Hostname: page-component-586b7cd67f-t8hqh Total loading time: 0 Render date: 2024-11-29T11:50:09.706Z Has data issue: false hasContentIssue false
  • English
  • Français

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
...Show all authors
Fatemeh S. Tabatabaei
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117-Heidelberg, Germany email: [email protected]
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: [email protected]
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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 125 - 127
Copyright
Copyright © International Astronomical Union 2012

References

Boquien, M., Calzetti, D., Kramer, C. et al. 2010, A&A, 518, 70Google Scholar
Gratier, P., Braine, J., Rodriguez-Fernandez, N. J. et al. 2010, A&A, 522, 3Google Scholar
Kramer, C., Buchbender, C., Xilouris, E. M. et al. 2010, A&A, 518, 67Google Scholar
Krügel, E. 2003, The Physics of Interstellar Dust (IoP Series in astronomy and astrophysics, ISBN 0750308613)CrossRefGoogle Scholar
Lisenfeld, U., Isaak, K. G., & Hills, R. 2000, MNRAS, 312, 433CrossRefGoogle Scholar
Paradis, D., Bernard, J.-Ph., & Mény, C. 2009, A&A, 506, 745Google Scholar