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dc.contributor.authorLaw, Ka-Hei*
dc.contributor.authorGordon, Karl D.*
dc.contributor.authorMisselt, Karl A.*
dc.date.accessioned2018-07-24T23:27:56Z
dc.date.available2018-07-24T23:27:56Z
dc.date.issued2018-06
dc.identifier.citationKa-Hei Law et al 2018 ApJS 236 32en_US
dc.identifier.issn1538-4365
dc.identifier.doi10.3847/1538-4365/aabf41
dc.identifier.urihttp://hdl.handle.net/10150/628292
dc.description.abstractUnderstanding the properties of stellar populations and interstellar dust has important implications for galaxy evolution. In normal star-forming galaxies, stars and the interstellar medium dominate the radiation from ultraviolet (UV) to infrared (IR). In particular, interstellar dust absorbs and scatters UV and optical light, re-emitting the absorbed energy in the IR. This is a strongly nonlinear process that makes independent studies of the UV-optical and IR susceptible to large uncertainties and degeneracies. Over the years, UV to IR spectral energy distribution (SED) fitting utilizing varying approximations has revealed important results on the stellar and dust properties of galaxies. Yet the approximations limit the fidelity of the derived properties. There is sufficient computer power now available that it is now possible to remove these approximations and map out of landscape of galaxy SEDs using full dust radiative transfer. This improves upon previous work by directly connecting the UV, optical, and IR through dust grain physics. We present the DIRTYGrid, a grid of radiative transfer models of SEDs of dusty stellar populations in galactic environments designed to span the full range of physical parameters of galaxies. Using the stellar and gas radiation input from the stellar population synthesis model PEGASE, our radiative transfer model DIRTY self-consistently computes the UV to far-IR/sub-mm SEDs for each set of parameters in our grid. DIRTY computes the dust absorption, scattering, and emission from the local radiation field and a dust grain model, thereby physically connecting the UV-optical to the IR. We describe the computational method and explain the choices of parameters in DIRTYGrid. The computation took millions of CPU hours on supercomputers, and the SEDs produced are an invaluable tool for fitting multi-wavelength data sets. We provide the complete set of SEDs in an online table.en_US
dc.description.sponsorshipNASA ADAP [11-ADAP11-0112]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0067-0049/236/i=2/a=32?key=crossref.95240dadac1f094ed4e22de77c9f4223en_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.subjectdust,extinctionen_US
dc.subjectgalaxies: star formationen_US
dc.subjectmethods: numericalen_US
dc.titleDirtyGrid I: 3D Dust Radiative Transfer Modeling of Spectral Energy Distributions of Dusty Stellar Populationsen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTROPHYSICAL JOURNAL SUPPLEMENT SERIESen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal Supplement Series
dc.source.volume236
dc.source.issue2
dc.source.beginpage32
refterms.dateFOA2018-07-24T23:27:56Z


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