Verley, S. and Relaño, M. and Kramer, C. and Xilouris, E. M. and Boquien, M. and Calzetti, D. and Combes, F. and Buchbender, C. and Braine, J. and Quintana-Lacaci, G. and Tabatabaei, F. S. and Lord, S. and Israel, F. and Stacey, G. and van der Werf, P. (2010) Properties of compact 250 μm emission and H II regions in M 33 (HERM33ES). Astronomy and Astrophysics, 518 . L68. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20101202-094802671
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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 Hα 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 Hα for those 159 extracted sources. The morphological study of the shells also benefits from a multiwavelength approach including Hα, 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 (r_24 = 0.94) and a rather strong correlation with the Hα emission, although with more scatter (r_(Hα) = 0.83). The morphological study of the Hα shells shows a displacement between far-ultraviolet, Hα, and the SPIRE bands. The cool dust emission from SPIRE clearly delineates the Hα shell structures. Conclusions. 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, allows us to provide star formation rate calibrations based on the 250 μm compact emission alone. The different locations of the Hα and far-ultraviolet emissions with respect to the SPIRE cool dust emission leads to a dynamical age of a few Myr for the Hα shells and the associated cool dust.
|Additional Information:||© 2010 ESO. Received 31 March 2010; Accepted 28 April 2010; Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. We thank R.Walterbos for the Hα map. This work was partially supported by a Junta de Andalucía Grant FQM108, a Spanish MEC Grant AYA-2007-67625-C02-02, and a Juan de la Cierva fellowship. This research was supported by an MC-IEF within the 7th European Community Framework Programme.|
|Subject Keywords:||galaxies: individual: M33; galaxies: ISM; Local Group; galaxies: spiral|
|Official Citation:||Properties of compact 250 μm emission and H II regions in M 33 (HERM33ES) S. Verley, M. Relaño, C. Kramer, E. M. Xilouris, M. Boquien, D. Calzetti, F. Combes, C. Buchbender, J. Braine, G. Quintana-Lacaci, F. S. Tabatabaei, S. Lord, F. Israel, G. Stacey and P. van der Werf A&A 518 L68 (2010) DOI: 10.1051/0004-6361/201014607|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||02 Dec 2010 22:22|
|Last Modified:||26 Dec 2012 12:42|
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