernova to every type Ia SN, three times higher than in the LMC. The difference can be ascribed to the absence of the enhanced star formation episode in the SMC, which occurred in the LMC 0.5 -1.5 Gyr ago. The hot-gas abundances of O, Ne, Mg, and Fe are 0.1 -0.2 times solar. Their ratios with respect to SMC stellar abundances reflect the effects of dust depletion and partial dust destruction in SNR shocks. We find evidence that the ambient medium probed by SMC SNRs is less disturbed and less dense on average than in the LMC, consistent with the different morphologies of the two galaxies.

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Section: Optical Spectroscopysupporting

confidence: 52%

Section: Abundances Of the Smc Ismmentioning

confidence: 99%

The supernova remnant population of the Small Magellanic Cloud

Maggi

Filipović

Vukotić

et al. 2019

A&A

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“…= 144.2/106). Obtained metal abundances of O, Ne, Mg, Si, and Fe are significant higher than the SMC values (O = 0.23, Ne = 0.20, Mg = 0.21, Si = 0.30, and Fe = 0.22; Dopita et al 2019), suggesting that the SNR plasma possibly originates from the SN ejecta.…”

Section: X-ray Spectral Analysismentioning

confidence: 68%

“…We linked the abundance of Ni and those of S, Ar, and Ca to Fe and Si, respectively. The other elements were fixed to the SMC values in the literature (He = 0.85, C = 0.10, N = 0.09, and others = 0.20; Dopita et al 2019). Figure 6(a) and Table 2 show the fitting results and the best-fit parameters, respectively.…”

Section: X-ray Spectral Analysismentioning

confidence: 99%

Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud

Sano

Matsumura

Yamane

et al. 2019

ApJ

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RX J0046.5−7308 is a shell-type supernova remnant (SNR) in the Small Magellanic Cloud (SMC). We carried out new 12 CO(J = 1-0, 3-2) observations toward the SNR using Mopra and the Atacama Submillimeter Telescope Experiment. We found eight molecular clouds (A-H) along the X-ray shell of the SNR. The typical cloud size and mass are ∼10-15 pc and ∼1000-3000 M ⊙ , respectively. The X-ray shell is slightly deformed and has the brightest peak in the southwestern shell where two molecular clouds A and B are located. The four molecular clouds A, B, F, and G have high intensity ratios of 12 CO(J = 3-2) / 12 CO(J = 1-0) > 1.2, which are not attributable to any identified internal infrared sources or high-mass stars. The Hi cavity and its expanding motion are found toward the SNR, which are likely created by strong stellar winds from a massive progenitor. We suggest that the molecular clouds A-D, F, and G, and Hi clouds within the wind-blown cavity at V LSR = 117.1-122.5 km s −1 are associated with the SNR. The X-ray spectroscopy reveals the dynamical age of 26000 +1000 −2000yr and the progenitor mass of 30 M ⊙ , which is also consistent with the proposed scenario. We determine physical conditions of the giant molecular cloud LIRS 36A using the large velocity gradient analysis with archival datasets of the Atacama Large Millimeter/submillimeter Array; the kinematic temperature is 72 +50 −37 K and the number density of molecular hydrogen is 1500 +600 −300 cm −3 . The next generation of γ-ray observations will allow us to study the pion-decay γ-rays from the molecular clouds in the SMC SNR.

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“…Metallicity dependence of the Mn/Fe (filled circle) and Ni/Fe (filled square) mass ratios in the incomplete Si burning layer (at a peak temperature of 5×10 9 K) for the delayed detonation model with transition density, ρ = 2.8×10 7 g cm −3 . Dopita et al (2019) investigated the abundances of interstellar medium clouds in the immediate vicinity of Kepler's SNR, which shows higher element abundances. For example, the carbon and oxygen abundances relative to hydrogen are ∼3-5 times higher than those in the sun (Asplund et al 2009), which would support our result and the Suzaku observation (Park et al 2013).…”

Section: Comparison With Nucleosynthesis Modelsmentioning

confidence: 99%

A Nucleosynthetic Origin for the Southwestern Fe-rich Structure in Kepler’s Supernova Remnant

Sato

Bravo

Badenes

et al. 2020

ApJ

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Chandra X-ray observations of Kepler's supernova remnant indicate the existence of a high speed Fe-rich ejecta structure in the southwestern region. We report strong K-shell emission from Fe-peak elements (Cr, Mn, Fe, Ni), as well as Ca, in this Fe-rich structure, implying that those elements could be produced in the inner area of the exploding white dwarf. We found Ca/Fe, Cr/Fe, Mn/Fe and Ni/Fe mass ratios of 1.0-4.1%, 1.0-4.6%, 1-11% and 2-30%, respectively. In order to constrain the burning regime that could produce this structure, we compared these observed mass ratios with those in 18 one-dimensional Type Ia nucleosynthesis models (including both near-M Ch and sub-M Ch explosion models). The observed mass ratios agree well with those around the middle layer of incomplete Si-burning in Type Ia nucleosynthesis models with a peak temperature of ∼(5.0-5.3)×10 9 K and a high metallicity, Z > 0.0225. Based on our results, we infer the necessity for some mechanism to produce protruding Fe-rich clumps dominated by incomplete Si-burning products during the explosion. We also discuss the future perspectives of X-ray observations of Fe-rich structures in other Type Ia supernova remnants.

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Calibrating Interstellar Abundances Using Supernova Remnant Radiative Shocks

Cited by 42 publications

References 77 publications

The supernova remnant population of the Small Magellanic Cloud

The supernova remnant population of the Small Magellanic Cloud

Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud

A Nucleosynthetic Origin for the Southwestern Fe-rich Structure in Kepler’s Supernova Remnant

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