# RADIATIVE TRANSFER MODEL OF DUST ATTENUATION CURVES IN CLUMPY, GALACTIC ENVIRONMENTS

## Author(s): Seon, Kwang-Il; Draine, Bruce T.

To refer to this page use: http://arks.princeton.edu/ark:/88435/pr1zd87
DC FieldValueLanguage
dc.contributor.authorSeon, Kwang-Il-
dc.contributor.authorDraine, Bruce T.-
dc.date.accessioned2019-05-06T18:09:28Z-
dc.date.available2019-05-06T18:09:28Z-
dc.date.issued2016-12-20en_US
dc.identifier.citationSeon, Kwang-Il, Draine, Bruce T. (2016). RADIATIVE TRANSFER MODEL OF DUST ATTENUATION CURVES IN CLUMPY, GALACTIC ENVIRONMENTS. ASTROPHYSICAL JOURNAL, 833 (10.3847/1538-4357/833/2/201en_US
dc.identifier.issn0004-637X-
dc.identifier.urihttp://arks.princeton.edu/ark:/88435/pr1zd87-
dc.description.abstractThe attenuation of starlight by dust in galactic environments is investigated through models of radiative transfer in a spherical, clumpy interstellar medium (ISM). We show that the attenuation curves are primarily determined by the wavelength dependence of absorption rather than by the underlying extinction (absorption+scattering) curve; the observationally derived attenuation curves cannot constrain a unique extinction curve unless the absorption or scattering efficiency is specified. Attenuation curves consistent with the “Calzetti curve” are found by assuming the silicate-carbonaceous dust model for the Milky Way (MW), but with the 2175 angstrom bump suppressed or absent. The discrepancy between our results and previous work that claimed the Small Magellanic Cloud dust to be the origin of the Calzetti curve is ascribed to the difference in adopted albedos; we use the theoretically calculated albedos, whereas the previous works adopted albedos derived empirically from observations of reflection nebulae. It is found that the attenuation curves calculated with the MW dust model are well represented by a modified Calzetti curve with a varying slope and UV bump strength. The strong correlation between the slope and UV bump strength, as found in star-forming galaxies at 0.5 < z < 2.0, is well reproduced when the abundance of the UV bump carriers is assumed to be 30%-40% of that of the MW dust; radiative transfer effects lead to shallower attenuation curves with weaker UV bumps as the ISM is more clumpy and dustier. We also argue that some local starburst galaxies have a UV bump in their attenuation curves, albeit very weak.en_US
dc.language.isoen_USen_US
dc.relation.ispartofASTROPHYSICAL JOURNALen_US
dc.rightsFinal published version. Article is made available in OAR by the publisher's permission or policy.en_US
dc.titleRADIATIVE TRANSFER MODEL OF DUST ATTENUATION CURVES IN CLUMPY, GALACTIC ENVIRONMENTSen_US
dc.typeJournal Articleen_US
dc.identifier.doidoi:10.3847/1538-4357/833/2/201-
dc.date.eissued2016-12-19en_US
dc.identifier.eissn1538-4357-
pu.type.symplectichttp://www.symplectic.co.uk/publications/atom-terms/1.0/journal-articleen_US

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