High-resolution radiative transfer modelling of M33
Metadatos
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Oxford University Press
Materia
Radiative transfer Dust, extinction Galaxies: individual:M33 Galaxies: ISM Galaxies: star formation
Date
2019-05-24Referencia bibliográfica
Thomas G Williams, Maarten Baes, Ilse De Looze, Monica Relaño, Matthew W L Smith, Sam Verstocken, Sébastien Viaene, High-resolution radiative transfer modelling of M33, Monthly Notices of the Royal Astronomical Society, Volume 487, Issue 2, August 2019, Pages 2753–2770, [https://doi.org/10.1093/mnras/stz1441]
Patrocinador
Funding from the UK Science and Technology Facilities Council consolidated grant ST/K000926/1. M.R. acknowledges support by the research projects AYA2014-53506-P and AYA2017-84897P from the Spanish Ministerio de Economía y Competitividad. This research made use of MONTAGE (http://montage.ipac.caltech.edu/), which is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration’s Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of TechnologyRésumé
In this work, we characterize the contributions from both ongoing star formation and the
ambient radiation field in Local Group galaxy M33, as well as estimate the scale of the local
dust-energy balance (i.e. the scale at which the dust is re-emitting starlight generated in that
same region) in this galaxy through high-resolution radiative transfer (RT) modelling, with
defined stellar and dust geometries. We have characterized the spectral energy distribution
(SED) of M33 from UV to sub-mm wavelengths, at a spatial scale of 100 pc. We constructed
input maps of the various stellar and dust geometries for use in the RTmodelling. By modifying
our dust mix (fewer very small carbon grains and a lower silicate-to-carbon ratio as compared
to the Milky Way), we can much better fit the sub-mm dust continuum. Using this new dust
composition, we find that we are able to well reproduce the observed SED of M33 using our
adopted model. In terms of stellar attenuation by dust, we find a reasonably strong, broad
UV bump, as well as significant systematic differences in the amount of dust attenuation
when compared to standard SED modelling.We also find discrepancies in the residuals of the
spiral arms versus the diffuse interstellar medium (ISM), indicating a difference in properties
between these two regimes. The dust emission is dominated by heating due to the young stellar
populations at all wavelengths (∼80 per cent at 10 μm to ∼50 per cent at 1 mm). We find that
the local dust-energy balance is restored at spatial scales greater than around 1.5 kpc.