Expected dust grain-size distributions in galaxies detected by ALMA at z &gt; 7

Liu, Hsin-Ming; Hirashita, Hiroyuki

doi:10.1093/mnras/stz2647

Cited by 15 publications

(17 citation statements)

References 60 publications

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“…This finding is in agreement with other works in the literature in which the large amount of dust in Quasars at z > 6 is explained by adopting similar assumptions (Gall et al 2011a,b). This result is also in agreement with the work from Liu & Hirashita (2019) who find that most of the ALMA observations of galaxies at z > 7 can be explained by assuming a dust condensation fraction of ≈0.5 for stellar sources. In the local Universe, top-heavy IMFs have been adopted to explain some observational properties of ultra-compact dwarf galaxies (Dabringhausen et al 2012), ultrafaint dwarf galaxies (Geha et al 2013;McWilliam et al 2013) and Galactic globular clusters (Marks et al 2012).…”

Section: Discussionsupporting

confidence: 92%

The gas, metal, and dust evolution in low-metallicity local and high-redshift galaxies

Nanni

Burgarella

Theulé

et al. 2020

A&A

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Context. The chemical enrichment in the interstellar medium (ISM) of galaxies is regulated by several physical processes: star birth and death, grain formation and destruction, and galactic inflows and outflows. Understanding such processes and their relative importance is essential to following galaxy evolution and the chemical enrichment through the cosmic epochs, and to interpreting current and future observations. Despite the importance of such topics, the contribution of different stellar sources to the chemical enrichment of galaxies, for example massive stars exploding as Type II supernovae (SNe) and low-mass stars, as well as the mechanisms driving the evolution of dust grains, such as for example grain growth in the ISM and destruction by SN shocks, remain controversial from both observational and theoretical viewpoints. Aims. In this work, we revise the current description of metal and dust evolution in the ISM of local low-metallicity dwarf galaxies and develop a new description of Lyman-break galaxies (LBGs) which are considered to be their high-redshift counterparts in terms of star formation, stellar mass, and metallicity. Our goal is to reproduce the observed properties of such galaxies, in particular (i) the peak in dust mass over total stellar mass (sMdust) observed within a few hundred million years; and (ii) the decrease in sMdust at a later time. Methods. We fitted spectral energy distribution of dwarf galaxies and LBGs with the “Code Investigating GALaxies Emission”, through which the total stellar mass, dust mass, and star formation rate are estimated. For some of the dwarf galaxies considered, the metal and gas content are available from the literature. We computed different prescriptions for metal and dust evolution in these systems (e.g. different initial mass functions for stars, dust condensation fractions, SN destruction, dust accretion in the ISM, and inflow and outflow efficiency), and we fitted the properties of the observed galaxies through the predictions of the models. Results. Only some combinations of models are able to reproduce the observed trend and simultaneously fit the observed properties of the galaxies considered. In particular, we show that (i) a top-heavy initial mass function that favours the formation of massive stars and a dust condensation fraction for Type II SNe of around 50% or more help to reproduce the peak of sMdust observed after ≈100 Myr from the beginning of the baryon cycle for both dwarf galaxies and LBGs; (ii) galactic outflows play a crucial role in reproducing the observed decline in sMdust with age and are more efficient than grain destruction from Type II SNe both in local galaxies and at high-redshift; (iii) a star formation efficiency (mass of gas converted into stars) of a few percent is required to explain the observed metallicity of local dwarf galaxies; and (iv) dust growth in the ISM is not necessary in order to reproduce the values of sMdust derived for the galaxies under study, and, if present, the effect of this process would be erased by galactic outflows.

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Section: Discussionsupporting

confidence: 92%

The gas, metal, and dust evolution in low-metallicity local and high-redshift galaxies

Nanni

Burgarella

Theulé

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…This finding is in agreement with other works in the literature in which the large amount of dust in Quasars at z > 6 is explained by adopting similar assumptions (Gall et al 2011a,b). This result is also in agreement with the work from Liu & Hirashita (2019) who find that the most of the ALMA observations of galaxies at z > 7 can be explain by assuming a dust condensation fraction of ≈ 0.5 for stellar sources. In the local Universe, top-heavy IMF have been adopted to explain some observational properties of ultra compact dwarf galaxies (Dabringhausen et al 2012), ultra faint dwarf galaxies (Geha et al 2013;McWilliam et al 2013) and Galactic globular clusters (Marks et al 2012).…”

Section: Discussionsupporting

confidence: 93%

The gas, metal and dust evolution in low-metallicity local and high-redshift galaxies

