Evolution of grain size distribution in galactic discs

Relaño, M.; Lisenfeld, U.; Hou, Kuan-Chou; Vílchez, J. M.; Kennicutt, Robert C.

doi:10.1051/0004-6361/201937087

Cited by 24 publications

(47 citation statements)

References 63 publications

(117 reference statements)

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“…As already remarked, with the present implementation we obtain low redshift values of 𝑆/𝐿 similar to those inferred from dust reprocessing models 0.2 − 0.3 (e.g. Silva et al 1998;Weingartner & Draine 2001;Relaño et al 2020), while C6_SharpShat runs predict in the last few Gyrs unsatisfactory values 𝑆/𝐿 0.05. McKinnon et al (2018) suggested that the ISM dust loss due to the formation of stars, that is the so-called astration, can be neglected in a full dust evolution model because other dust destruction mechanisms, in particular SNae destruction (Section 2.3.4), would largely dominate it.…”

Section: Sharp Shatteringsupporting

confidence: 86%

Dust evolution in zoom-in cosmological simulations of galaxy formation

Granato,

Ragone-Figueroa,

Taverna

et al. 2020

Preprint

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We present cosmological zoom-in hydro-dynamical simulations for the formation of disc galaxies, implementing dust evolution and dust promoted cooling of hot gas. We couple an improved version of our previous treatment of dust evolution, which adopts the twosize approximation to estimate the grain size distribution, with the MUPPI star formation and feedback sub-resolution model. Our dust evolution model follows carbon and silicate dust separately. To distinguish differences induced by the chaotic behaviour of simulations from those genuinely due to different simulation set-up, we run each model six times, after introducing tiny perturbations in the initial conditions. With this method, we discuss the role of various dust-related physical processes and the effect of a few possible approximations adopted in the literature.Metal depletion and dust cooling affect the evolution of the system, causing substantial variations in its stellar, gas and dust content. We discuss possible effects on the Spectral Energy Distribution of the significant variations of the size distribution and chemical composition of grains, as predicted by our simulations during the evolution of the galaxy. We compare dust surface density, dust-to-gas ratio and small-to-big grain mass ratio as a function of galaxy radius and gas metallicity predicted by our fiducial run with recent observational estimates for three disc galaxies of different masses. The general agreement is good, in particular taking into account that we have not adjusted our model for this purpose.

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Section: Sharp Shatteringsupporting

confidence: 86%

Dust evolution in zoom-in cosmological simulations of galaxy formation

Granato,

Ragone-Figueroa,

Taverna

et al. 2020

Preprint

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“…As before, however, the simulation of Hou et al (2019) still relies on a sub-grid treatment for the dense gas fraction. It is also interesting that the ratio between small-and large-grain abundances calculated by Hou et al (2019) is consistent with that derived from the dust emission SEDs of nearby galaxies (Relaño et al 2020). With empirical information on the grain size distribution and individual dust components, we could further calculate the IR SED by assuming a typical interstellar radiation field as heating source, which would enable a future comparison between our model results and observations.…”

Section: Other Simulations Of the Grain Size Distributionsupporting

confidence: 73%

Evolution of the grain size distribution in Milky Way-like galaxies in post-processed IllustrisTNG simulations

Yu-Hsiu

Hirashita

Hsu

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We model dust evolution in Milky Way-like galaxies by post-processing the IllustrisTNG cosmological hydrodynamical simulations in order to predict dust-to-gas ratios and grain size distributions. We treat grain-size-dependent dust growth and destruction processes using a 64-bin discrete grain size evolution model without spatially resolving each galaxy. Our model broadly reproduces the observed dust–metallicity scaling relation in nearby galaxies. The grain size distribution is dominated by large grains at z ≳ 3 and the small-grain abundance rapidly increases by shattering and accretion (dust growth) at z ≲ 2. The grain size distribution approaches the so-called MRN distribution at z ∼ 1, but a suppression of large-grain abundances occurs at z < 1. Based on the computed grain size distributions and grain compositions, we also calculate the evolution of the extinction curve for each Milky Way analogue. Extinction curves are initially flat at z > 2, and become consistent with the Milky Way extinction curve at z ≲ 1 at $1/\lambda < 6~{\rm \mu m}^{-1}$. However, typical extinction curves predicted by our model have a steeper slope at short wavelengths than is observed in the Milky Way. This is due to the low-redshift decline of gas-phase metallicity and the dense gas fraction in our TNG Milky Way analogues that suppresses the formation of large grains through coagulation.

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“…In addition to dust growth, models show that star formation history (Zhukovska 2014) and the change in dust size distributions (e.g. coagulation and shattering; Hirashita & Kuo 2011;Relaño et al 2020) also affect D/M. Simulations also suggest that the resolved D/M is correlated with a galaxy's gas fraction (f gas , the fraction of gas mass to the total gas and stellar mass) and stellar mass distribution (Hou et al 2019;Li et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Resolving the Dust-to-Metals Ratio and CO-to-H$_2$ Conversion Factor in the Nearby Universe

Chiang,

Sandstrom,

Chastenet

et al. 2020

Preprint

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We investigate the relationship between the dust-to-metals ratio (D/M) and the local interstellar medium environment at ∼2 kpc resolution in five nearby galaxies: IC342, M31, M33, M101, and NGC628. A modified blackbody model with a broken power-law emissivity is used to model the dust emission from 100 to 500 µm observed by Herschel. We utilize the metallicity gradient derived from auroral line measurements in HII regions whenever possible. Both archival and new CO rotational line and HI 21 cm maps are adopted to calculate gas surface density, including new wide field CO and HI maps for IC342 from IRAM and the VLA, respectively. We experiment with several prescriptions of CO-to-H 2 conversion factor, and compare the resulting D/M-metallicity and D/M-density correlations, both of which are expected to be non-negative from depletion studies. The D/M is sensitive to the choice of the conversion factor. The conversion factor prescriptions based on metallicity only yield too much molecular gas in the center of IC342 to obtain the expected correlations. Among the prescriptions tested, the one that yields the expected correlations depends on both metallicity and surface density. The 1-σ range of the derived D/M spans 0.40−0.58. Compared to chemical evolution models, our measurements suggest that the dust growth time scale is much shorter than the dust destruction time scale. The measured D/M is consistent with D/M in galaxy-integrated studies derived from infrared dust emission. Meanwhile, the measured D/M is systematically higher than the D/M derived from absorption, which likely indicates a systematic offset between the two methods.

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Evolution of grain size distribution in galactic discs

Cited by 24 publications

References 63 publications

Dust evolution in zoom-in cosmological simulations of galaxy formation

Dust evolution in zoom-in cosmological simulations of galaxy formation

Evolution of the grain size distribution in Milky Way-like galaxies in post-processed IllustrisTNG simulations

Resolving the Dust-to-Metals Ratio and CO-to-H$_2$ Conversion Factor in the Nearby Universe

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