100 mum and 160 mum emission as resolved star-formation rate estimators in M33 HERM33ES - Astrophysics > Cosmology and Nongalactic AstrophysicsReportar como inadecuado




100 mum and 160 mum emission as resolved star-formation rate estimators in M33 HERM33ES - Astrophysics > Cosmology and Nongalactic Astrophysics - Descarga este documento en PDF. Documentación en PDF para descargar gratis. Disponible también para leer online.

Abstract: Over the past few years several studies have provided estimates of the SFRstar-formation rate or the total infrared luminosity from just one infraredband. However these relations are generally derived for entire galaxies, whichare known to contain a large scale diffuse emission that is not necessarilyrelated to the latest star-formation episode. We provide new relations toestimate the SFR from resolved star-forming regions at 100 mum and 160 mum. Weselect individual star-forming regions in the nearby 840 kpc galaxy M33. Weestimate the SFR combining the emission in Halpha and at 24 mum to calibratethe emission at 100 mum and 160 mum as SFR estimators, as mapped withPACS-Herschel. The data are obtained in the framework of the HERM33ES open timekey project. There is less emission in the HII regions at 160 mum than at 100mum. Over a dynamic range of almost 2 dex in SigmaSFR we find that the 100mum emission is a nearly linear estimator of the SFR, whereas that at 160 mumis slightly superlinear. The behaviour of individual star-forming regions issurprisingly similar to that of entire galaxies. At high SigmaSFR, starformation drives the dust temperature, whereas uncertainties and variations inradiation-transfer and dust-heated processes dominate at low SigmaSFR.Detailed modelling of both galaxies and individual star forming regions will beneeded to interpret similarities and differences between the two and assess thefraction of diffuse emission in galaxies.



Autor: M. Boquien, D. Calzetti, C. Kramer, E. M. Xilouris, F. Bertoldi, J. Braine, C. Buchbender, F. Combes, F. Israel, B. Koribalski, S

Fuente: https://arxiv.org/







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