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The dust morphology of the elliptical Galaxy M 86 with SPIRE

dc.contributor.authorGomez, H.L.
dc.contributor.authorBaes, M.
dc.contributor.authorCortese, L.
dc.contributor.authorSmith, M. W. L.
dc.contributor.authorBoselli, A.
dc.contributor.authorCiesla, L.
dc.contributor.authorBendo, G. J.
dc.contributor.authorPohlen, M.
dc.contributor.authordi Serego Alighieri, S.
dc.contributor.authorAuld, R.
dc.contributor.authorBarlow, M.J.
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.authorClements, D. L.
dc.contributor.authorCooray, A.
dc.contributor.authorCormier, D.
dc.contributor.authorDavies, J. I.
dc.contributor.authorDwek, E.
dc.contributor.authorEales, S.
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.authorPapageorgiou, A.
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.authorSchirm, M. R. P.
dc.contributor.authorSchulz, B.
dc.contributor.authorSpinoglio, L.
dc.contributor.authorSrinivasan, S.
dc.contributor.authorStevens, Jason
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.accessioned2012-02-21T17:47:54Z
dc.date.available2012-02-21T17:47:54Z
dc.date.issued2010-07-01
dc.identifier.citationGomez , H L , Baes , M , Cortese , L , Smith , M W L , Boselli , A , Ciesla , L , Bendo , G J , Pohlen , M , di Serego Alighieri , S , Auld , R , Barlow , M J , Bock , J J , Bradford , M , Buat , V , Castro-Rodriguez , N , Chanial , P , Charlot , S , Clements , D L , Cooray , A , Cormier , D , Davies , J I , Dwek , E , Eales , S , 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 , Papageorgiou , A , Parkin , T J , Perez-Fournon , I , Rangwala , N , Rigby , E E , Roussel , H , Rykala , A , Sacchi , N , Sauvage , M , Schirm , M R P , Schulz , B , Spinoglio , L , Srinivasan , S , Stevens , J , Symeonidis , M , Trichas , M , Vaccari , M , Vigroux , L , Wilson , C D , Wozniak , H , Wright , G S & Zeilinger , W W 2010 , ' The dust morphology of the elliptical Galaxy M 86 with SPIRE ' , Astronomy and Astrophysics , vol. 518 , L45 . https://doi.org/10.1051/0004-6361/201014530
dc.identifier.issn0004-6361
dc.identifier.otherBibtex: urn:9bf339b4db458b0457377ef115f307db
dc.identifier.otherORCID: /0000-0002-4010-8310/work/62747553
dc.identifier.urihttp://hdl.handle.net/2299/7854
dc.description.abstractWe present Herschel-SPIRE observations at 250–500 μm of the giant elliptical galaxy M 86 and examine the distribution of the resolved cold dust emission and its relation with other galactic tracers. The SPIRE images reveal three dust components: emission from the central region; a dust lane extending north-south; and a bright emission feature 10 kpc to the south-east. We estimate that ~106  M ? of dust is spatially coincident with atomic and ionized hydrogen, originating from stripped material from the nearby spiral NGC 4438 due to recent tidal interactions with M 86. The gas-to-dust ratio of the cold gas component ranges from ~20–80. We discuss the different heating mechanisms for the dust features.en
dc.format.extent1222818
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.subjectgalaxies: ellipticals and lenticular, cD, galaxies: individual: M 86, submillimeter: ISM, dust, extinction
dc.titleThe dust morphology of the elliptical Galaxy M 86 with SPIREen
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecord10.1051/0004-6361/201014530
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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