Nanni,

Burgarella,

Theulé

et al. 2020

Preprint

Self Cite

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Context. The chemical enrichment in the interstellar medium (ISM) of galaxies is regulated by several physical processes: star birth and death, grain formation and destruction and galactic inflows and outflows. Understanding such processes and their relative importance is essential in order to follow galaxy evolution and the chemical enrichment through the cosmic epochs, and to interpret the current and future observations. Despite the importance of such topics, the contribution of different stellar sources to the chemical enrichment of galaxies, e.g. massive stars exploding as Type II supernovae (SNe) and low-mass stars, as well as the mechanisms driving the evolution of dust grains, e.g. grain growth in the ISM and destruction by SN shocks, remain controversial both on the observational and on the theoretical viewpoints. Aims. In this work, we revise the current description of metal and dust evolution in the ISM of local low-metallicity dwarf galaxies and we develop a new description of Lyman Break Galaxies (LBGs) that are considered to be their high-redshift counterparts in terms of star formation, stellar mass and metallicity. Our goal is to reproduce the observed properties of such galaxies, in particular i) the peak in the mass of dust over the mass of stars (sMdust) observed within few hundreds Myrs; ii) the decrease of sMdust at later time. Methods. The spectral energy distribution (SED) of dwarf galaxies and LBGs is fitted with the "Code Investigating GALaxies Emission" (CIGALE), through which the mass of stars, mass of dust and star formation rate are estimated. For some of the dwarf galaxies considered, the metal and gas content are available from the literature. We compute different prescriptions for metal and dust evolution in these systems (e.g. different initial mass functions for stars, dust condensation fractions, SN destruction, dust accretion in the ISM, inflow and outflow efficiency), and we fit the properties of the observed galaxies through the predictions of the models. Results. Only some combinations of models are able to reproduce the observed trend and to simultaneously fit the observed properties of the galaxies considered. In particular, we show that i) a top-heavy initial mass function that favours the formation of massive stars and a dust condensation fraction for Type II SNe around 50% or more help to reproduce the peak of sMdust observed after ≈100 Myrs since the beginning of the baryon cycle for both dwarf galaxies and LBGs; ii) galactic outflows play a crucial role in reproducing the observed decline in sMdust with age, and they are more efficient than grain destruction from Type II SNe both in local galaxies and at high-redshift; iii) a star formation efficiency (mass of gas converted into stars) of few per cent is required to explain the observed metallicity of local dwarf galaxies; iv) dust growth in the ISM is not necessary in order to reproduce the values of sMdust derived for the galaxies under study and, if present, the effect of this process would be erased by galactic ou...

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“…Polarization could also be important to predict, since it may also constrain the porosity (Draine & Hensley 2021b). We could also extend our predictions to high redshift galaxies to investigate the evolution of dust porosity as well as grain size distribution (see Liu & Hirashita 2019 for a model at high redshift) in the history of the Universe.…”

Section: Discussionmentioning

confidence: 88%

Remodelling the evolution of grain size distribution in galaxies

Hirashita

Aoyama

2018

Monthly Notices of the Royal Astronomical Society

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We revisit the evolution model of grain size distribution in a galaxy for the ultimate purpose of implementing it in hydrodynamical simulations. We simplify the previous model in such a way that some model-dependent assumptions are replaced with simpler functional forms. For the first test of the developed framework, we apply it to a onezone chemical evolution model of a galaxy, confirming that our new model satisfactorily reproduces the previous results and that efficient coagulation of small grains produced by shattering and accretion is essential in reproducing the so-called MRN grain size distribution. For the next step, in order to test if our model can be treated together with the hydrodynamical evolution of the interstellar medium (ISM), we post-process a hydrodynamical simulation of an isolated disc galaxy using the new grain evolution model. We sample hydrodynamical particles representing each of the dense and diffuse ISM phases. By this post-processing, we find that the processes occurring in the dense gas (grain growth by accretion and coagulation) are important in reproducing the grain size distribution consistent with the Milky Way extinction curve. In our model, the grain size distributions are similar between the dense and diffuse ISM, although we observe a larger dispersion in the dense ISM. Moreover, we also show that even if we degrade the grain radius resolution (with 16 grid points), the overall shape of grain size distribution (and of resulting extinction curve) can be captured.

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Expected dust grain-size distributions in galaxies detected by ALMA at z > 7

Cited by 15 publications

References 60 publications

The gas, metal, and dust evolution in low-metallicity local and high-redshift galaxies

The gas, metal, and dust evolution in low-metallicity local and high-redshift galaxies

The gas, metal and dust evolution in low-metallicity local and high-redshift galaxies

Remodelling the evolution of grain size distribution in galaxies

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