Cold dust in galaxies

Eales, Stephen Anthony ORCID: https://orcid.org/0000-0002-7394-426X, Wynn-Williams, C. G. and Duncan, W. D. 1990. Cold dust in galaxies. Presented at: Kona Symposium on Millimetre and Submillimetre Astronomy, Kona, Hawaii, 3–6 October 1988. Published in: Watt, Graeme D. and Webster, Adrian S. eds. Submillimetre Astronomy: Proceedings of the Kona Symposium on Millimetre and Submillimetre Astronomy, Held at Kona, Hawaii, October 3–6, 1988. Astrophysics and Space Science Library (158) Dordrecht: Springer Netherlands, pp. 217-218. 10.1007/978-94-015-6850-0_80

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Abstract

Models for dust heated by the interstellar radiation field of a normal galaxy show that most of the thermal emission from the dust should be occurring in the submillimeter waveband (100 µm < λ < 1000 µm) (Spitzer 1978; Draine and Lee 1984; Draine and Anderson 1985). The IRAS survey confirmed that because most galaxies are emitting more strongly at 100 µm than at 60 µm, much of a galaxy’s emission should be in this wavelength region. We have used the UKT14 bolometer on the United Kingdom Infrared Telescope to observe the submillimeter emission from a sample of 11 spiral galaxies that are bright at 100 pm. The instrumental beam of the bolometer system has an approximately Gaussian shape with size (FWHM) of ≈80 arcsec. We used a beam separation of 136 arcsec E-W. The flux calibration and the extinction coefficients were obtained from observations of Saturn, Uranus, OMC-1, and IRC+10216. More details are given in Eales, Wynn-Williams, and Duncan (1989).

Item Type:	Conference or Workshop Item (Paper)
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Publisher:	Springer Netherlands
ISBN:	9789401568524
ISSN:	0067-0057
Related URLs:	Publisher
Last Modified:	24 Oct 2022 11:48
URI:	https://orca.cardiff.ac.uk/id/eprint/49368

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