Planck intermediate results. XXV. The Andromeda Galaxy as seen by Planck
Planck Collaboration: P. A. R. Ade, N. Aghanim, M. Arnaud, M. Ashdown,, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, N. Bartolo, E., Battaner, R. Battye, K. Benabed, G. J. Bendo, A. Benoit-L\'evy, J.-P., Bernard, M. Bersanelli, P. Bielewicz, A. Bonaldi, L. Bonavera

TL;DR
This study uses Planck data to map and analyze the dust emission and properties of the Andromeda Galaxy, revealing details about dust heating mechanisms, temperature distribution, and star formation activity.
Contribution
First detailed Planck-based analysis of M31's dust morphology, heating mechanisms, and spectral energy distribution across multiple wavelengths.
Findings
Dust emission at longer wavelengths is heated by diffuse stellar populations.
Dust temperature decreases linearly with galactocentric distance.
Detected free-free and potential spinning dust emission consistent with star formation rates.
Abstract
The Andromeda Galaxy (M31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiral arms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M31. We find that dust dominating the longer wavelength emission (mm) is heated by the diffuse stellar population (as traced by 3.6m emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24m emission). We also fit spectral energy distributions (SEDs) for individual 5'…
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