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dc.contributor.authorO'Halloran, B.
dc.contributor.authorGalametz, M.
dc.contributor.authorMadden, S. C.
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-Rodriguez, N.
dc.contributor.authorChanial, P.
dc.contributor.authorCharlot, S.
dc.contributor.authorCiesla, L.
dc.contributor.authorClements, D. L.
dc.contributor.authorCormier, D.
dc.contributor.authorCooray, A.
dc.contributor.authorCortese, L.
dc.contributor.authorDavies, J. I.
dc.contributor.authorDwek, E.
dc.contributor.authorEales, S. A.
dc.contributor.authorElbaz, D.
dc.contributor.authorGalliano, F.
dc.contributor.authorGear, W. K.
dc.contributor.authorGlenn, J.
dc.contributor.authorGomez, H. L.
dc.contributor.authorHony, S.
dc.contributor.authorIsaak, K. G.
dc.contributor.authorLevenson, L. R.
dc.contributor.authorLu, N.
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.authorPohlen, M.
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.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.accessioned2012-01-31T09:01:01Z
dc.date.available2012-01-31T09:01:01Z
dc.date.issued2010-07-01
dc.identifier.citationO'Halloran , B , Galametz , M , Madden , S C , Auld , R , Baes , M , Barlow , M J , Bendo , G J , Bock , J J , Boselli , A , Bradford , M , Buat , V , Castro-Rodriguez , N , Chanial , P , Charlot , S , Ciesla , L , Clements , D L , Cormier , D , Cooray , A , Cortese , L , Davies , J I , Dwek , E , Eales , S A , Elbaz , D , Galliano , F , Gear , W K , Glenn , J , Gomez , H L , Hony , S , Isaak , K G , Levenson , L R , Lu , N , Okumura , K , Oliver , S , Page , M J , Panuzzo , P , Papageorgiou , A , Parkin , T J , Perez-Fournon , I , Pohlen , M , 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 , Srinivasan , S , Stevens , J , 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 low metallicity dwarf galaxy NGC 1705 ' , Astronomy and Astrophysics , vol. 518 , L58 . https://doi.org/10.1051/0004-6361/201014580
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 518164
dc.identifier.otherPURE UUID: b2132db2-77cc-4540-8ec2-89c731dcdfb4
dc.identifier.otherBibtex: urn:3e99219f5dfe5ada8e91c13e8d4eb00c
dc.identifier.otherScopus: 77957780198
dc.identifier.otherORCID: /0000-0002-4010-8310/work/62747680
dc.identifier.urihttp://hdl.handle.net/2299/7746
dc.description.abstractWe present Herschel SPIRE and PACS photometeric observations of the low metallicity (Z ~ 0.35ΖΘ ) nearby dwarf galaxy, NGC 1705, in six wavelength bands as part of the Dwarf Galaxy Survey guaranteed time Herschel key program. We confirm the presence of two dominant circumnuclear IR-bright regions surrounding the central super star cluster that had been previously noted at mid-IR wavelengths and in the sub-mm by LABOCA. On constructing a global spectral energy distribution using the SPIRE and PACS photometry, in conjunction with archival IR measurements, we note the presence of an excess at sub-mm wavelengths. This excess suggests the presence of a signiPcant cold dust component within NGC 1705 and was modeled as an additional cold component in the SED. Although alternative explanations for the sub-mm excess beyond 350 μm, such as changes to the dust emissivity cannot be ruled out, the most likely explanation for the observed submillimetre excess is that of an additional cold dust component.en
dc.format.extent5
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.subjectgalaxies: dwarf, dust, extinction, evolution
dc.titleHerschel photometric observations of the low metallicity dwarf galaxy NGC 1705en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201014580
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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