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À propos de : Properties of compact 250 μm emission and H  II regions in M 33 (HERM33ES)        

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  • Properties of compact 250 μm emission and H  II regions in M 33 (HERM33ES)
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  • Aims. Within the framework of the HERM33ES key program, using the high resolution and sensitivity of the Herschel photometric data, we study the compact emission in the Local Group spiral galaxy M 33 to investigate the nature of the compact SPIRE emission sources. We extracted a catalogue of sources at 250 μm in order to investigate the nature of this compact emission. Taking advantage of the unprecedented Herschel resolution at these wavelengths, we also focus on a more precise study of some striking H α shells in the northern part of the galaxy. Methods. We present a catalogue of 159 compact emission sources in M 33 identified by SExtractor in the 250 μm SPIRE band that is the one that provides the best spatial resolution. We also measured fluxes at 24 μm and H α for those 159 extracted sources. The morphological study of the shells also benefits from a multiwavelength approach including H α, far-ultraviolet from GALEX, and infrared from both Spitzer IRAC 8 μm and MIPS 24 μm in order to make comparisons. Results. For the 159 compact sources selected at 250 μm, we find a very strong Pearson correlation coefficient with the MIPS 24 μm emission ( r24 = 0.94) and a rather strong correlation with the H α emission, although with more scatter ( rH$r_{\alpha}$ = 0.83). The morphological study of the H α shells shows a displacement between far-ultraviolet, H α, and the SPIRE bands. The cool dust emission from SPIRE clearly delineates the H α shell structures. Conclusions. The very strong link between the 250 μm compact emission and the 24 μm and H α emissions, by recovering the star formation rate from standard recipes for H  II regions, allows us to provide star formation rate calibrations based on the 250 μm compact emission alone. The different locations of the H α and far-ultraviolet emissions with respect to the SPIRE cool dust emission leads to a dynamical age of a few Myr for the H α shells and the associated cool dust.
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  • aa14607-10
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  • © ESO, 2010
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  • ESO
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