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

Trčka, Ana; Baes, M.; Camps, Peter; Meidt, Sharon E.; Trayford, James W.; Bianchi, S.; Casasola, V.; Cassarà, L. P.; Looze, I. De; Vis, P. De; Dobbels, Wouter; Fritz, J.; Galametz, M.; Galliano, F.; Katsianis, Antonios; Madden, S.; Mosenkov, Aleksandr V.; Nersesian, Angelos; Viaene, S.; Xilouris, E. M.

doi:10.1093/mnras/staa857

Cited by 42 publications

(40 citation statements)

References 128 publications

(221 reference statements)

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“…Finally, it has been suggested that E may underestimate the FUV attenuation (Baes et al 2019). This may be a result of the constant dust-to-metals ratio governing the diffuse dust mass, the modelling of dust in HII regions (Trčka et al 2020), or the global star-dust geometry (e.g. Narayanan et al 2018;Salim & Narayanan 2020).…”

Section: Model Comparisonsmentioning

confidence: 99%

Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations

Lovell

Geach

Davé

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Matching the number counts of high-z submillimetre-selected galaxies (SMGs) has been a long-standing problem for galaxy formation models. In this paper, we use 3D dust radiative transfer to model the submm emission from galaxies in the simba cosmological hydrodynamic simulations, and compare predictions to the latest single-dish observational constraints on the abundance of 850 μm-selected sources. We find good agreement with the shape of the integrated 850 μm luminosity function, and the normalization is within 0.25 dex at >3 mJy, unprecedented for a fully cosmological hydrodynamic simulation, along with good agreement in the redshift distribution of bright SMGs. The agreement is driven primarily by simba’s good match to infrared measures of the star formation rate (SFR) function between z = 2 and 4 at high SFRs. Also important is the self-consistent on-the-fly dust model in simba, which predicts, on average, higher dust masses (by up to a factor of 2.5) compared to using a fixed dust-to-metals ratio of 0.3. We construct a light-cone to investigate the effect of far-field blending, and find that 52 per cent of sources are blends of multiple components, which makes a small contribution to the normalization of the bright end of the number counts. We provide new fits to the 850 μm luminosity as a function of SFR and dust mass. Our results demonstrate that solutions to the discrepancy between submm counts in simulations and observations, such as a top-heavy initial mass function, are unnecessary, and that submillimetre-bright phases are a natural consequence of massive galaxy evolution.

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Section: Model Comparisonsmentioning

confidence: 99%

Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations

Lovell

Geach

Davé

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…We leave for future work the effect of realistic non-spherical or complex structures, which could be treated by postprocessing simulated galaxies (e.g. Trčka et al 2020;Vogelsberger et al 2020).…”

Section: Galaxy Modelmentioning

confidence: 99%

“…Therefore, as mentioned in Section 2.2, we leave for future work the effect of realistic structures, which could be treated by post-processing simulated galaxies (e.g. Camps et al 2016Camps et al , 2018Trayford et al 2017;Trčka et al 2020;Liang et al 2018;Ma et al 2019;Vogelsberger et al 2020). Note that we realized the desired spatial distribution of dust using discrete particles (Section 2.3).…”

Section: Possible Other Effectsmentioning

confidence: 99%

Geometry effects on dust attenuation curves with different grain sources at high redshift

Lin

Hirashita

Camps

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Dust has been detected in high-redshift (z > 5) galaxies but its origin is still being debated. Dust production in high-redshift galaxies could be dominated by stellar production or by accretion (dust growth) in the interstellar medium. Previous studies have shown that these two dust sources predict different grain-size distributions, which lead to significantly different extinction curves. In this paper, by performing radiative transfer calculations, we investigate how the difference in the extinction curves affects the dust attenuation properties of galaxies. To examine the major effects of the dust–stars distribution geometry, we adopt two representative cases in spherical symmetry: the well-mixed geometry (stars and dust are homogeneously mixed) and the two-layer geometry (young stars are more concentrated in the centre). In both cases, we confirm that the attenuation curve can be drastically steepened by scattering and by different optical depths between young and old stellar populations, and can be flattened by the existence of unobscured stellar populations. We can reproduce similar attenuation curves even with very different extinction curves. Thus, we conclude that it is difficult to distinguish dust sources only with attenuation curves. However, if we include information on dust emission and plot the relation between infrared excess (IRX) and the ultraviolet spectral slope (β), then different dust sources predict different positions in the IRX–β diagram. A larger β is preferred under a similar IRX if dust growth is the dominant dust source.

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“…This is an expected behaviour, since the three ratios correlate with each other. Bianchi et al (2018) and Trčka et al (2020) showed a strong correlation of sSFR with f abs and the dust-to-stellar mass ratio, respectively. A correlation between f abs and the dust-to-stellar mass ratio is also expected, since the dust mass and stellar mass are calculated from their respective luminosities.…”

Section: Discussionmentioning

confidence: 94%

Probing the spectral shape of dust emission with the DustPedia galaxy sample

Nersesian

Dobbels

Xilouris

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The objective of this paper is to understand the variance of the far-infrared (FIR) spectral energy distribution (SED) of the DustPedia galaxies, and its link with the stellar and dust properties. An interesting aspect of the dust emission is the inferred FIR colours which could inform us about the dust content of galaxies, and how it varies with the physical conditions within galaxies. However, the inherent complexity of dust grains as well as the variety of physical properties depending on dust, hinder our ability to utilize their maximum potential. We use principal component analysis (PCA) to explore new hidden correlations with many relevant physical properties such as the dust luminosity, dust temperature, dust mass, bolometric luminosity, star-formation rate (SFR), stellar mass, specific SFR, dust-to-stellar mass ratio, the fraction of absorbed stellar luminosity by dust (fabs), and metallicity. We find that 95 per cent of the variance in our sample can be described by two principal components (PCs). The first component controls the wavelength of the peak of the SED, while the second characterises the width. The physical quantities that correlate better with the coefficients of the first two PCs, and thus control the shape of the FIR SED are: the dust temperature, the dust luminosity, the SFR, and fabs. Finally, we find a weak tendency for low-metallicity galaxies to have warmer and broader SEDs, while on the other hand high-metallicity galaxies have FIR SEDs that are colder and narrower.

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

Cited by 42 publications

References 128 publications

Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations

Reproducing submillimetre galaxy number counts with cosmological hydrodynamic simulations

Geometry effects on dust attenuation curves with different grain sources at high redshift

Probing the spectral shape of dust emission with the DustPedia galaxy sample

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