Show simple item record

dc.contributor.authorGalametz, M.
dc.contributor.authorMadden, S. C.
dc.contributor.authorGalliano, F.
dc.contributor.authorHony, S.
dc.contributor.authorSauvage, M.
dc.contributor.authorPohlen, M.
dc.contributor.authorBendo, G. J.
dc.contributor.authorAuld, R.
dc.contributor.authorBaes, M.
dc.contributor.authorBarlow, M. J.
dc.contributor.authorBock, J. J.
dc.contributor.authorBoselli, A.
dc.contributor.authorBradford, M.
dc.contributor.authorBuat, V.
dc.contributor.authorCastro-Rodríguez, 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.authorCortese, L.
dc.contributor.authorDavies, J. I.
dc.contributor.authorDwek, E.
dc.contributor.authorEales, S. A.
dc.contributor.authorElbaz, D.
dc.contributor.authorGear, W. K.
dc.contributor.authorGlenn, J.
dc.contributor.authorGomez, H. L.
dc.contributor.authorGriffin, M.
dc.contributor.authorIsaak, K. G.
dc.contributor.authorLevenson, L. R.
dc.contributor.authorLu, N.
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.authorPérez-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.authorSchulz, B.
dc.contributor.authorSchirm, M. R. P.
dc.contributor.authorSmith, M. W. L.
dc.contributor.authorSpinoglio, L.
dc.contributor.authorStevens, Jason
dc.contributor.authorSundar, 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.accessioned2012-01-31T09:01:06Z
dc.date.available2012-01-31T09:01:06Z
dc.date.issued2010-07-01
dc.identifier.citationGalametz , M , Madden , S C , Galliano , F , Hony , S , Sauvage , M , Pohlen , M , Bendo , G J , Auld , R , Baes , M , Barlow , M J , Bock , J J , Boselli , A , Bradford , M , Buat , V , Castro-Rodríguez , N , Chanial , P , Charlot , S , Ciesla , L , Clements , D L , Cooray , A , Cormier , D , Cortese , L , Davies , J I , Dwek , E , Eales , S A , Elbaz , D , Gear , W K , Glenn , J , Gomez , H L , Griffin , M , Isaak , K G , Levenson , L R , Lu , N , O'Halloran , B , Okumura , K , Oliver , S , Page , M J , Panuzzo , P , Papageorgiou , A , Parkin , T J , Pérez-Fournon , I , Rangwala , N , Rigby , E E , Roussel , H , Rykala , A , Sacchi , N , Schulz , B , Schirm , M R P , Smith , M W L , Spinoglio , L , Stevens , J , Sundar , S , Symeonidis , M , Trichas , M , Vaccari , M , Vigroux , L , Wilson , C D , Wozniak , H , Wright , G S & Zeilinger , W W 2010 , ' Herschel photometric observations of the nearby low metallicity irregular galaxy NGC 6822 ' , Astronomy and Astrophysics , vol. 518 , L55 . https://doi.org/10.1051/0004-6361/201014604
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 518292
dc.identifier.otherPURE UUID: c2cf790a-60f7-438e-813b-5dc5acf0f384
dc.identifier.otherBibtex: urn:176719bb316ad6471ca549d2e35922da
dc.identifier.otherScopus: 77957851994
dc.identifier.urihttp://hdl.handle.net/2299/7747
dc.description.abstractWe present the first Herschel PACS and SPIRE images of the low-metallicity galaxy NGC 6822 observed from 70 to 500 μm and clearly resolve the H ii regions with PACS and SPIRE. We find that the ratio 250/500 is dependent on the 24 μm surface brightness in NGC 6822, which would locally link the heating processes of the coldest phases of dust in the ISM to the star formation activity. We model the SEDs of some regions H ii regions and less active regions across the galaxy and find that the SEDs of H ii regions show warmer ranges of dust temperatures. We derive very high dust masses when graphite is used in our model to describe carbon dust. Using amorphous carbon, instead, requires less dust mass to account for submm emission due to its lower emissivity properties. This indicates that SED models including Herschel constraints may require different dust properties than commonly used. The global G/D of NGC 6822 is finally estimated to be 186, using amorphous carbon.en
dc.format.extent6
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectgalaxies: ISM, galaxies: dwarf, galaxies: photometry
dc.titleHerschel photometric observations of the nearby low metallicity irregular galaxy NGC 6822en
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
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201014604
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record