VERLEY, S.; RELAÑO, M.; KRAMER, C.; XILOURIS, E. M.; BOQUIEN, M.; CALZETTI, D.; COMBES, F.; BUCHBENDER, C.; BRAINE, J.; QUINTANA-LACACI, G.; TABATABAEI, F. S.; LORD, S.; ISRAEL, F.; STACEY, G.; VAN DER WERF, P.

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VERLEY, S.
Dept. fısica Teorica y del Cosmos

RELAÑO, M.
Dpto. Fisica Teorica y del Cosmos

KRAMER, C.
Instituto de RadioAstronomía Milimétrica [IRAM]

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SF2A-2010: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics. Eds.: S. Boissier, M. Heydari-Malayeri, R. Samadi and D. Valls-Gabaud, SF2A-2010: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics. Eds.: S. Boissier, M. Heydari-Malayeri, R. Samadi and D. Valls-Gabaud, SF2A-2010: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics. Eds.: S. Boissier, M. Heydari-Malayeri, R. Samadi and D. Valls-Gabaud - 21 - 24 June 2010, Marseille, p.57, 2010, 2010, Marseille. 2010-12p. 57

Resumen en inglés

Within the framework of the HERM33ES Key Project (Kramer et al. 2010), using the high resolution and sensitivity of the Herschel photometric data, we study the compact emission in the Local Group spiral galaxy M 33. We present a catalogue of 159 compact emission sources in M 33 identified by SExtractor in the 250 μm SPIRE band which is the one that provides the best spatial resolution. We measure fluxes at 24 μm and Hα for those 159 extracted sources. We find a very strong Pearson correlation coefficient with the MIPS 24 μm emission (r24 = 0.94) and a rather strong correlation with the Hα emission, although with more scatter (rHα = 0.83). Due to the very strong link between the 250 μm compact emission and the 24 μm and Hα emissions, by recovering the star formation rate from standard recipes for H II regions, we are able to provide star formation rate calibrations based on the 250 μm compact emission alone. Finally, the morphological study of a set of three Hα shells shows that there is a displacement between far-ultraviolet and the SPIRE bands, while the Hα structure is in general much more coincident with the cool dust.< Leer menos

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Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804