Dust spectral energy distributions in Milky Way-like galaxies in the IllustrisTNG simulations based on the evolution of grain size distribution

Chang, Chiung-Yin; Yu-Hsiu, Huang,; Hirashita, Hiroyuki; Cooper, Andrew P.

doi:10.1093/mnras/stac995

Cited by 4 publications

(2 citation statements)

References 89 publications

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“…The data are taken by the Diffuse Infrared Background Experiment (DIRBE) instrument on the Cosmic Background Explorer (COBE) and instruments onboard Herschel. The same data for the IR SED were also used for comparison in our previous dust evolution models Chang et al 2022). In addition, since the above broad-band data do not really reflect the height of PAH emission features, we also refer to the spectroscopic data taken by the Infrared Space Observatory (ISO) shown by Compiègne et al (2011), originally from Flagey et al (2006).…”

Section: Observational Data For Comparisonmentioning

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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Section: Observational Data For Comparisonmentioning

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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“…Narayanan et al 2018;Lin et al 2021) or to dust emission SEDs in the IR with an appropriate modelling of interstellar radiation field intensity (e.g. Relaño et al 2020;Chang et al 2022;Nishida et al 2022). This step is useful for comparison with observational data at various redshifts (e.g.…”

Section: Discussionmentioning

confidence: 99%

Cosmic evolution of grain size distribution in galaxies using the $ν^2$GC semi-analytic model

Makiya,

Hirashita

2022

Preprint

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We investigate the cosmological evolution of interstellar dust with a semi-analytical galaxy formation model (𝜈 2 GC), focusing on the evolution of grain size distribution. The model predicts the statistical properties of dust mass and grain size distribution in galaxies across cosmic history. We confirm that the model reproduces the relation between dust-to-gas ratio and metallicity in the local Universe, and that the grain size distributions of the Milky Way (MW)-like sample become similar to the so-called MRN distribution that reproduces the observed MW extinction curve. Our model, however, tends to overpredict the dust mass function at the massive end at redshift 𝑧 0.8 while it reproduces the abundance of dusty galaxies at higher redshifts. We also examine the correlation between grain size distribution and galaxy properties (metallicity, specific star formation rate, gas fraction, and stellar mass), and observe a clear trend of large-grain-dominated, small-grain-dominated, and MRN-like grain size distributions from unevolved to evolved stages. As a consequence, the extinction curve shapes are flat, steep, and intermediate (MW-like) from the unevolved to evolved phases. At a fixed metallicity, the grain size distribution tends to have larger fractions of small grains at lower redshift; accordingly, the extinction curve tends to be steeper at lower redshift. We also predict that supersolar-metallicity objects at high redshift have flat extinction curves with weak 2175 Å bump strength.

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Cosmic evolution of grain size distribution in galaxies using the ν2GC semi-analytical model

Makiya

Hirashita

2022

Monthly Notices of the Royal Astronomical Society

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We investigate the cosmological evolution of interstellar dust with a semi-analytical galaxy formation model (ν2GC), focusing on the evolution of grain size distribution. The model predicts the statistical properties of dust mass and grain size distribution in galaxies across cosmic history. We confirm that the model reproduces the relation between dust-to-gas ratio and metallicity in the local Universe, and that the grain size distributions of the Milky Way (MW)-like sample become similar to the so-called MRN distribution that reproduces the observed MW extinction curve. Our model, however, tends to overpredict the dust mass function at the massive end at redshift z ≲ 0.8 while it reproduces the abundance of dusty galaxies at higher redshifts. We also examine the correlation between grain size distribution and galaxy properties (metallicity, specific star formation rate, gas fraction, and stellar mass), and observe a clear trend of large-grain-dominated, small-grain-dominated, and MRN-like grain size distributions from unevolved to evolved stages. As a consequence, the extinction curve shapes are flat, steep, and intermediate (MW-like) from the unevolved to evolved phases. At a fixed metallicity, the grain size distribution tends to have larger fractions of small grains at lower redshift; accordingly, the extinction curve tends to be steeper at lower redshift. We also predict that supersolar-metallicity objects at high redshift have flat extinction curves with weak 2175 Å bump strength.

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Dust spectral energy distributions in Milky Way-like galaxies in the IllustrisTNG simulations based on the evolution of grain size distribution

Cited by 4 publications

References 89 publications

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

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

Cosmic evolution of grain size distribution in galaxies using the $ν^2$GC semi-analytic model

Cosmic evolution of grain size distribution in galaxies using the ν2GC semi-analytical model

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