The Herschel Space Observatory view of dust in M81
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. and Zeilinger, W.W.
(2010)
The Herschel Space Observatory view of dust in M81.
ISSN 0004-6361
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.
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