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Spatially resolving the dust properties and submillimetre excess in M 33

hal.structure.identifierDpto. Fisica Teorica y del Cosmos
dc.contributor.authorRELANO, M.
hal.structure.identifierSterrenkundig Observatorium
dc.contributor.authorDE LOOZE, I.
hal.structure.identifierInstitute of Astronomy [Cambridge]
dc.contributor.authorKENNICUTT, R. C.
hal.structure.identifierDepartamento Física Teórica y del Cosmos
dc.contributor.authorLISENFELD, U.
hal.structure.identifierInstitute of Astronomy [Cambridge]
dc.contributor.authorDARIUSH, A.
hal.structure.identifierDepartamento Física Teórica y del Cosmos
dc.contributor.authorVERLEY, S.
hal.structure.identifierFORMATION STELLAIRE 2018
dc.contributor.authorBRAINE, J.
hal.structure.identifierInstitut für Physik [Potsdam]
dc.contributor.authorTABATABAEI, F.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorKRAMER, C.
hal.structure.identifierUnidad de Astronomia
dc.contributor.authorBOQUIEN, M.
hal.structure.identifierInstitute for Astronomy, Astrophysics, Space Applications and Remote Sensing [Penteli] [IAASARS]
dc.contributor.authorXILOURIS, M.
hal.structure.identifierAMOR 2018
dc.contributor.authorGRATIER, P.
dc.date.issued2018
dc.identifier.issn0004-6361
dc.description.abstractEnThe relative abundance of the dust grain types in the interstellar medium (ISM) is directly linked to physical quantities that trace the evolution of galaxies. We study the dust properties of the whole disc of M33 at spatial scales of ~170 pc. This analysis allows us to infer how the relative dust grain abundance changes with the conditions of the ISM, study the existence of a submillimetre excess and look for trends of the gas-to-dust mass ratio (GDR) with other physical properties of the galaxy. For each pixel in the disc of M33 we fit the infrared SED using a physically motivated dust model that assumes an emissivity index beta close to 2. We derive the relative amount of the different dust grains in the model, the total dust mass, and the strength of the interstellar radiation field (ISRF) heating the dust at each spatial location. The relative abundance of very small grains tends to increase, and for big grains to decrease, at high values of Halpha luminosity. This shows that the dust grains are modified inside the star-forming regions, in agreement with a theoretical framework of dust evolution under different physical conditions. The radial dependence of the GDR is consistent with the shallow metallicity gradient observed in this galaxy. The strength of the ISRF derived in our model correlates with the star formation rate in the galaxy in a pixel by pixel basis. Although this is expected it is the first time that a correlation between both quantities is reported. We produce a map of submillimetre excess in the 500 microns SPIRE band for the disc of M33. The excess can be as high as 50% and increases at large galactocentric distances. We further study the relation of the excess with other physical properties of the galaxy and find that the excess is prominent in zones of diffuse ISM outside the main star-forming regions, where the molecular gas and dust surface density are low.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enSpatially resolving the dust properties and submillimetre excess in M 33
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201732347
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1801.04806
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A43
bordeaux.volume613
bordeaux.peerReviewedoui
hal.identifierhal-01685186
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01685186v1
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