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Molecular gas in the Small Magellanic Cloud

  • Monica Rubio (a1)

Abstract

We summarize the results of observations of molecular gas from the Small Magellanic Cloud (SMC) made with low angular resolution (8'.8). These observations show that the CO emission is weak (TA˜ 0.04K) and that the CO luminosities of the Clouds are low compared to those of Galactic molecular clouds. The factor to convert the CO luminosity to molecular hydrogen column density for the SMC is ˜20 and three times larger than those derived for clouds in our Galaxy and in the Large Magellanic Cloud (LMC) respectively. In addition, we present preliminary results of high resolution (40″) observations of SMC molecular clouds made with the SEST telescope.

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References

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Castets, A., Duvert, G., Dutrey, A., Bally, J., Langer, W.D., Wilson, R.W. (1990), Astr. Ap. in press.
Henize, K. (1956), Ap. J. Supp. 2, 315.
Israel, F.P., Johansson, L.E.B. (1989), Recent Developments of Magellanic Cloud Research , de Boer, K.S., Spite, F., Stasinska, G. (eds.) (Observatoire de Paris: Paris) p. 11.
Johansson, L.E.B. (1990), IAU Symp 146 Dynamics of Galaxies and Molecular Clouds Distribution , in press.
Rubio, M., Garay, G., Montani, J., Thaddeus, P. (1990), Ap. J. in press.
Schwering, P. (1988), PhD Thesis, Leiden University, Holland.

Molecular gas in the Small Magellanic Cloud

  • Monica Rubio (a1)

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