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dc.contributor.authorParadis, D.
dc.contributor.authorVeneziani, M.
dc.contributor.authorNoriega-Crespo, A.
dc.contributor.authorPaladini, R.
dc.contributor.authorPiacentini, F.
dc.contributor.authorBernard, J.P.
dc.contributor.authorde Bernardis, P.
dc.contributor.authorCalzoletti, L.
dc.contributor.authorFaustini, F.
dc.contributor.authorMartin, P.
dc.contributor.authorMasi, S.
dc.contributor.authorMontier, L.
dc.contributor.authorNatoli, P.
dc.contributor.authorRistorcelli, I.
dc.contributor.authorThompson, M.A.
dc.contributor.authorTraficante, A.
dc.contributor.authorMolinari, S.
dc.date.accessioned2010-11-12T10:19:17Z
dc.date.available2010-11-12T10:19:17Z
dc.date.issued2010
dc.identifier.citationParadis , D , Veneziani , M , Noriega-Crespo , A , Paladini , R , Piacentini , F , Bernard , J P , de Bernardis , P , Calzoletti , L , Faustini , F , Martin , P , Masi , S , Montier , L , Natoli , P , Ristorcelli , I , Thompson , M A , Traficante , A & Molinari , S 2010 , ' Variations of the spectral index of dust emissivity from Hi-GAL observations of the Galactic plane ' , Astronomy and Astrophysics , vol. 520 . https://doi.org/10.1051/0004-6361/201015301
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 159303
dc.identifier.otherPURE UUID: b24bbd9d-185e-4e55-bdc9-39f0413b56be
dc.identifier.otherdspace: 2299/4981
dc.identifier.otherScopus: 77957558018
dc.identifier.otherORCID: /0000-0001-5392-909X/work/30970838
dc.identifier.urihttp://hdl.handle.net/2299/4981
dc.descriptionOriginal article can be found at: http://www.aanda.org/ Copyright The European Southern Observatory
dc.description.abstractContext. Variations in the dust emissivity are critical for gas mass determinations derived from far-infrared observations, but also for separating dust foreground emission from the Cosmic Microwave Background (CMB). Hi-GAL observations allow us for the first time to study the dust emissivity variations in the inner regions of the Galactic plane at resolution below 1°. Aims. We present maps of the emissivity spectral index derived from the combined Herschel PACS 160 μm, SPIRE 250 μm, 350 μm, and 500 μm data, and the IRIS 100 μm data, and we analyze the spatial variations of the spectral index as a function of dust temperature and wavelength in the two science demonstration phase Hi-GAL fields, centered at l = 30° and l = 59°. Methods. Applying two different methods, we determine both dust temperature and emissivity spectral index between 100 and 500 μm, at an angular resolution (θ) of 4'. Results. Combining both fields, the results show variations of the emissivity spectral index in the range 1.8–2.6 for temperatures between 14 and 23 K. The median values of the spectral index are similar in both fields, i.e. 2.3 in the range 100–500 μm, while the median dust temperatures are equal to 19.1 K and 16.0 K in the l = 30° and l = 59° field, respectively. Statistically, we do not see any significant deviations in the spectra from a power law emissivity between 100 and 500 μm. We confirm the existence of an inverse correlation between the emissivity spectral index and dust temperature, found in previous analyses.en
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rightsOpen
dc.titleVariations of the spectral index of dust emissivity from Hi-GAL observations of the Galactic planeen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2010
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201015301
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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