The Herschel Space Observatory view of dust in M81
G. J. Bendo, C. D. Wilson, M. Pohlen, M. Sauvage, R. Auld, M. Baes, M., J. Barlow, J. J. Bock, A. Boselli, M. Bradford, V. Buat, N. Castro-Rodriguez,, P. Chanial, S. Charlot, L. Ciesla, D. L. Clements, A. Cooray, D. Cormier, L., Cortese, J. I. Davies, E. Dwek, S. A. Eales
TL;DR
This study uses Herschel data to analyze dust emission in M81, revealing how different infrared wavelengths trace dust heated by various stellar populations and the active nucleus.
Contribution
It provides new observational constraints on dust emission properties across multiple wavelengths in a nearby galaxy.
Findings
160-500 micron emission traces 15-30 K dust heated by evolved stars
70 micron emission includes dust heated by the active nucleus and young stars
Ratios between 160 and 500 microns depend on radius, not surface brightness
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 microns in the nearby spiral galaxy M81. We find that the ratios of wave bands between 160 and 500 microns are primarily dependent on radius but that the ratio of 70 to 160 micron 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 micron emission traces 15-30 K dust heated by evolved stars in the bulge and disc whereas the 70 micron emission includes dust heated by the active galactic nucleus and young stars in star forming regions.
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