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Comparison of CO in the Galaxy and the Magellanic Clouds

Published online by Cambridge University Press:  04 August 2017

F. P. Israel ,
Th. De Graauw ,
H. van de Stadt  and
C.P. De Vries
F. P. Israel
Affiliation:
Astronomy Division, ESA Space Science Department, Estec
Th. De Graauw
Affiliation:
Astronomy Division, ESA Space Science Department, Estec
H. van de Stadt
Affiliation:
Sterrewacht Sonnenborgh, Utrecht
C.P. De Vries
Affiliation:
Sterrewacht Sonnenborgh, Utrecht

Extract

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We have used the Estec/Utrecht heterodyne submillimetre receiver and the ESO 3.6-m telescope at La Silla (Chile) to observe the CO(2–1) transition at 230 GHz (1.3 mm) in the Magellanic Clouds. We used a beam of 2 arcmin HPBW (corresponding to linear resolutions of 32 and 46 pc for LMC and SMC respectively), the system temperature was 2200 K (DSB) and the overall system efficiency was 0.55. In this paper we summarize the results, which are published in more detail elsewhere (cf. Israel et al., 1982, 1983; Israel, 1984).

Type
PART II: COMPOSITION, STRUCTURE AND KINEMATICS
Information
Symposium - International Astronomical Union , Volume 106: The Milky Way Galaxy , 1985 , pp. 333 - 334
Copyright
Copyright © Reidel 1985 

References

Elmegreen, B.G., Elmegreen, D.M., Morris, M.: 1980, Astrophys. J. 240, 455.CrossRefGoogle Scholar
Israel, F.P., de Graauw, Th., van de Stadt, H., de Vries, C.P.: 1982, Astrophys. J. 262, 100 Google Scholar
Israel, F.P., de Graauw, Th., van de Stadt, H., de Vries, C.P.: 1983, Astrophys. J., submitted Google Scholar
Israel, F.P.: 1984, in Proc. IAU Symposium No. 108, van den Bergh, S., and de Boer, K.S. (eds.), 319 Google Scholar