Remodelling the evolution of grain size distribution in galaxies

Hirashita, Hiroyuki; Aoyama, Shohei

doi:10.1093/mnras/sty2838

Cited by 60 publications

(42 citation statements)

References 143 publications

(284 reference statements)

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“…Dust is produced from the late stage of stellar evolution-namely supernovae (SNe) and stellar winds of asymptotic giant branch stars (e.g., Dwek 1998;Aoyama et al 2017;Gjergo et al 2018)grows in the interstellar medium (ISM), especially in dense molecular clouds (e.g., Hirashita & Voshchinnikov 2014); and is destroyed by SN shocks (e.g., Aoyama et al 2017). Such dust processes substantially alter the dust abundance and the size distribution of dust grains (e.g., Asano et al 2013;Aoyama et al 2017;Hirashita & Aoyama 2019) and hence affect the absorption and scattering of light (see Galliano 2018 for a review). Therefore, to better understand the formation and evolution of galaxies, we should know how and how much stellar light is reprocessed by the dust extinction/attenuation effect.…”

Section: Introductionmentioning

confidence: 99%

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

Lin

Kong

2020

ApJ

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The state-of-the-art geometry models of stars/dust suggest that dust attenuation toward nebular regions (A V,gas ) is always larger than that of stellar regions (A V,star ). Utilizing the newly released integral field spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory survey, we investigate whether and how the A V,star /A V,gas ratio varies from subgalactic to galactic scales. On a subgalactic scale, we report a stronger correlation between A V,star and A V,gas for more active H ii regions. The local A V,star /A V,gas is found to have moderate nonlinear correlations with three tracers of diffuse ionized gas (DIG), as well as indicators of gas-phase metallicity and ionization. The DIG regions tend to have larger A V,star /A V,gas compared to classic H ii regions excited by young OB stars. Metal-poor regions with a higher ionized level suffer much less nebular attenuation and thus have larger A V,star /A V,gas ratios. A low-A V,gas and high-A V,star /A V,gas sequence, which can be resolved into DIG-dominated and metal-poor regions, on the three BPT diagrams is found. Based on these observations, we suggest that besides the geometry of stars/dust, local physical conditions such as metallicity and ionized level also play an important role in determining the A V,star /A V,gas . On a galactic scale, the global A V,star /A V,gas ratio has strong correlations with stellar mass (M * ), moderate correlations with star formation rate (SFR) and metallicity, and weak correlations with inclination and specific SFR. Galaxies with larger M * and higher SFR that are more metal-rich tend to have smaller A V,star /A V,gas ratios. Such correlations form a decreasing trend of A V,star /A V,gas along the star-forming main sequence and mass-metallicity relation. The dust growth process accompanied by galaxy growth might be one plausible explanation for our observations.

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Section: Introductionmentioning

confidence: 99%

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

Lin

Kong

2020

ApJ

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“…An accurate description of the dust content and the grain size distribution would require to follow in detail the processes involved in the grains formation and destruction, whose efficiency depends on the local gas physical conditions, such as density, temperature, metallicity (see e.g. Hirashita & Aoyama 2019;Aoyama et al 2020). This detailed treatment of the dust physics is beyond the scope of our work.…”

Section: Discussionmentioning

confidence: 99%

“…Gaskell et al 2004;Czerny et al 2004;Gallerani et al 2010) and justified by theoretical models (e.g. Hirashita & Aoyama 2019;Nozawa et al 2015).…”

Section: Comparison With Quasar Datamentioning

confidence: 93%

“…Later on, similar models have been developed (e.g. Hirashita 2015;Nozawa et al 2015;Hirashita & Aoyama 2019), and they have been used to make predictions for extinction curves of high-redshift galaxies. However, despite these efforts, many uncertainties in the theoretical models remain and a complete picture of the dust properties at high redshift is still missing.…”

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confidence: 99%

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The dust attenuation law in z ∼ 6 quasars

Mascia

Gallerani

Ferrara

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We investigate the attenuation law in z ∼ 6 quasars by combining cosmological zoom-in hydrodynamical simulations of quasar host galaxies, with multi-frequency radiative transfer calculations. We consider several dust models differing in terms of grain size distributions, dust mass and chemical composition, and compare the resulting synthetic Spectral Energy Distributions (SEDs) with data from bright, early quasars. We show that only dust models with grain size distributions in which small grains ($a\lesssim 0.1~\mu {\rm m}$, corresponding to $\approx 60{{\ \rm per\ cent}}$ of the total dust mass) are selectively removed from the dusty medium provide a good fit to the data. Removal can occur if small grains are efficiently destroyed in quasar environments and/or early dust production preferentially results in large grains. Attenuation curves for these models are close to flat, and consistent with recent data; they correspond to an effective dust-to-metal ratio fd ≃ 0.38, i.e. close to the Milky Way value.

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“…Since there is no available physical model for the fragment mass distribution in rotational disruption, we use the fragment distribution function in shattering as a guide. The maximum and minimum masses of the fragments produced from a grain mass m 1 are assumed to be m f,max = 0.02m 1 and m f,min = 10 −6 m f,max , respectively (Guillet et al 2011;Hirashita & Aoyama 2019). We adopt the following mass distribution function of fragments produced from a grain with mass m 1 : The above fragment mass distribution could be optimistic in the number of small fragments, but we basically adopt it to investigate a possibility of rotational disruption being an alternative to shattering for small-grain production.…”

Section: Effect Of Rotational Disruptionmentioning

confidence: 99%

Effects of rotational disruption on the evolution of grain size distribution in galaxies

Hirashita

Hoang

2020

Monthly Notices of the Royal Astronomical Society

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Interstellar dust grains can be spun up by radiative torques, and the resulting centrifugal force may be strong enough to disrupt large dust grains. We examine the effect of this rotational disruption on the evolution of grain size distribution in galaxies. To this goal, we modify our previous model by assuming that rotational disruption is the major small-grain production mechanism. We find that rotational disruption can have a large influence on the evolution of grain size distribution in the following two aspects especially for composites and grain mantles (with tensile strength ∼ 10 7 erg cm −3 ). First, because of the short time-scale of rotational disruption, the smallgrain production occurs even in the early phase of galaxy evolution. Therefore, even though stars produce large grains, the abundance of small grains can be large enough to steepen the extinction curve. Secondly, rotational disruption is important in determining the maximum grain radius, which regulates the steepness of the extinction curve. For compact grains with tensile strength 10 9 erg cm −3 , the size evolution is significantly affected by rotational disruption only if the radiation field is as strong as (or the dust temperature is as high as) expected for starburst galaxies. For compact grains, rotational disruption predicts that the maximum grain radius becomes less than 0.2 µm for galaxies with a dust temperature 50 K.

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Remodelling the evolution of grain size distribution in galaxies

Cited by 60 publications

References 143 publications

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

The dust attenuation law in z ∼ 6 quasars

Effects of rotational disruption on the evolution of grain size distribution in galaxies

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