Dust evolution with MUPPI in cosmological volumes

Parente, Massimiliano; Ragone-Figueroa, Cinthia; Granato, G. L.; Borgani, S.; Murante, Giuseppe; Valentini, Milena; Bressan, A.; Lapi, A.

doi:10.1093/mnras/stac1913

Cited by 17 publications

(13 citation statements)

References 91 publications

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“…We note that this limitation prevents us from choosing more realistic yields based on expected elemental ratios; several previous investigations (e.g., Zhukovska et al 2008;Gjergo et al 2018;Granato et al 2021;Choban et al 2022;Parente et al 2022) have utilized the expectation that silicate dust is composed mainly of MgFeSiO 4 molecules to fix Mg:Fe:Si:O number ratios to 1:1:1:4, thus limiting the total dust mass that can be produced. This further motivates the systematic exploration of a wide range of y D values done in Section 3.1.1.…”

Section: Dust Production In Evolved Stars and Supernovaementioning

confidence: 99%

Modeling Dust Production, Growth, and Destruction in Reionization-era Galaxies with the CROC Simulations: Methods and Parameter Exploration

Esmerian

Gnedin

2022

ApJ

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We introduce a model for the explicit evolution of interstellar dust in a cosmological galaxy formation simulation. We post-process a simulation from the Cosmic Reionization on Computers project, integrating an ordinary differential equation for the evolution of the dust-to-gas ratio along pathlines in the simulation sampled with a tracer particle technique. This model incorporates the effects of dust grain production in asymptotic giant branch star winds and supernovae, grain growth due to the accretion of heavy elements from the gas phase of the interstellar medium, and grain destruction due to thermal sputtering in the high-temperature gas of supernova remnants due to thermal sputtering. A main conclusion of our analysis is the importance of a carefully chosen dust destruction model, for which different reasonable parameterizations can predict very different values at the ∼100 pc resolution of the interstellar medium (ISM) in our simulations. We run this dust model on the single most massive galaxy in a 10 h−1 comoving megaparsec box, which attains a stellar mass of ∼2 × 109 M ⊙ by z = 5. We find that the model is capable of reproducing dust masses and dust-sensitive observable quantities broadly consistent with existing data from high-redshift galaxies. The total dust mass in the simulated galaxy is somewhat sensitive to parameter choices for the dust model, especially the timescale for grain growth due to accretion in the ISM. Consequently, observable quantity observations that can constrain galaxy dust masses at these epochs are potentially useful for placing constraints on dust physics.

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Section: Dust Production In Evolved Stars and Supernovaementioning

confidence: 99%

Modeling Dust Production, Growth, and Destruction in Reionization-era Galaxies with the CROC Simulations: Methods and Parameter Exploration

Esmerian

Gnedin

2022

ApJ

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“…The dust formation and evolution model implemented in this work is conceptually similar to that implemented recently by our group (Gjergo et al 2018;Granato et al 2021;Parente et al 2022) in hydrodynamic simulations. However, here we adapt it to the semianalytic framework of L-G .…”

Section: Dust Production and Evolutionmentioning

confidence: 99%

“…As a result, the mass, chemical composition and size distribution of grains is a product of the interplay between the various processes, which in turn depend on the variety of physical conditions in the ISM (e.g. Aoyama et al 2017;Parente et al 2022).…”

Section: Introductionmentioning

confidence: 99%

“…This behaviour is still not clear from a theoretical point of view. Indeed, the relatively recent inclusion of dust in some semianalytic-models (Popping et al 2017;Vĳayan et al 2019;Triani et al 2020) and hydrodynamic cosmological simulations (McKinnon et al 2017;Aoyama et al 2018;Hou et al 2019;Li et al 2019;Graziani et al 2020;Parente et al 2022) of galaxy evolution, has made it possible to study the build-up of the DMF across cosmic epochs, investigating the role of the various processes shaping dust evolution in a cosmological context. However, most of the aforementioned works do not reproduce the observed peak of Ω ISM dust .…”

Section: Introductionmentioning

confidence: 99%

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The $z \lesssim 1$ drop of cosmic dust abundance in a semi-analytic framework

