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The Nature of the Low-Metallicity ISMin the Dwarf Galaxy NGC 1569

Published online by Cambridge University Press:  25 September 2002

M. Giard ,
J.P. Bernard ,
A. Klotz ,
I. Ristorcelli ,
F. Galliano ,
S. Madden ,
A. P. Jones ,
C. Wilson ,
J. P. Bernard  and
F. Le Peintre
F. Galliano
Affiliation:
Service d'Astrophysique, CEA/Saclay, L'Orme des Merisiers, 91191 Gif-sur-Yvette, France
S. Madden
Affiliation:
Service d'Astrophysique, CEA/Saclay, L'Orme des Merisiers, 91191 Gif-sur-Yvette, France
A. P. Jones
Affiliation:
Institut d'Astrophysique Spatiale (CNRS), Université de Paris XI, 91405 Orsay, France
C. Wilson
Affiliation:
Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada
J. P. Bernard
Affiliation:
Institut d'Astrophysique Spatiale (CNRS), Université de Paris XI, 91405 Orsay, France
F. Le Peintre
Affiliation:
Institut d'Astrophysique Spatiale (CNRS), Université de Paris XI, 91405 Orsay, France
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Abstract

We are modeling the spectra of dwarf galaxies from infrared to submillimeter wavelengths to understand the nature of the various dust components in low-metallicity environments, which may be comparable to the ISM of galaxies in their early evolutionary state.The overall nature of the dust in these environments appears to differ fromthose of higher metallicity starbursting systems.Here, we present a study of one of our sample of dwarf galaxies, NGC 1569, which is a nearby, well-studied starbursting dwarf.Using ISOCAM, IRAS, ISOPHOT and SCUBA data with the Désert et al. (1990) [1] model, we find consistency with little contributionfrom PAHs and Very Small Grains and a relative abundance of bigger colder grains, which dominate the FIR and submillimeter wavelengths.We are compelled to use 4 dust components, adding a very cold dust component,to reproduce the submillimetre excess of our observations.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 4: Infrared and Submillimeter Space Astronomy: An International Colloquium to Honor the Memory of Guy Serra , 2002 , pp. 381
Copyright
© EAS, EDP Sciences, 2002

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