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hal.structure.identifierDepartment of Astronomy [Ithaca]
dc.contributor.authorADAMS, J. D.,
hal.structure.identifierDepartment of Astronomy [Ithaca]
dc.contributor.authorHERTER, T. L.,
dc.contributor.authorHORA, J. L.,
hal.structure.identifierKOSMA, I. Physikalisches Institut
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierCity University of Hong Kong [Hong Kong] [CUHK]
dc.contributor.authorLAU, R. M.,
dc.contributor.authorSTAUGHN, J. G.,
dc.contributor.authorSIMON, R.,
hal.structure.identifierDepartment of Epidemiology, University of Washington
hal.structure.identifierSeattle Epidemiologic Research and Information Center of the Department of Veterans Affairs Office of Research and Development
dc.contributor.authorSMITH, N.,
dc.contributor.authorGEHRZ, R. D.,
dc.contributor.authorALLEN, L. E.,
hal.structure.identifierFORMATION STELLAIRE 2015
dc.contributor.authorBONTEMPS, Sylvain
dc.contributor.authorCAREY, S. J.,
hal.structure.identifierUSDA, Plant Genet Resources Unit
dc.contributor.authorFAZIO, G. G.,
dc.contributor.authorGUTERMUTH, R. A.,
dc.contributor.authorGUZMAN FERNANDEZ, A.,
hal.structure.identifierGeneral Practice
dc.contributor.authorHANKINS, M.,
hal.structure.identifierJoint ALMA Observatory [JAO]
dc.contributor.authorHILL, T.,
dc.contributor.authorKETO, E.,
dc.contributor.authorKOENIG, X. P.,
dc.contributor.authorKRAEMER, K. E.,
dc.contributor.authorMEGEATH, S. T.,
dc.contributor.authorMIZUNO, D. R.,
hal.structure.identifierProcédés, Matériaux et Energie Solaire [PROMES]
dc.contributor.authorMOTTE, F.,
dc.contributor.authorMYERS, P. C.,
hal.structure.identifierMiami University [Ohio] [MU]
dc.contributor.authorSMITH, H. A.,
dc.date.issued2015-10
dc.identifier.issn0004-637X
dc.description.abstractEnWe present mid-IR (19 - 37 microns) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6 - 8.0 microns), IRTF/MIRLIN (11.3 and 12.5 microns), and Herschel/PACS (70 and 160 microns). We use these observations, observations in the literature, and radiation transfer modeling to study the heating and composition of the warm (~ 100 K) dust in the region. The dust is heated radiatively by the source S106 IR, with little contributions from grain-electron collisions and Ly-alpha radiation. The dust luminosity is >~ (9.02 +/- 1.01) x 10^4 L_sun, consistent with heating by a mid- to late-type O star. We find a temperature gradient (~ 75 - 107 K) in the lobes, which is consistent with a dusty equatorial geometry around S106 IR. Furthermore, the SOFIA observations resolve several cool (~ 65 - 70 K) lanes and pockets of warmer (~ 75 - 90 K) dust in the ionization shadow, indicating that the environment is fragmented. We model the dust mass as a composition of amorphous silicates, amorphous carbon, big grains, very small grains, and PAHs. We present the relative abundances of each grain component for several locations in S106.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.title.enSOFIA/FORCAST Observations of Warm Dust in S106: A Fragmented Environment
dc.typeArticle de revue
dc.identifier.doi10.1088/0004-637X/814/1/54
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1510.04360
bordeaux.journalThe Astrophysical Journal
bordeaux.pageid. 54
bordeaux.volume814
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-01217944
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01217944v1
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