Maximally Dusty Star-forming Galaxies: Supernova Dust Production and Recycling in Local Group and High-redshift Galaxies

Gall, C.; Hjorth, J.

doi:10.3847/1538-4357/aae520

Cited by 45 publications

(38 citation statements)

References 160 publications

(268 reference statements)

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“…Some dust destruction, but not a significant amount, by SNe would be allowed in these cases as the derived dust yields are above 0.1M . This is in line with the result of Gall & Hjorth (2018) that dust in distant galaxies (including A2744_YD4) was formed by SNe, which requires very little dust destruction. Again, the required dust yields per AGB star for these three galaxies are significantly above the theoretical limit, so AGB stars have not contributed substantially to the dust production in these galaxies.…”

Section: Resultssupporting

confidence: 91%

Dust production scenarios in galaxies at z ∼6–8.3

Leśniewska

Michałowski

2019

A&A

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Context. The mechanism of dust formation in galaxies at high redshift is still unknown. Asymptotic giant branch (AGB) stars and explosions of supernovae (SNe) are possible dust producers, and non-stellar processes may substantially contribute to dust production, for example grain growth in the interstellar medium (ISM). Aims. Our aim is to determine the contribution to dust production of AGB stars and SNe in nine galaxies at z ∼ 6-8.3, for which observations of dust have been recently attempted. Methods. In order to determine the origin of the observed dust we have determined dust yields per AGB star and SN required to explain the total amounts of dust in these galaxies.Results. We find that AGB stars were not able to produce the amounts of dust observed in the galaxies in our sample. In order to explain these dust masses, SNe would have to have maximum efficiency and not destroy the dust which they formed. Conclusions. Therefore, the observed amounts of dust in the galaxies in the early universe were formed either by efficient supernovae or by a non-stellar mechanism, for instance the grain growth in the interstellar medium.

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Section: Resultssupporting

confidence: 91%

Dust production scenarios in galaxies at z ∼6–8.3

Leśniewska

Michałowski

2019

A&A

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“…The average dust produced per SN is ∼0.1 M e for all three metallicities. We note that dust formation in SN ejecta is still uncertain and measurements range from∼10 −6 to 1 M e of dust per SN (Temim et al 2015;Gall & Hjorth 2018;Sarangi et al 2018), but SNe would have to form dust beyond the highest mass range of the observed values in order to compensate for the dust destruction rate.…”

Section: Binary Population and Spectra Synthesis Modelsmentioning

confidence: 88%

Revisiting the Impact of Dust Production from Carbon-rich Wolf–Rayet Binaries

Lau¹,

Eldridge

Hankins

et al. 2020

ApJ

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We present a dust spectral energy distribution (SED) and binary stellar population analysis revisiting the dust production rates (DPRs) in the winds of carbon-rich Wolf-Rayet (WC) binaries and their impact on galactic dust budgets. DustEMSED models of 19Galactic WC "dustars" reveal DPRs of~-M 10 10 d 10 6- M e yr −1 and carbon dust condensation fractions, χ C , between 0.002% and 40%. A large (0.1-1.0μm) dust grain size composition is favored for efficient dustars where χ C 1%. Results for dustars with known orbital periods verify a power-law relation between χ C , orbital period, WC mass-loss rate, and wind velocity consistent with predictions from theoretical models of dust formation in colliding-wind binaries. We incorporated dust production into Binary Population and Spectral Synthesis (BPASS) models to analyze dust production rates from WC dustars, asymptotic giant branch stars (AGBs), red supergiants (RSGs), and core-collapse supernovae (SNe). BPASS models assuming constant star formation (SF) and a coeval 10 6 M e stellar population were performed at low, Large Magellanic Cloud (LMC)-like, and solar metallicities (Z=0.001, 0.008, and 0.020). Both constant SF and coeval models indicate that SNe are net dust destroyers at all metallicities. Constant SF models at LMC-like metallicities show that AGB stars slightly outproduce WC binaries and RSGs by factors of 2-3, whereas at solar metallicities WC binaries are the dominant source of dust for ∼60 Myr until the onset of AGBs, which match the dust input of WC binaries. Coeval population models show that, for "bursty" SF, AGB stars dominate dust production at late times (t 70 Myr).

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“…A recent study by De found that observed galaxy scaling relations are better fit by longer grain lifetimes and less efficient grain growth, supporting this interpretation. Gall & Hjorth (2018) have also suggested that the relationship between dust and stellar masses can be explained by inefficient dust destruction processes, although they offer rapid replenishment of dust in the ISM as an alternative interpretation. This overestimation of the destruction efficiency would only be the case if the objects we investigate are representative of SNRs in general, which is not necessarily true given that we were able to select only three from a sample size of hundreds.…”

Section: Discussionmentioning

confidence: 99%

Revisiting the dust destruction efficiency of supernovae

Priestley

Chawner

Matsuura

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Dust destruction by supernovae is one of the main processes removing dust from the interstellar medium (ISM). Estimates of the efficiency of this process, both theoretical and observational, typically assume a shock propagating into a homogeneous medium, whereas the ISM possesses significant substructure in reality. We self-consistently model the dust and gas properties of the shocked ISM in three supernova remnants (SNRs), using X-ray and infrared (IR) data combined with corresponding emission models. Collisional heating by gas with properties derived from X-ray observations produces dust temperatures too high to fit the far-IR fluxes from each SNR. An additional colder dust component is required, which has a minimum mass several orders of magnitude larger than that of the warm dust heated by the X-ray emitting gas. Dust-to-gas mass ratios indicate that the majority of the dust in the X-ray emitting material has been destroyed, while the fraction of surviving dust in the cold component is plausibly close to unity. As the cold component makes up virtually all the total dust mass, destruction timescales based on homogeneous models, which cannot account for multiple phases of shocked gas and dust, may be significantly overestimating actual dust destruction efficiencies, and subsequently underestimating grain lifetimes.

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Maximally Dusty Star-forming Galaxies: Supernova Dust Production and Recycling in Local Group and High-redshift Galaxies

Cited by 45 publications

References 160 publications

Dust production scenarios in galaxies at z ∼6–8.3

Dust production scenarios in galaxies at z ∼6–8.3

Revisiting the Impact of Dust Production from Carbon-rich Wolf–Rayet Binaries

Revisiting the dust destruction efficiency of supernovae

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