THE INFLUENCE OF SUPERNOVA REMNANTS ON THE INTERSTELLAR MEDIUM IN THE LARGE MAGELLANIC CLOUD SEEN AT 20-600 μm WAVELENGTHS

Lakićević, M.; Loon, Jacco Th. van; Meixner, M.; Gordon, K. D.; Bot, Caroline; Roman-Duval, Julia; Babler, B.; Bolatto, Alberto D.; Engelbracht, C. W.; Filipović, Miroslav; Hony, S.; Indebetouw, R.; Misselt, K. A.; Montiel, Edward; Okumura, K.; Panuzzo, P.; Patat, F.; Sauvage, M.; Seale, Jonathan; Sonneborn, G.; Temim, Tea; Urošević, D.; Zanardo, Giovanna

doi:10.1088/0004-637x/799/1/50

Cited by 73 publications

(70 citation statements)

References 91 publications

(90 reference statements)

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“…polarisation measurements) are therefore needed to distinguish the two components (Dunne et al 2009). The difficulty in determining how much emission comes from dust in the remnant and how much from the ISM was also recognised in the recent analysis of a sample of SNRs in the LMC by Lakićević et al (2015): while they placed constraints on the influence of the remnant on the nearby ISM, the data lacked the resolution and sensitivity to study the amount of dust within the remnants themselves.…”

Section: Referencesmentioning

confidence: 99%

“…In contrast, supernova (SN) explosions in the interstellar medium (ISM) trigger shock waves that are able to quickly process dust grains and are considered the dominant mechanism of dust destruction in the ISM (Barlow 1978a,b;Draine & Salpeter 1979a,b;Dwek & Scalo 1980;Seab & Shull 1983;McKee et al 1987;Jones et al , 1996Lakićević et al 2015;Slavin et al 2015). A recent theoretical work on interstellar dust destruction in shock waves led to an estimated lifetime of ∼6 × 10 7 yr and ∼3 × 10 8 yr for carbonaceous and silicate grains in our Galaxy, respectively (Bocchio et al 2014), which is much shorter than the assumed dust formation timescale from AGB stars.…”

Section: Introductionmentioning

confidence: 99%

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Dust grains from the heart of supernovae

Bocchio

Marassi

Schneider

et al. 2016

A&A

141

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Dust grains are classically thought to form in the winds of asymptotic giant branch (AGB) stars. However, there is increasing evidence today for dust formation in supernovae (SNe). To establish the relative importance of these two classes of stellar sources of dust, it is important to know the fraction of freshly formed dust in SN ejecta that is able to survive the passage of the reverse shock and be injected in the interstellar medium. With this aim, we have developed a new code, GRASH_Rev, that allows following the dynamics of dust grains in the shocked SN ejecta and computing the time evolution of the mass, composition, and size distribution of the grains. We considered four well-studied SNe in the Milky Way and Large Magellanic Cloud: SN 1987A, CasA, the Crab nebula, and N49. These sources have been observed with both Spitzer and Herschel, and the multiwavelength data allow a better assessment the mass of warm and cold dust associated with the ejecta. For each SN, we first identified the best explosion model, using the mass and metallicity of the progenitor star, the mass of 56 Ni, the explosion energy, and the circumstellar medium density inferred from the data. We then ran a recently developed dust formation model to compute the properties of freshly formed dust. Starting from these input models, GRASH_Rev self-consistently follows the dynamics of the grains, considering the effects of the forward and reverse shock, and allows predicting the time evolution of the dust mass, composition, and size distribution in the shocked and unshocked regions of the ejecta. All the simulated models aagree well with observations. Our study suggests that SN 1987A is too young for the reverse shock to have affected the dust mass. Hence the observed dust mass of 0.7−0.9 M in this source can be safely considered as indicative of the mass of freshly formed dust in SN ejecta. Conversely, in the other three SNe, the reverse shock has already destroyed between 10−40% of the initial dust mass. However, the largest dust mass destruction is predicted to occur between 10 3 and 10 5 yr after the explosions. Since the oldest SN in the sample has an estimated age of 4800 yr, current observations can only provide an upper limit to the mass of SN dust that will enrich the interstellar medium, the so-called effective dust yields. We find that only between 1−8% of the currently observed mass will survive, resulting in an average SN effective dust yield of (1.55 ± 1.48) × 10 −2 M . This agrees well with the values adopted in chemical evolution models that consider the effect of the SN reverse shock. We discuss the astrophysical implications of our results for dust enrichment in local galaxies and at high redshift.

