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Dust and Gas in the Small Magellanic Cloud

Published online by Cambridge University Press:  25 May 2016

Tj.R. Bontekoe ,
D.J.M. Kester ,
S. Stanimirović ,
L. Staveley–Smith  and
J.M. van der Hulst
Tj.R. Bontekoe
Affiliation:
Bontekoe Data Consultancy, Herengracht 2-B, 2312 LD Leiden, The Netherlands
D.J.M. Kester
Affiliation:
Space Research Organisation Netherlands, P.O. Box 800, 9700 AV Groningen, The Netherlands
S. Stanimirović
Affiliation:
Space Research Organisation Netherlands, P.O. Box 800, 9700 AV Groningen, The Netherlands
L. Staveley–Smith
Affiliation:
Australia Telescope National Facility, CSIRO, P. 0. Box 76, Epping, NSW 2121, Australia
J.M. van der Hulst
Affiliation:
Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands

Extract

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Here we present four IRAS high resolution images of the Small Magellanic Cloud, as reconstructed by the HIRAS program using the Pyramid Maximum Entropy method (Bontekoe et al. 1994). (HIRAS is not to be confused with HiRes (Aumann et al. 1990).) The images show much more detail than in Schwering & Israel (1990). Dust temperatures range from 25–41 K (Stanimirović et al. in prep).

Type
Part 2. Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 190: New Views of the Magellanic Clouds , 1999 , pp. 122 - 123
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

Aumann, H.H., Fowler, J.W., & Melnyk, M. 1990, AJ, 99, 1674 Google Scholar
Bontekoe, Tj.R., Koper, E., & Kester, D.J.M. 1994, A&A, 284, 1037 Google Scholar
Schwering, P.B.W. & Israel, F.P. 1990, Atlas and catalogue of infrared sources in the Magellanic clouds, Cambridge University Press.CrossRefGoogle Scholar