Parente¹,

Ragone-Figueroa²,

Granato³

et al. 2023

Preprint

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Observations suggest that the amount of galactic dust in the Universe decreased by a factor ∼ 2 − 3 during the last ∼ 8 Gyr. However, cosmological models of galaxy evolution usually struggle to explain this decrease. Here we use the semi-analytic model (SAM) L-G 2020 to show that this drop may be reproduced assuming standard prescriptions for dust production and evolution. We extend the SAM with i) a state-of-the-art dust model which adopts the two-size approximation and ii) a new disc instability criterion which triggers bulge and central black hole growth. The model reproduces some fundamental properties of the local galaxy population, such as the fraction of spheroid-dominated galaxies and some scaling relations involving dust. Moreover, the model predicts a galactic dust drop from 𝑧 ∼ 1 → 0, which becomes closer to the observed one when adopting the new treatment of disc instabilities. This result is related to the newly implemented super-massive black hole growth during disc instabilities, which enhances the quenching of massive galaxies. Consequently, these objects feature a lower gas and dust content. We provide a census of the contribution of all the processes affecting the galactic dust content. Accretion is the dominant dust mass growth process. Destruction by supernovae, astration and ejection by winds have all a non-negligible role in decreasing the overall dust content in galaxies below 𝑧 ∼ 1. We also discuss predictions concerning extra-galactic dust, confirming that a sputtering efficiency lower than the canonical one is required to match the few available observations.

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“…Cosmological simulations and isolated galaxy simulations with comparable resolution have started to include dust evolution models at different levels of sophistication (McKinnon et al 2017(McKinnon et al , 2018Aoyama et al 2017Aoyama et al , 2018Li et al 2019;Parente et al 2022;Lewis et al 2022;Romano et al 2022;Lower et al 2022). However, these simulations do not resolve either SN feedback or the density structure of the ISM, forcing them to adopt dust evolution models in a sub-grid fashion.…”

Section: Introductionmentioning

confidence: 99%

Co-evolution of Dust and Chemistry in Galaxy Simulations with a Resolved Interstellar Medium

Hu¹,

Sternberg²,

Dishoeck³

2023

Preprint

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Nearby dwarf irregular galaxies are ideal laboratories for studying the interstellar medium (ISM) at low metallicity, which is expected to be common for galaxies at very high redshift that will be observed by the James Webb Space Telescope. We present the first high-resolution (∼ 0.2 pc) hydrodynamical simulations of an isolated low-metallicity (0.1 Z ) dwarf galaxy coupled with a time-dependent chemistry network and a dust evolution model where dust is locally produced and destroyed by various processes. To accurately model carbon monoxide (CO), we post-process the simulations with a detailed chemistry network including the time-dependent effect of molecular hydrogen (H 2 ). Our model successfully reproduces the observed star formation rate and CO(1-0) luminosity (L CO ). We find that dust growth in dense gas is required to reproduce the observed L CO as otherwise CO would be completely photodissociated. In contrast, the H 2 abundance is extremely small and is insensitive to dust growth, leading to a CO-to-H 2 conversion factor similar to the Milky Way value despite the low metallicity. Observationally inferred dust-to-gas ratio is thus underestimated if adopting the metallicity-dependent CO-to-H 2 conversion factor. The newly-produced dust in dense gas mixes with the ISM through supernova feedback without being completely destroyed by sputtering, which leads to galactic outflows 20% -50% dustier than the ISM, providing a possible source for intergalactic dust.

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Dust evolution with MUPPI in cosmological volumes

Cited by 17 publications

References 91 publications

Modeling Dust Production, Growth, and Destruction in Reionization-era Galaxies with the CROC Simulations: Methods and Parameter Exploration

Modeling Dust Production, Growth, and Destruction in Reionization-era Galaxies with the CROC Simulations: Methods and Parameter Exploration

The $z \lesssim 1$ drop of cosmic dust abundance in a semi-analytic framework

Co-evolution of Dust and Chemistry in Galaxy Simulations with a Resolved Interstellar Medium

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