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dc.contributor.authorPohlen, M.
dc.contributor.authorCortese, L.
dc.contributor.authorSmith, M. W. L.
dc.contributor.authorEales, S. A.
dc.contributor.authorBoselli, A.
dc.contributor.authorBendo, G. J.
dc.contributor.authorGomez, H. L.
dc.contributor.authorPapageorgiou, A.
dc.contributor.authorAuld, R.
dc.contributor.authorBaes, M.
dc.contributor.authorBock, J. J.
dc.contributor.authorBradford, M.
dc.contributor.authorBuat, V.
dc.contributor.authorCastro-Rodriguez, N.
dc.contributor.authorChanial, P.
dc.contributor.authorCharlot, S.
dc.contributor.authorCiesla, L.
dc.contributor.authorClements, D. L.
dc.contributor.authorCooray, A.
dc.contributor.authorCormier, D.
dc.contributor.authorDwek, E.
dc.contributor.authorEales, S. A.
dc.contributor.authorElbaz, D.
dc.contributor.authorGalametz, M.
dc.contributor.authorGalliano, F.
dc.contributor.authorGear, W. K.
dc.contributor.authorGlenn, J.
dc.contributor.authorGriffin, M.
dc.contributor.authorHony, S.
dc.contributor.authorIsaak, K. G.
dc.contributor.authorLevenson, L. R.
dc.contributor.authorLu, N.
dc.contributor.authorMadden, S.
dc.contributor.authorO'Halloran, B.
dc.contributor.authorOkumura, K.
dc.contributor.authorOliver, S.
dc.contributor.authorPage, M. J.
dc.contributor.authorPanuzzo, P.
dc.contributor.authorParkin, T. J.
dc.contributor.authorPerez-Fournon, I.
dc.contributor.authorRangwala, N.
dc.contributor.authorRigby, E. E.
dc.contributor.authorRoussel, H.
dc.contributor.authorRykala, A.
dc.contributor.authorSacchi, N.
dc.contributor.authorSauvage, M.
dc.contributor.authorSchulz, B.
dc.contributor.authorSchirm, M. R. P.
dc.contributor.authorSmith, M. W. L.
dc.contributor.authorSpinoglio, L.
dc.contributor.authorStevens, Jason
dc.contributor.authorSrinivasan, S.
dc.contributor.authorSymeonidis, M.
dc.contributor.authorTrichas, M.
dc.contributor.authorVaccari, M.
dc.contributor.authorVigroux, L.
dc.contributor.authorWilson, C. D.
dc.contributor.authorWozniak, H.
dc.contributor.authorWright, G. S.
dc.contributor.authorZeilinger, W. W.
dc.date.accessioned2012-01-31T10:01:02Z
dc.date.available2012-01-31T10:01:02Z
dc.date.issued2010-07-01
dc.identifier.citationPohlen , M , Cortese , L , Smith , M W L , Eales , S A , Boselli , A , Bendo , G J , Gomez , H L , Papageorgiou , A , Auld , R , Baes , M , Bock , J J , Bradford , M , Buat , V , Castro-Rodriguez , N , Chanial , P , Charlot , S , Ciesla , L , Clements , D L , Cooray , A , Cormier , D , Dwek , E , Eales , S A , Elbaz , D , Galametz , M , Galliano , F , Gear , W K , Glenn , J , Griffin , M , Hony , S , Isaak , K G , Levenson , L R , Lu , N , Madden , S , O'Halloran , B , Okumura , K , Oliver , S , Page , M J , Panuzzo , P , Parkin , T J , Perez-Fournon , I , Rangwala , N , Rigby , E E , Roussel , H , Rykala , A , Sacchi , N , Sauvage , M , Schulz , B , Schirm , M R P , Smith , M W L , Spinoglio , L , Stevens , J , Srinivasan , S , Symeonidis , M , Trichas , M , Vaccari , M , Vigroux , L , Wilson , C D , Wozniak , H , Wright , G S & Zeilinger , W W 2010 , ' Radial distribution of gas and dust in spiral galaxies : the case of M 99 (NGC 4254) and M 100 (NGC 4321) ' , Astronomy and Astrophysics , vol. 518 , L72 . https://doi.org/10.1051/0004-6361/201014554
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 516980
dc.identifier.otherPURE UUID: a40ff3b9-fde3-4383-b392-f192e655f37b
dc.identifier.otherBibtex: urn:e91e09483f1527e7a4ef400dd5314f88
dc.identifier.otherScopus: 77957771111
dc.identifier.urihttp://hdl.handle.net/2299/7750
dc.description.abstractBy combining Herschel-SPIRE data with archival Spitzer, H i , and CO maps, we investigate the spatial distribution of gas and dust in the two famous grand-design spirals M 99 and M 100 in the Virgo cluster. Thanks to the unique resolution and sensitivity of the Herschel-SPIRE photometer, we are for the first time able to measure the distribution and extent of cool, submillimetre (submm)-emitting dust inside and beyond the optical radius. We compare this with the radial variation in both the gas mass and the metallicity. Although we adopt a model-independent, phenomenological approach, our analysis provides important insights. We find the dust extending to at least the optical radius of the galaxy and showing breaks in its radial profiles at similar positions as the stellar distribution. The colour indices f350/f500 and f250/f350 decrease radially consistent with the temperature decreasing with radius. We also find evidence of an increasing gas to dust ratio with radius in the outer regions of both galaxies.en
dc.format.extent5
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rightsOpen
dc.subjectgalaxies: structure, galaxies: individual: M 99, galaxies: individual: M 100, infrared: galaxies, ISM: dust, extinction, submillimetre: galaxies
dc.titleRadial distribution of gas and dust in spiral galaxies : the case of M 99 (NGC 4254) and M 100 (NGC 4321)en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2010-07-01
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201014554
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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