Molecular Clouds in the 30-DORADUS Halo

Details Molecular Clouds in the 30-DORADUS Halo Molecular Clouds in the 30-DORADUS Halo

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...274..743g&link_type=abstract

Astronomy and Astrophysics, Vol. 274, NO. 3/JUL(III), P. 743, 1993

Astronomy and Astrophysics

Astrophysics

24

Scientific paper

Using the Columbia telescope we mapped with high sensitivity (0.02 K in radiation temperature) the CO(1-0) line emission from a region of 1.0^deg^ x 0.75^deg^ in size, centered near the 30 Doradus Nebula of the Large Magellanic Cloud. Most of the emission arises from six well discernable molecular clouds, with radii between 60 and 160 pc and luminosities between 1 x 10^4^ and 6 x 10^4^ K km s^-1^ pc^2^. The CO brightness temperature and luminosity of these clouds are significantly weaker than those of Galactic molecular clouds with similar linear dimensions. The proportionality factor between the total column density of gas, N(H_2_+2H), and the velocity integrated CO intensity for the 30 Doradus halo clouds is ~13 times larger than that for molecular complexes of similar size in the inner Galaxy, and ~2 times larger than the average value for clouds in the LMC. The strongest CO emission, although very weak compared with that of Galactic clouds, is associated with the 30 Doradus Nebula. The bulk of the molecular gas is at the heliocentric velocity of 265 km s^-1^, essentially equal to the mean velocity of both the stellar component and of the ionized gas in that region. This result, together with the low brightness temperature of the CO emission, suggests that the CO emission arises from small molecular clumps embedded in a region filled mainly by ionized gas and also possible by atomic gas where CO is photodissociated. Toward the Doradus Nebula there is also CO emission that is redshifted with respect to the main component, which we suggest arises from molecular gas that has been accelerated by the stellar winds from the many hot stars in that region.

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