Dust production 680–850 million years after the Big Bang

Michałowski, M. J.

doi:10.1051/0004-6361/201525644

Cited by 109 publications

(100 citation statements)

References 117 publications

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“…The importance of dust growth by accretion for the total dust abundance has already been shown for various galaxy samples by many authors (e.g. Dwek et al 2007;Michałowski et al 2010aMichałowski et al , 2010bHirashita & Kuo 2011;Valiante et al 2011;Kuo & Hirashita 2012;Mancini et al 2015;Michałowski 2015). Recent experiments by Rouillé et al (2014) showed that accretion actually occurs in cold environments.…”

Section: Constraint On the Parametersmentioning

confidence: 83%

Dust evolution processes constrained by extinction curves in nearby galaxies

Hou

Hirashita

Michałowski

2016

Publications of the Astronomical Society of Japan

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Extinction curves, especially those in the Milky Way (MW), the Large Magellanic Cloud (LMC), and the Small Magellanic Cloud (SMC), have provided us with a clue to the dust properties in the nearby Universe. We examine whether or not these extinction curves can be explained by well known dust evolution processes. We treat the dust production in stellar ejecta, destruction in supernova shocks, dust growth by accretion and coagulation, and dust disruption by shattering. To make a survey of the large parameter space possible, we simplify the treatment of the grain size distribution evolution by adopting the 'two-size approximation', in which we divide the grain population into small ( < ∼ 0.03 µm) and large ( > ∼ 0.03 µm) grains. It is confirmed that the MW extinction curve can be reproduced in reasonable ranges for the time-scale of the above processes with a silicate-graphite mixture. This indicates that the MW extinction curve is a natural consequence of the dust evolution through the above processes. We also find that the same models fail to reproduce the SMC/LMC extinction curves. Nevertheless, this failure can be remedied by giving higher supernova destruction rates for small carbonaceous dust and considering amorphous carbon for carbonaceous dust; these modification fall in fact in line with previous studies. Therefore, we conclude that the current dust evolution scenario composed of the aforementioned processes is successful in explaining the extinction curves. All the extinction curves favor efficient interstellar processing of dust, especially, strong grain growth by accretion and coagulation.

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Section: Constraint On the Parametersmentioning

confidence: 83%

Dust evolution processes constrained by extinction curves in nearby galaxies

Hou

Hirashita

Michałowski

2016

Publications of the Astronomical Society of Japan

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“…By courtesy of S. Liljegren grated light of galaxies. Estimates suggest that AGB stars are a major source of dust in the Milky Way (e.g., Tielens 2005), but their contribution to dust production in the early universe is still debated (Michałowski 2015, and references therein). To asses the effects of AGB stars on their host galaxies requires, among other things, an understanding of how the mass-loss process depends on stellar metallicity.…”

Section: Stars On the Asymptotic Giant Branch: Evolution And Propertiesmentioning

confidence: 99%

Mass loss of stars on the asymptotic giant branch

Höfner

Olofsson

2018

Astron Astrophys Rev

440

376

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As low-and intermediate-mass stars reach the asymptotic giant branch (AGB), they have developed into intriguing and complex objects that are major players in the cosmic gas/dust cycle. At this stage, their appearance and evolution are strongly affected by a range of dynamical processes. Large-scale convective flows bring newlyformed chemical elements to the stellar surface and, together with pulsations, they trigger shock waves in the extended stellar atmosphere. There, massive outflows of gas and dust have their origin, which enrich the interstellar medium and, eventually, lead to a transformation of the cool luminous giants into white dwarfs. Dust grains forming in the upper atmospheric layers play a critical role in the wind acceleration process, by scattering and absorbing stellar photons and transferring their outward-directed momentum to the surrounding gas through collisions. Recent progress in high-angularresolution instrumentation, from the visual to the radio regime, is leading to valuable new insights into the complex dynamical atmospheres of AGB stars and their windforming regions. Observations are revealing asymmetries and inhomogeneities in the photospheric and dust-forming layers which vary on time-scales of months, as well as more long-lived large-scale structures in the circumstellar envelopes. High-angularresolution observations indicate at what distances from the stars dust condensation occurs, and they give information on the chemical composition and sizes of dust grains in the close vicinity of cool giants. These are essential constraints for building B Susanne Höfner

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“…Depending on the dust formation mechanism, it is argued that early galaxies have limited dust (e.g. Micha lowski 2015). Indeed, low dust attenuation is often assumed for high-redshift galaxies and is what is expected from the evolution of the colourmagnitude relation (Rogers et al 2014;Bouwens et al 2015).…”

Section: Shape Of the Rest-frame Uv Lf At Z = 8-9mentioning

confidence: 99%

A lack of evolution in the very bright end of the galaxy luminosity function from z ≃ 8 to 10

Bowler

Jarvis

Dunlop

et al. 2020

Monthly Notices of the Royal Astronomical Society

203

227

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We utilize deep near-infrared survey data from the UltraVISTA fourth data release (DR4) and the VIDEO survey, in combination with overlapping optical and Spitzer data, to search for bright star-forming galaxies at z 7.5. Using a full photometric redshift fitting analysis applied to the ∼ 6 deg 2 of imaging searched, we find 27 Lyman-break galaxies (LBGs), including 20 new sources, with best-fitting photometric redshifts in the range 7.4 < z < 9.1. From this sample we derive the rest-frame UV luminosity function (LF) at z = 8 and z = 9 out to extremely bright UV magnitudes (M UV −23) for the first time. We find an excess in the number density of bright galaxies in comparison to the typically assumed Schechter functional form derived from fainter samples. Combined with previous studies at lower redshift, our results show that there is little evolution in the number density of very bright (M UV ∼ −23) LBGs between z 5 and z 9. The tentative detection of an LBG with best-fit photometric redshift of z = 10.9 ± 1.0 in our data is consistent with the derived evolution. We show that a double power-law fit with a brightening characteristic magnitude (∆M * /∆z −0.5) and a steadily steepening bright-end slope (∆β/∆z −0.5) provides a good description of the z > 5 data over a wide range in absolute UV magnitude (−23 < M UV < −17). We postulate that the observed evolution can be explained by a lack of mass quenching at very high redshifts in combination with increasing dust obscuration within the first ∼ 1 Gyr of galaxy evolution.

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Dust production 680–850 million years after the Big Bang

Cited by 109 publications

References 117 publications

Dust evolution processes constrained by extinction curves in nearby galaxies

Dust evolution processes constrained by extinction curves in nearby galaxies

Mass loss of stars on the asymptotic giant branch

A lack of evolution in the very bright end of the galaxy luminosity function from z ≃ 8 to 10

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