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        The Herschel Space Observatory view of dust in M81

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        Author
        Bendo, G. J.
        Wilson, C. D.
        Pohlen, M.
        Sauvage, M.
        Auld, R.
        Baes, M.
        Barlow, M.J.
        Bock, J. J.
        Boselli, A.
        Bradford, M.
        Buat, V.
        Castro-Rodriguez, 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.
        Galametz, M.
        Galliano, F.
        Gear, W.K.
        Glenn, J.
        Gomez, H.L.
        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.
        Schulz, B.
        Schirm, M. R. P.
        Smith, M. W. L.
        Spinoglio, L.
        Stevens, Jason
        Sundar, S.
        Symeonidis, M.
        Trichas, M.
        Vaccari, M.
        Vigroux, L.
        Wozniak, H.
        Wright, G. S.
        Zeilinger, W.W.
        Attention
        2299/7759
        Abstract
        We use Herschel Space Observatory data to place observational constraints on the peak and Rayleigh-Jeans slope of dust emission observed at 70–500 μm in the nearby spiral galaxy M81. We find that the ratios of wave bands between 160 and 500 μm are primarily dependent on radius but that the ratio of 70 to 160 μm emission shows no clear dependence on surface brightness or radius. These results along with analyses of the spectral energy distributions imply that the 160–500 μm emission traces 15–30 K dust heated by evolved stars in the bulge and disc whereas the 70 μm emission includes dust heated by the active galactic nucleus and young stars in star forming regions.
        Publication date
        2010-07-01
        Published in
        Astronomy and Astrophysics
        Published version
        https://doi.org/10.1051/0004-6361/201014568
        Other links
        http://hdl.handle.net/2299/7759
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