Dust grain size evolution in local galaxies: a comparison between observations and simulations
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Oxford University Press
ISM: dust, extinctionISM: evolutiongalaxies: abundancesgalaxies: evolutiongalaxies: star formationinfrared: ISM
M Relaño... [et al.]. Dust grain size evolution in local galaxies: a comparison between observations and simulations, Monthly Notices of the Royal Astronomical Society, Volume 515, Issue 4, October 2022, Pages 5306–5334, [https://doi.org/10.1093/mnras/stac2108]
SponsorshipMCIN/AEI PID2020-114414GB-100 Spanish Government AYA2017-84897-P; Junta de Andalucia P2000334 A-FQM-510-UGR20; FEDER/Junta de Andalucia-Consejeria de Transformacion Economica, Industria, Conocimiento y Universidades European Research Council (ERC) European Commission 851622; HPCI System Research Project hp200041 hp210090; Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT); Japan Society for the Promotion of Science; Grants-in-Aid for Scientific Research (KAKENHI) JP17H01111 19H05810 20H00180; Ministry of Science and Technology, China MOST 107-2923-M-001-003-MY3 MOST 108-2112-M-001-007-MY3; Academia Sinica - Taiwan AS-IA-109-M02; National Basic Research Program of China 2017YFA0402704; Comunidad de Madrid 2018-T1/TIC-11035
The evolution of the dust grain size distribution has been studied in recent years with great detail in cosmological hydrodynamical simulations taking into account all the channels under which dust evolves in the interstellar medium. We present a systematic analysis of the observed spectral energy distribution of a large sample of galaxies in the local Universe in order to derive not only the total dust masses but also the relative mass fraction between small and large dust grains ( D S / D L ). Simulations reproduce fairly well the observations except for the high-stellar mass regime where dust masses tend to be o v erestimated. We find that ∼45 per cent of galaxies exhibit D S / D L consistent with the expectations of simulations, while there is a subsample of massive galaxies presenting high D S / D L (log ( D S / D L ) ∼−0.5), and deviating from the prediction in simulations. For these galaxies which also have high-molecular gas mass fractions and metallicities, coagulation is not an important mechanism affecting the dust e volution. Including dif fusion, transporting large grains from dense regions to a more diffuse medium where they can be easily shattered, would explain the observed high D S / D L values in these galaxies. With this study, we reinforce the use of the small-to-large grain mass ratio to study the relative importance of the different mechanisms in the dust life cycle. Multiphase hydrodynamical simulations with detailed feedback prescriptions and more realistic subgrid models for the dense phase could help to reproduce the evolution of the dust grain size distribution traced by observations.