Results of the ESO / SEST Key Programme on Co/ in the Magellanic Clouds - Part One - a Survey of Co/ in the Large Magellanic Cloud and the Small Magellanic Cloud

Details Results of the ESO / SEST Key Programme on Co/ in the Magellanic Clouds - Part One - a Survey of Co/ in the Large Magellanic Cloud and the Small Magellanic Cloud Results of the ESO / SEST Key Programme on Co/ in the Magellanic Clouds - Part One - a Survey of Co/ in the Large Magellanic Cloud and the Small Magellanic Cloud

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...276...25i&link_type=abstract

Astronomy and Astrophysics, Vol.276, NO. 1/SEPI, P. 25, 1993

Astronomy and Astrophysics

Astrophysics

112

Scientific paper

As the first part of the ESO-Swedish SEST Key Programme on CO in the Magellanic Clouds, we have observed ^12^CO J = 1-0 towards 92 positions in the LMC and 42 positions in the SMC. In the SMC we searched for emission from H II regions, dark clouds and IRAS infrared sources. The generally negative detection rate of non-IRAS sources in the SMC led to an LMC source selection based on the IRAS results. In both galaxies, CO was detected towards the majority of sources observed. We also observed ^13^C0 J = 1-0 towards the brighter ^12^CO sources in the LMC (37) and SMC (9). Compared to the strength of CO lines observed in the Milky Way Galaxy with identical linear resolutions, velocity-integrated CO emission is weaker by at least a factor of three in the LMC sources and an order of magnitude in the SMC sources. The mean velocity-integrated isotopic intensity ratio I_12_/I_13_ is 12.5 in the LMC and about 15 in the SMC. Individual ratios range from 8.5 to 20. These isotopic intensity ratios are two to three times higher than those found in Galactic molecular clouds.

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