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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.otherPURE: 518417
dc.identifier.otherPURE UUID: d447e16c-6b5c-470b-b075-639e9ffbb4ea
dc.identifier.otherBibtex: urn:9bf339b4db458b0457377ef115f307db
dc.identifier.otherScopus: 77957820280
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.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rightsOpen
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.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/10.1051/0004-6361/201014530
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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