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Probing the molecular interstellar medium of M82 with Herschel-SPIRE spectroscopy

dc.contributor.authorPanuzzo, P.
dc.contributor.authorRangwala, N.
dc.contributor.authorRykala, A.
dc.contributor.authorIsaak, K. G.
dc.contributor.authorGlenn, J.
dc.contributor.authorWilson, C. D.
dc.contributor.authorAuld, R.
dc.contributor.authorBaes, M.
dc.contributor.authorBarlow, M. J.
dc.contributor.authorBendo, G. 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.authorFulton, T.
dc.contributor.authorGalametz, M.
dc.contributor.authorGalliano, F.
dc.contributor.authorGear, W. K.
dc.contributor.authorGomez, H. L.
dc.contributor.authorGriffin, M.
dc.contributor.authorHony, S.
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.authorPapageorgiou, A.
dc.contributor.authorParkin, T. J.
dc.contributor.authorPérez-Fournon, I.
dc.contributor.authorPohlen, M.
dc.contributor.authorPolehampton, E. T.
dc.contributor.authorRigby, E. E.
dc.contributor.authorRoussel, H.
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.authorSwinyard, B.
dc.contributor.authorTrichas, M.
dc.contributor.authorVaccari, M.
dc.contributor.authorVigroux, L.
dc.contributor.authorWozniak, H.
dc.contributor.authorWright, G. S.
dc.contributor.authorZeilinger, W. W.
dc.date.accessioned2012-01-31T10:01:11Z
dc.date.available2012-01-31T10:01:11Z
dc.date.issued2010-07-01
dc.identifier.citationPanuzzo , P , Rangwala , N , Rykala , A , Isaak , K G , Glenn , J , Wilson , C D , Auld , R , Baes , M , Barlow , M J , Bendo , G 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 , Fulton , T , Galametz , M , Galliano , F , Gear , W K , Gomez , H L , Griffin , M , Hony , S , Levenson , L R , Lu , N , Madden , S , O'Halloran , B , Okumura , K , Oliver , S , Page , M J , Papageorgiou , A , Parkin , T J , Pérez-Fournon , I , Pohlen , M , Polehampton , E T , Rigby , E E , Roussel , H , Sacchi , N , Sauvage , M , Schulz , B , Schirm , M R P , Smith , M W L , Spinoglio , L , Stevens , J , Srinivasan , S , Symeonidis , M , Swinyard , B , Trichas , M , Vaccari , M , Vigroux , L , Wozniak , H , Wright , G S & Zeilinger , W W 2010 , ' Probing the molecular interstellar medium of M82 with Herschel-SPIRE spectroscopy ' , Astronomy and Astrophysics , vol. 518 , L37 . https://doi.org/10.1051/0004-6361/201014558
dc.identifier.issn0004-6361
dc.identifier.otherBibtex: urn:26abd4bd3bda9997cc72cbb982990891
dc.identifier.otherORCID: /0000-0002-4010-8310/work/62747681
dc.identifier.urihttp://hdl.handle.net/2299/7753
dc.description.abstractWe present the observations of the starburst galaxy M82 taken with the Herschel SPIRE Fourier-transform spectrometer. The spectrum (194–671 μm) shows a prominent CO rotational ladder from J = 4–3 to 13–12 emitted by the central region of M82. The fundamental properties of the gas are well constrained by the high J lines observed for the first time. Radiative transfer modeling of these high-S/N 12CO and 13CO lines strongly indicates a very warm molecular gas component at ~500 K and pressure of ~3×106 K cm-3, in good agreement with the H2 rotational lines measurements from Spitzer and ISO. We suggest that this warm gas is heated by dissipation of turbulence in the interstellar medium (ISM) rather than X-rays or UV flux from the straburst. This paper illustrates the promise of the SPIRE FTS for the study of the ISM of nearby galaxies.en
dc.format.extent5
dc.format.extent197825
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.subjectgalaxies: ISM, galaxies: starburst, galaxies: individual: M82, ISM: molecules, submillimeter: galaxies
dc.titleProbing the molecular interstellar medium of M82 with Herschel-SPIRE spectroscopyen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.description.statusPeer reviewed
rioxxterms.versionofrecord10.1051/0004-6361/201014558
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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