Dust scaling relations in a cosmological simulation

Hou, Kuan-Chou; Aoyama, Shohei; Hirashita, Hiroyuki; Nagamine, Kentaro; Shimizu, Ikkoh

doi:10.1093/mnras/stz121

Cited by 77 publications

(177 citation statements)

References 120 publications

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“…Remarkably, the EAGLE SEDs fits agree well within the range of these observational relations, comparable to the previous studies that included cosmological simulations (e.g. Narayanan et al 2018a;Hou et al 2019). In general, star-forming EAGLE galaxies show the same trend as star-forming DustPedia galaxies.…”

Section: The Eagle Simulations and The Skirt Post-processingsupporting

confidence: 89%

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Reproducing the Universe: a comparison between the EAGLE simulations and the nearby DustPedia galaxy sample

Trčka

Baes

Camps

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We compare the spectral energy distributions (SEDs) and inferred physical properties for simulated and observed galaxies at low redshift. We exploit UV-submillimetre mock fluxes of ∼ 7000 z=0 galaxies from the EAGLE suite of cosmological simulations, derived using the radiative transfer code skirt. We compare these to ∼ 800 observed galaxies in the UV-submillimetre range, from the DustPedia sample of nearby galaxies. To derive global properties, we apply the SED fitting code cigale consistently to both data sets, using the same set of ∼ 80 million models. The results of this comparison reveal overall agreement between the simulations and observations, both in the SEDs and in the derived physical properties, with a number of discrepancies. The optical and far-infrared regimes, and the scaling relations based upon the global emission, diffuse dust and stellar mass, show high levels of agreement. However, the mid-infrared fluxes of the EAGLE galaxies are overestimated while the far-UV domain is not attenuated enough, compared to the observations. We attribute these discrepancies to a combination of galaxy population differences between the samples, and limitations in the subgrid treatment of star-forming regions in the EAGLE-skirt post-processing recipe. Our findings show the importance of detailed radiative transfer calculations and consistent comparison, and provide suggestions for improved numerical models.

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Section: The Eagle Simulations and The Skirt Post-processingsupporting

confidence: 89%

“…One approach adopted is to incorporate dust creation, growth, destruction and dynamics into simulations directly (McKinnon et al 2016(McKinnon et al , 2017Aoyama et al 2018Aoyama et al , 2019Hou et al 2019;Davé et al 2019). This, however is a very computationally expensive method, involving many processes that remain poorly understood.…”

Section: Introductionmentioning

confidence: 99%

Reproducing the Universe: a comparison between the EAGLE simulations and the nearby DustPedia galaxy sample

Trčka

Baes

Camps

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The strength of the 2175Å bump created by small graphite grains correlates with the steepness of the extinction curve. The above evolutionary trend confirms the evolution of grain size distribution calculated by one-zone models Hou et al 2016) and hydrodynamic simulations (Hou et al , 2019. Because a significant fraction of carbonaceous grains are aromatized for η dense = 0.5 and 0.1, the 2175Å bump is prominent.…”

Section: Extinction Curvessupporting

confidence: 82%

Self-consistent modelling of aromatic dust species and extinction curves in galaxy evolution

Hirashita

Murga

2020

Monthly Notices of the Royal Astronomical Society

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We formulate and calculate the evolution of dust in a galaxy focusing on the distinction among various dust components -silicate, aromatic carbon, and non-aromatic carbon. We treat the galaxy as a one-zone object and adopt the evolution model of grain size distribution developed in our previous work. We further include aromatization and aliphatization (inverse reaction of aromatization). We regard small aromatic grains in a radius range of 3-50Å as polycyclic aromatic hydrocarbons (PAHs). We also calculate extinction curves in a consistent manner with the abundances of silicate and aromatic and non-aromatic carbonaceous dust. Our model nicely explains the PAH abundance as a function of metallicity in nearby galaxies. The extinction curve become similar to the Milky Way curve at age ∼ 10 Gyr, in terms of the carbon bump strength and the far-ultraviolet slope. We also apply our model to starburst galaxies by shortening the star formation time-scale (0.5 Gyr) and increasing the dense-gas fraction (0.9), finding that the extinction curve maintains bumpless shapes (because of low aromatic fractions), which are similar to the extinction curves observed in the Small Magellanic Cloud and high-redshift quasars. Thus, our model successfully explains the variety in extinction curve shapes at low and high redshifts.

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“…Our predictions are compared with the results of Hou et al (2019) 14 (green lines) and of Popping et al (2017) (violet lines). Despite the agreement found in the cosmic dust density parameter (see Figure 1), the amplitude and slope of the DMF show significant variations across models.…”

Section: Dust Mass Functionmentioning

confidence: 80%

“…Our slopes are closer to the ones found by Popping et al (2017), but we find a smaller amplitude, probably as a result of less efficient grain growth in galaxies with low stellar mass (see discussion in Section 5.2.2). The differences with Hou et al (2019) are likely due to a combination of different simulation volumes/resolution 15 and sub-grid prescriptions for grain growth. In fact, the adopted rate has a similar functional form, but it is implemented in a different ISM phase.…”

Section: Dust Mass Functionmentioning

confidence: 99%

The assembly of dusty galaxies at z ≥ 4: statistical properties

Graziani

Schneider

Ginolfi

et al. 2020

Monthly Notices of the Royal Astronomical Society

103

104

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The recent discovery of high redshift dusty galaxies implies a rapid dust enrichment of their interstellar medium (ISM). To interpret these observations, we run a cosmological simulation in a 30h −1 cMpc/size volume down to z ≈ 4. We use the hydrodynamical code dustyGadget, which accounts for the production of dust by stellar populations and its evolution in the ISM. We find that the cosmic dust density parameter (Ω d ) is mainly driven by stellar dust at z 10, so that mass-and metallicity-dependent yields are required to assess the dust content in the first galaxies. At z 9 the growth of grains in the ISM of evolved systems (Log(M ⋆ /M ⊙ ) > 8.5) significantly increases their dust mass, in agreement with observations in the redshift range 4 z < 8. Our simulation shows that the variety of high redshift galaxies observed with ALMA can naturally be accounted for by modeling the grain-growth timescale as a function of the physical conditions in the gas cold phase. In addition, the trends of dust-to-metal (DTM) and dust-to-gas (D) ratios are compatible with the available data. A qualitative investigation of the inhomogeneous dust distribution in a representative massive halo at z ≈ 4 shows that dust is found from the central galaxy up to the closest satellites along polluted filaments with Log(D) −2.4, but sharply declines at distances d 30 kpc along many lines of sight, where Log(D) −4.0.

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Dust scaling relations in a cosmological simulation

Cited by 77 publications

References 120 publications

Reproducing the Universe: a comparison between the EAGLE simulations and the nearby DustPedia galaxy sample

Reproducing the Universe: a comparison between the EAGLE simulations and the nearby DustPedia galaxy sample

Self-consistent modelling of aromatic dust species and extinction curves in galaxy evolution

The assembly of dusty galaxies at z ≥ 4: statistical properties

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