Dust grain size evolution in local galaxies: a comparison between observations and simulations

Relaño, M.; Saintonge, A.; Hou, Kuan-Chou; Romano, Leonard E. C.; Nagamine, Kentaro; Hirashita, Hiroyuki; Aoyama, Shohei; Lamperti, Isabella; Lisenfeld, U.; Smith, M.; Chastenet, Jérémy; Xiao, Ting; Gao, Yu; Sargent, M.; Giessen, S.A. van der

doi:10.1093/mnras/stac2108

Cited by 8 publications

(5 citation statements)

References 159 publications

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“…Vis et al 2017a)11 . Comparisons with the literature require to pay attention to derivation method of the involved quantities and this is particularly important for the dust mass whose values are strongly dependent on adopted SED fitting and dust model (see, e.g.,Relaño et al 2022). However, De Vis et al (2019) found that dust masses used in De Vis et al (2017a) derived with MAGPHYS (da Cunha et al 2008) and the DustPedia ones (see Sect.…”

mentioning

confidence: 95%

The resolved scaling relations in DustPedia: Zooming in on the local Universe

Casasola¹,

Bianchi²,

Magrini³

et al. 2022

A&A

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Aims. We perform a homogeneous analysis of an unprecedented set of spatially resolved scaling relations (SRs) between interstellar medium (ISM) components, that is to say dust, gas, and gas-phase metallicity, and other galaxy properties, such as stellar mass (M star ), total baryonic content, and star-formation rate (SFR), in a range of physical scales between 0.3 and 3.4 kpc. We also study some ratios between galaxy components: dust-to-stellar, dust-to-gas, and dust-to-metal ratios. Methods. We use a sample of 18 large, spiral, face-on DustPedia galaxies. The sample consists of galaxies with spatially resolved dust maps corresponding to 15 Herschel-SPIRE 500 µm resolution elements across the optical radius, with the morphological stage spanning from T = 2 to 8, M star from 2 × 10 9 to 1 × 10 11 M , SFR from 0.2 to 13 M yr −1 , and oxygen abundance from 12 + log(O/H) = 8.3 to 8.8. Results. All the SRs are moderate or strong correlations except the dust-Hi SR that does not exist or is weak for most galaxies. The SRs do not have a universal form but each galaxy is characterized by distinct correlations, affected by local processes and galaxy peculiarities. The SRs hold, on average, starting from the scale of 0.3 kpc, and if a breaking down scale exists it is below 0.3 kpc. By evaluating all galaxies together at the common scale of 3.4 kpc, differences due to peculiarities of individual galaxies are cancelled out and the corresponding SRs are consistent with those of whole galaxies. By comparing subgalactic and global scales, the most striking result emerges from the SRs involving ISM components: the dust-total gas SR is a good correlation at all scales, while the dust-H 2 and dust-Hi SRs are good correlations at subkiloparsec/kiloparsec and total scales, respectively. For the other explored SRs, there is a good agreement between small and global scales and this may support the picture where the main physical processes regulating the properties and evolution of galaxies occur locally. In this scenario, our results are consistent with the hypothesis of self-regulation of the star-formation process. The analysis of subgalactic ratios between galaxy components shows that they are consistent with those derived for whole galaxies, from low to high redshift, supporting the idea that also these ratios could be set by local processes. Conclusions. Our results highlight the heterogeneity of galaxy properties and the importance of resolved studies on local galaxies in the context of galaxy evolution. They also provide fundamental observational constraints to theoretical models and updated references for high-redshift studies.

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confidence: 95%

The resolved scaling relations in DustPedia: Zooming in on the local Universe

Casasola¹,

Bianchi²,

Magrini³

et al. 2022

A&A

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“…The models are also applied to nearby galaxies in order to extract the information on dust properties (e.g. Li & Draine 2002; Draine & Li ★ E-mail: hirashita@asiaa.sinica.edu.tw 2007; Galliano et al 2018;Relaño et al 2020Relaño et al , 2022. All these models are useful not only to understand dust extinction and emission but also to infer the dust composition and grain size distribution.…”

Section: Introductionmentioning

confidence: 99%

Evolution of grain size distribution with enhanced abundance of small carbonaceous grains in galactic environments

Hirashita

2022

Monthly Notices of the Royal Astronomical Society

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We propose an updated dust evolution model that focuses on the grain size distribution in a galaxy. We treat the galaxy as a one-zone object and include five main processes (stellar dust production, dust destruction in supernova shocks, grain growth by accretion and coagulation, and grain disruption by shattering). In this paper, we improve the predictions related to small carbonaceous grains, which are responsible for the 2175 Å bump in the extinction curve and the polycyclic aromatic hydrocarbon (PAH) emission features in the dust emission spectral energy distribution (SED), both of which were underpredicted in our previous model. In the new model, we hypothesize that small carbonaceous grains are not involved in interstellar processing. This avoids small carbonaceous grains being lost by coagulation. We find that this hypothetical model shows a much better match to the Milky Way (MW) extinction curve and dust emission SED than the previous one. The following two additional modifications further make the fit to the MW dust emission SED better: (i) The chemical enrichment model is adjusted to give a nearly solar metallicity in the present epoch, and the fraction of metals available for dust growth is limited to half. (ii) Aromatization for small carbonaceous grains is efficient, so that the aromatic fraction is unity at grain radii ≲ 20 Å. As a consequence of our modelling, we succeed in obtaining a dust evolution model that explains the MW extinction curve and dust emission SED at the same time.

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“…Observationally, the determination of the relative abundance of small and large grains may be estimated with SED fitting. This estimate has been done for a sample of local galaxies in two recent works by Relaño et al (2020) and Relaño et al (2022), whose results are shown in Fig. 9 together with our model predictions.…”

Section: Grain Sizesmentioning

confidence: 83%

“…We caution the reader about this comparison. Indeed, while in our two size approximation the transition from small to large grains occurs at 0.03 𝜇m, it occurs at 0.015 𝜇m in the model 16 adopted by Relaño et al (2020) and Relaño et al (2022). Moreover, they assume carbonaceous properties for small grains, while we also consider small grains to have a silicate composition.…”

Section: Grain Sizesmentioning

confidence: 90%

“…The relation between the observed Small-to-Large grain mass ratio (S-to-L) and stellar mass (left panel) exhibits e nearly flat trend with a median value of S-to-L∼ 0.2 − 0.3 and ∼ 0.7 dex dispersion. However, the more recent work by Relaño et al (2022), who made use of a significantly larger sample of galaxies, suggests a slowly decreasing trend of S-to-L with 𝑀 stars . The relationship between S-to-L and ISM metallicity (right panel) shows qualitatively similar behaviour.…”

Section: Grain Sizesmentioning

confidence: 95%

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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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Dust grain size evolution in local galaxies: a comparison between observations and simulations

Cited by 8 publications

References 159 publications

The resolved scaling relations in DustPedia: Zooming in on the local Universe

The resolved scaling relations in DustPedia: Zooming in on the local Universe

Evolution of grain size distribution with enhanced abundance of small carbonaceous grains in galactic environments

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

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