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#### A multiwavelength analysis of the clumpy FIR-bright sources in M33

##### MPS-Authors
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Natale,  G.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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1404.2310.pdf
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##### Citation

Natale, G., Foyle, K., Wilson, C. D., & Kuno, N. (2014). A multiwavelength analysis of the clumpy FIR-bright sources in M33. Monthly Notices of the Royal Astronomical Society, 441(1), 224-242. doi:10.1093/mnras/stu560.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0025-689F-2
##### Abstract
We present a multiwavelength study of a sample of far-infrared (FIR) sources detected on the Herschel broad--band maps of the nearby galaxy M33. We perform source photometry on the FIR maps as well as mid-infrared (MIR), H$\alpha$, far-ultraviolet and integrated HI and CO line emission maps. By fitting MIR/FIR dust emission spectra, the source dust masses, temperatures and luminosities are inferred. The sources are classified based on their H$\alpha$ morphology (substructured versus not-substructured) and on whether they have a significant CO detection ($S/N>$3$\sigma$). We find that the sources have dust masses in the range 10$^2$-10$^4$~M$_\odot$ and that they present significant differences in their inferred dust/star formation/gas parameters depending on their H$\alpha$ morphology and CO detection classification. The results suggests differences in the evolutionary states or in the number of embedded HII regions between the subsamples. The source background--subtracted dust emission seems to be predominantly powered by local star formation, as indicated by a strong correlation between the dust luminosity and the dust-corrected H$\alpha$ luminosity and the fact that the extrapolated young stellar luminosity is high enough to account for the observed dust emission. Finally, we do not find a strong correlation between the dust-corrected H$\alpha$ luminosity and the dust mass of the sources, consistent with previous results on the breakdown of simple scaling relations at sub-kpc scales. However, the scatter in the relation is significantly reduced by correcting the H$\alpha$ luminosity for the age of the young stellar populations in the star--forming regions.