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Section: Referencesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Dust grains from the heart of supernovae

Bocchio

Marassi

Schneider

et al. 2016

A&A

141

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“…Theoretical models predict that a SN can produce at most ∼1.3 M of dust (Todini & Ferrara 2001;Nozawa et al 2003), but likely only < ∼ 0.1 M survives the associated shocks and is released into the ISM (Bianchi & Schneider 2007;Cherchneff & Dwek 2010;Gall et al 2011a;Lakićević et al 2015). Large amounts of dust have been found in the Scottish Universities Physics Alliance.…”

Section: Introductionmentioning

confidence: 99%

Dust production 680–850 million years after the Big Bang

Michałowski

2015

A&A

107

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Dust plays an important role in our understanding of the Universe, but it is not obvious yet how the dust in the distant universe was formed. I derived the dust yields per asymptotic giant branch (AGB) star and per supernova (SN) required to explain dust masses of galaxies at z = 6.3-7.5 (680-850 million years after the Big Bang) for which dust emission has been detected (HFLS3 at z = 6.34, ULAS J1120+0641 at z = 7.085, and A1689-zD1 at z = 7.5), or unsuccessfully searched for. I found very high required yields, implying that AGB stars could not contribute substantially to dust production at these redshifts, and that SNe could explain these dust masses, but only if they do not destroy most of the dust they form (which is unlikely given the upper limits on the SN dust yields derived for galaxies where dust is not detected). This suggests that the grain growth in the interstellar medium is likely required at these early epochs.

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“…Williams et al (1999) produced an X-ray atlas of LMC SNRs, while Sasaki et al (2000) compiled a ROSAT HRI catalogue of X-ray sources in the LMC region. Blair et al (2006) and Lakićević et al (2015) surveyed SNRs in the MCs at far UV wavelengths. Seok et al (2013) presented a survey of infrared SNRs in the LMC.…”

mentioning

confidence: 99%

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Bozzetto

Filipović

Vukotić

et al. 2017

ApJS

Self Cite

107

158

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We construct the most complete sample of supernova remnants (SNRs) in any galaxy -the Large Magellanic Cloud (LMC) SNR sample. We study their various properties such as spectral index (α), size and surface-brightness. We suggest an association between the spatial distribution, environment density of LMC SNRs and their tendency to be located around supergiant shells. We find evidence that the 16 known type Ia LMC SNRs are expanding in a lower density environment compared to the Core-Collapse (CC) type. The mean diameter of our entire population (74) is 41 pc, which is comparable to nearby galaxies. We didn't find any correlation between the type of SN explosion, ovality or age. The N (< D) relationship of a = 0.96 implies that the randomised diameters are readily mimicking such an exponent. The rate of SNe occurring in the LMC is estimated to be ∼1 per 200 yr. The mean α of the entire LMC SNR population is α=-0.52, which is typical of most SNRs. However, our estimates show a clear flattening of the synchrotron α as the remnants age. As predicted, our CC SNRs sample are significantly brighter radio emitters than the type Ia remnants. We also estimate the Σ − D relation for the LMC to have a slope ∼3.8 which is comparable with other nearby galaxies. We also find the residency time of electrons in the galaxy

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THE INFLUENCE OF SUPERNOVA REMNANTS ON THE INTERSTELLAR MEDIUM IN THE LARGE MAGELLANIC CLOUD SEEN AT 20-600 μm WAVELENGTHS

Cited by 73 publications

References 91 publications

Dust grains from the heart of supernovae

Dust grains from the heart of supernovae

Dust production 680–850 million years after the Big Bang

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

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