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Variation in the dust spectral index across M33

Published online by Cambridge University Press:  17 August 2012

Fatemeh S. Tabatabaei ,
Jonathan Braine ,
Carsten Kramer ,
Manolis Xilouris ,
Mederic Boquien ,
Simon Verley ,
Eva Schinnerer ,
Daniela Calzetti ,
Francoise Combes  and
Frank Israel
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Fatemeh S. Tabatabaei
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117-Heidelberg, Germany email: taba@mpia.de
Jonathan Braine
Affiliation:
Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, 33271 Floirac, France
Carsten Kramer
Affiliation:
Instituto Radioastronomia Milimetrica, 18012 Granada, Spain
Manolis Xilouris
Affiliation:
Institute of Astronomy and Astrophysics, National Observatory of Athens, GR-15236 Athens, Greece
Mederic Boquien
Affiliation:
Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS, Marseille, France
Simon Verley
Affiliation:
Department Física Teórica y del Cosmos, Universidad de Granada, Spain
Eva Schinnerer
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117-Heidelberg, Germany email: taba@mpia.de
Daniela Calzetti
Affiliation:
Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA
Francoise Combes
Affiliation:
Observatoire de Paris, 75014 Paris, France
Frank Israel
Affiliation:
Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands
Christian Henkel
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121-Bonn, Germany
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Abstract

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Using the Herschel PACS and SPIRE FIR/submm data, we investigate variations in the dust spectral index β in the nearby spiral galaxy M33 at a linear resolution of 160 pc. We use an iteration method in two different approaches, single and two-component modified black body models. In both approaches, β is higher in the central disk than in the outer disk similar to the dust temperature. There is a positive correlation between β and Hα as well as with the molecular gas traced by CO(2-1). A Monte-Carlo simulation shows that the physical parameters are better constrained when using the two-component model.

Keywords

Interstellar MediumStar formationDustGalaxies: M33

References

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